planet_experiment.json

[{"classification_procedure": {"id": "OED", "term": "planet", "definition": "Any of various rocky or gaseous bodies that revolve in approximately elliptical orbits \naround the sun and are visible by its reflected light; esp. each of the planets Mercury, Venus, \nEarth, Mars, Jupiter, Saturn, Uranus, Neptune, and (until 2006) Pluto (in order of increasing \ndistance from the sun); a similar body revolving around another star. Also: any of various \nsmaller bodies that revolve around these (cf. satellite n. 2a).", "reference": "https://www.oed.com/dictionary/planet_n", "model_name": "gpt-4", "temperature": 0.1}, "results": [{"id": "http://www.wikidata.org/entity/Q18649725", "name": "CoRoT-19b", "article": "https://en.wikipedia.org/wiki/CoRoT-19b", "description": "CoRoT-19b is a transiting exoplanet found by the CoRoT space telescope in 2011.", "actual": "positive", "rationale": "CoRoT-19b is described as a transiting exoplanet, which means it is a body that revolves around a star other than the sun. This aligns with the definition of a planet as a body that revolves around a star. Therefore, based on the provided definition, CoRoT-19b can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q85765171", "name": "HIP 65426 b", "article": "https://en.wikipedia.org/wiki/HIP_65426_b", "description": "HIP 65426 b, formally named Najsakopajk, is a super-Jupiter exoplanet orbiting the star HIP 65426. It was discovered on 6 July 2017 by the SPHERE consortium using the Spectro-Polarimetric High-Contrast Exoplanet Research (SPHERE) instrument belonging to the European Southern Observatory (ESO). It is 385 light-years from Earth. It is the first planet discovered by ESO's SPHERE instrument.", "actual": "positive", "rationale": "HIP 65426 b fits the definition of a planet as it is a body that revolves around a star, in this case, the star HIP 65426. It is visible by the reflected light of its star. Furthermore, it is similar to the planets in our solar system, such as Jupiter, in that it is a super-Jupiter exoplanet, indicating it has a similar composition and size. Therefore, based on the provided definition, HIP 65426 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q42956220", "name": "OGLE-2016-BLG-1190Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2016-BLG-1190Lb", "description": "OGLE-2016-BLG-1190Lb is an extremely massive exoplanet, with a mass about 13.4 times that of Jupiter (MJ), or is, possibly, a low mass brown dwarf, orbiting the G-dwarf star OGLE-2016-BLG-1190L, located about 22,000 light years from Earth, in the constellation of Sagittarius, in the galactic bulge of the Milky Way.\u201cSince the existence of the brown dwarf desert is the signature of different formation mechanisms for stars and planets, the extremely close proximity of OGLE-2016-BLG-1190Lb to this desert raises the question of whether it is truly a \u2018planet\u2019 (by formation mechanism) and therefore reacts back upon its role tracing the galactic distribution of planets,\\\" according to astronomers reporting the findings.", "actual": "positive", "rationale": "OGLE-2016-BLG-1190Lb fits the definition of a planet as it is a body that revolves around a star, in this case, the G-dwarf star OGLE-2016-BLG-1190L. It is visible by the reflected light of its star, and it is similar to the planets in our solar system in that it is a massive body in space. Although its mass is much larger than that of Jupiter, it still falls within the broad definition of a planet as a body that orbits a star. Furthermore, the fact that it is located in the galactic bulge of the Milky Way suggests that it is part of a solar system, which is another characteristic of a planet. Therefore, based on the provided definition, OGLE-2016-BLG-1190Lb can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q19672944", "name": "Kepler-56c", "article": "https://en.wikipedia.org/wiki/Kepler-56c", "description": "Kepler-56c is a hot Jupiter (a class of exoplanets) orbiting the star Kepler-56, located in the constellation Cygnus. It was discovered by the Kepler telescope in October 2013. It orbits its parent star only 0.17 AU (16 million mi; 25 million km) away; at its distance, it completes an orbit once every 21.4 days. Its orbit is significantly misaligned with its parent star's equator.Both Kepler-56b and Kepler-56c will be devoured by their parent star in about 130 and 155 million years, respectively. Further research shows that it will have its atmosphere boiled away by intense heat from the star, and it will be stretched by the strengthening stellar tides.", "actual": "positive", "rationale": "Kepler-56c fits the definition of a planet as it is a body that revolves in an orbit around a star, in this case, the star Kepler-56. It is visible by the reflected light of its parent star. It is similar to the planets in our solar system, such as Jupiter, in that it is a gaseous body. Furthermore, it has a specific orbit, completing a revolution around its star every 21.4 days. Therefore, based on the provided definition, Kepler-56c can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q597170", "name": "HD 28185 b", "article": "https://en.wikipedia.org/wiki/HD_28185_b", "description": "HD 28185 b is an extrasolar planet 128 light-years away from Earth in the constellation of Eridanus. The planet was discovered orbiting the Sun-like star HD 28185 in April 2001 as a part of the CORALIE survey for southern extrasolar planets, and its existence was independently confirmed by the Magellan Planet Search Survey in 2008. HD 28185 b orbits its sun in a circular orbit that is at the inner edge of its star's habitable zone.", "actual": "positive", "rationale": "HD 28185 b fits the definition of a planet as it is a body that revolves around a star, in this case, the Sun-like star HD 28185. It was discovered as part of a survey for extrasolar planets, which are planets outside our solar system, further supporting its classification as a planet. Additionally, it has a circular orbit and is located at the inner edge of its star's habitable zone, characteristics that align with the definition of a planet. Therefore, based on the provided definition, HD 28185 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5629302", "name": "HD 16175 b", "article": "https://en.wikipedia.org/wiki/HD_16175_b", "description": "HD 16175 b is an exoplanet located approximately 195.7 light-years away in the constellation of Andromeda, orbiting the star HD 16175. This planet has a minimum mass 4.8 times that of Jupiter; the true mass was initially unknown since the inclination of the orbit was unknown. This planet orbits at about 2.2 astronomical units, taking 2.73 years to revolve around the star. The orbit of the planet is highly elliptical with an eccentricity of 0.64. In 2023, the inclination and true mass of HD 16175 b were determined via astrometry.The planet HD 16175 b is named Abol. The name was selected in the NameExoWorlds campaign by Ethiopia, during the 100th anniversary of the IAU. Abol is the first of three rounds of coffee in the Ethiopian traditional coffee ceremony.", "actual": "positive", "rationale": "HD 16175 b fits the definition of a planet as it is a body that revolves in an elliptical orbit around a star, in this case, the star HD 16175. It is visible by the reflected light of its star. Furthermore, it is similar to the planets in our solar system, such as Jupiter, in terms of having a significant mass and an elliptical orbit. Therefore, based on the provided definition, HD 16175 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1074458", "name": "HD 155358 c", "article": "https://en.wikipedia.org/wiki/HD_155358_c", "description": "HD 155358 c is an extrasolar planet orbiting the star HD 155358 located 142 light years away in the constellation Hercules. This is a gas giant which orbits at 1.224 AU and takes 530.3 days to orbit HD 155358. This planet orbits in an eccentric orbit. This planet has at least half the mass of Jupiter.", "actual": "positive", "rationale": "HD 155358 c fits the definition of a planet as it is a gaseous body that revolves around a star, in this case, HD 155358. It is visible by the reflected light of its star. It also orbits in an elliptical path, which is in line with the definition of a planet. Furthermore, it is similar to Jupiter, which is one of the planets listed in the definition. Therefore, based on the provided definition, HD 155358 c can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1146974", "name": "HAT-P-9b", "article": "https://en.wikipedia.org/wiki/HAT-P-9b", "description": "HAT-P-9b, formally named Alef, is an exoplanet approximately 1500 light years away in the constellation Auriga. This planet was found by the transit method on June 26, 2008. It has a mass 78% that of Jupiter and a radius 140% that of Jupiter. As with most transiting planets, this planet is a hot Jupiter, meaning this Jupiter-like planet orbits extremely close to its parent star, taking only 3.92 days to orbit.The study in 2012, utilizing a Rossiter\u2013McLaughlin effect, have determined the planetary orbit is mildly misaligned with the rotational axis of the star, misalignment equal to -16\u00b18\u00b0.The name Alef was selected in the NameExoWorlds campaign by Israel, during the 100th anniversary of the IAU. Alef is the first letter in the Hebrew alphabet and also means bull.", "actual": "positive", "rationale": "HAT-P-9b, or Alef, fits the definition of a planet as it is a body that revolves around a star, in this case, a star in the constellation Auriga. It was found using the transit method, which is a method used to detect planets. Furthermore, it has a mass and radius comparable to Jupiter, one of the planets in our solar system, and it orbits its parent star in a similar manner to how planets in our solar system orbit the sun. The fact that it is referred to as a \"hot Jupiter\" further supports the assertion that it is a planet, as this term is typically used to describe gas giant exoplanets that are similar in characteristics to the planet Jupiter. Therefore, based on the provided definition, HAT-P-9b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1039917", "name": "HD 49674 b", "article": "https://en.wikipedia.org/wiki/HD_49674_b", "description": "HD 49674 b, formally named Eburonia, is an extrasolar planet located approximately 134 light-years away in the constellation of Auriga, orbiting the star HD 49674. This planet was discovered orbiting the star in 2002. The planet is a gas giant and orbits extremely close to its star, which takes only 4.95 days to revolve.HD 49674 b, along with its parent star, was chosen as part of the 2019 NameExoWorlds campaign organised by the International Astronomical Union in which each country was assigned a star and planet to be named.  The HD 49674 system was assigned to Belgium.  The winning proposal named HD 49674 b Eburonia and the parent star Nervia, both after prominent Belgic tribes, the Eburones and Nervii respectively.", "actual": "positive", "rationale": "HD 49674 b fits the definition of a planet as it is a gaseous body that revolves around a star, in this case, the star HD 49674. It is visible by the reflected light of its star. Furthermore, it is similar to the planets in our solar system, such as Jupiter, in that it is a gas giant. Therefore, based on the provided definition, HD 49674 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q85058985", "name": "HAT-P-11c", "article": "https://en.wikipedia.org/wiki/HAT-P-11c", "description": "HAT-P-11c is a gas giant exoplanet that orbits HAT-P-11, a K-type star. Its mass is 2.3 Jupiters, it takes 9.3 years to complete one orbit of its star, and is 4.13 AU from its star. Its discovery was announced in 2018.", "actual": "positive", "rationale": "HAT-P-11c fits the definition of a planet as it is a gaseous body that revolves around a star, specifically HAT-P-11. It is visible by the reflected light of its star. Furthermore, it fits the description of a similar body revolving around another star, as it is an exoplanet, which is a planet outside our solar system. Therefore, based on the provided definition, HAT-P-11c can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q11717218", "name": "Kepler-62d", "article": "https://en.wikipedia.org/wiki/Kepler-62d", "description": "Kepler-62d (also known by its Kepler Object of Interest designation KOI-701.01) is the third innermost and the largest exoplanet discovered orbiting the star Kepler-62, with a size roughly twice the diameter of Earth. It was found using the transit method, in which the dimming that a planet causes as it crosses in front of its star is measured. Its stellar flux is 15 \u00b1 2 times Earth's. Due to its closer orbit to its star, it is a super-Venus or, if it has a volatile composition, a hot Neptune, with an estimated equilibrium temperature of 510 K (237 \u00b0C; 458 \u00b0F), too hot to sustain life on its surface.", "actual": "positive", "rationale": "Kepler-62d fits the definition of a planet as it is a body that revolves around a star, in this case, the star Kepler-62. It is visible by the reflected light from its star. It was discovered using the transit method, which measures the dimming that a planet causes as it crosses in front of its star, further supporting its classification as a planet. Although it is not one of the planets in our solar system, the definition allows for similar bodies revolving around other stars, which Kepler-62d does. Therefore, based on the provided definition, Kepler-62d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5177665", "name": "HD 164604 b", "article": "https://en.wikipedia.org/wiki/HD_164604_b", "description": "HD 164604 b is an extrasolar planet discovered in January 2010 in association with the Magellan Planet Search Program. It has a minimum mass 2.7 times the mass of Jupiter and an orbital period of 606.4 days. Its star is classified as a K2 V dwarf and is roughly 124 light-years away from Earth.HD 164604 b is named Caleuche. The name was selected in the NameExoWorlds campaign by Chile, during the 100th anniversary of the IAU. Caleuche is a large ghost ship from southern Chilean mythology which sails the seas around the island of Chilo\u00e9 at night.An astrometric measurement of the planet's inclination and true mass was published in 2022 as part of Gaia DR3.", "actual": "positive", "rationale": "HD 164604 b fits the definition of a planet as it is a body that revolves in an orbit, specifically around a star (its star is classified as a K2 V dwarf). It is also similar to the planets in our solar system, such as Jupiter, in terms of having a significant mass (2.7 times the mass of Jupiter). Furthermore, it was discovered as part of the Magellan Planet Search Program, indicating that it is indeed considered a planet by the scientific community. Lastly, it is visible by its reflected light from its star, which aligns with the definition of a planet being visible by the reflected light of the sun or another star.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q391576", "name": "HD 40307 f", "article": "https://en.wikipedia.org/wiki/HD_40307_f", "description": "HD 40307 f is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus  by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of G\u00f6ttingen, Germany. The existence of planet was confirmed in 2015.", "actual": "positive", "rationale": "HD 40307 f fits the definition of a planet as it is a body that revolves around a star, in this case, the star HD 40307. The fact that it was discovered using the radial velocity method, a common technique for detecting extrasolar planets, further supports this assertion. Additionally, the definition includes bodies that revolve around stars other than the sun, which applies to HD 40307 f as it orbits the star HD 40307, not the sun. Therefore, based on the provided definition, HD 40307 f can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q842110", "name": "Gliese 436 b", "article": "https://en.wikipedia.org/wiki/Gliese_436_b", "description": "Gliese 436 b  (sometimes called GJ 436 b, formally named Awohali) is a Neptune-sized exoplanet orbiting the red dwarf Gliese 436. It was the first hot Neptune discovered with certainty (in 2007) and was among the smallest-known transiting planets in mass and radius, until the much smaller Kepler exoplanet discoveries began circa 2010.\nIn December 2013, NASA reported that clouds may have been detected in the atmosphere of GJ 436 b.", "actual": "positive", "rationale": "Gliese 436 b fits the definition of a planet as it is a body that revolves around a star, in this case, the red dwarf Gliese 436. It is also visible by its reflected light, as evidenced by its discovery and subsequent observations. Furthermore, it is similar to Neptune, one of the planets in our solar system, in size. Therefore, based on the provided definition, Gliese 436 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q946435", "name": "HD 33564 b", "article": "https://en.wikipedia.org/wiki/HD_33564_b", "description": "HD 33564 b is an extrasolar planet located approximately 68 light-years away in the constellation of Camelopardalis. This planet orbits around F6V star HD 33564. The planet has an eccentric orbit, ranging in distance from 0.737 AU at periastron to 1.497 AU at apastron.\nHD 33564 b is a gas giant in a habitable zone of its star. Based on a probable 10\u22124 fraction of the planet mass as a satellite, it can have a Mars-sized moon with habitable surface. On the other hand, this mass can be distributed into many small satellites as well.", "actual": "positive", "rationale": "HD 33564 b fits the definition of a planet as it is a gaseous body that revolves in an orbit around a star, specifically the F6V star HD 33564. Its orbit is approximately elliptical, as indicated by its varying distance from the star at periastron and apastron. Furthermore, it is visible by the reflected light of its star. Therefore, based on the provided definition, HD 33564 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1329165", "name": "HD 4308 b", "article": "https://en.wikipedia.org/wiki/HD_4308_b", "description": "HD 4308 b is a low-mass exoplanet orbiting around HD 4308. It is believed to have almost no orbital eccentricity.", "actual": "positive", "rationale": "HD 4308 b fits the definition of a planet as it is a body that revolves around a star, in this case, HD 4308. The definition does not specify that the star has to be the sun, so HD 4308 b can still be considered a planet even though it orbits a different star. Furthermore, the definition does not exclude low-mass bodies or those with almost no orbital eccentricity, which are characteristics of HD 4308 b. Therefore, based on the provided definition, HD 4308 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5176581", "name": "HD 181433 d", "article": "https://en.wikipedia.org/wiki/HD_181433_d", "description": "HD 181433 d is an extrasolar planet located approximately 87 light years away in the constellation of Pavo, orbiting the star HD 181433. This planet has a minimum mass of 0.54 Jupiter mass and takes 2172 days to orbit the star. The average orbital distance is 3.00 AU. At periastron distance, it will have distance from the star similar to Mars\u2019 distance from the Sun at 1.56 AU. At apastron, the distance is 4.44 AU. These corresponds to the orbital eccentricity of 0.48.", "actual": "positive", "rationale": "HD 181433 d fits the definition of a planet as it is a body that revolves in an orbit around a star, in this case, the star HD 181433. It is visible by the reflected light of its star. It also has a mass and an orbital distance, similar to the planets in our solar system. The fact that it has a periastron and apastron distance indicates that it has an elliptical orbit, which is also a characteristic of a planet. Therefore, based on the provided definition, HD 181433 d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q843038", "name": "HD 171028 b", "article": "https://en.wikipedia.org/wiki/HD_171028_b", "description": "HD 171028 b is a >1.83 MJ exoplanet orbiting very eccentrically around HD 171028. The period is 1.47 years and semi-major axis of 1.29 AU. The Geneva Extrasolar Planet Search team announced the discovery of planet on July 13, 2007.", "actual": "positive", "rationale": "HD 171028 b fits the definition of a planet as it is a body that revolves around a star, in this case, HD 171028. The definition does not specify that the star has to be the sun, so planets revolving around other stars are also considered planets. Furthermore, the definition includes bodies that revolve in approximately elliptical orbits, which is consistent with the description of HD 171028 b's very eccentric orbit. Therefore, based on the provided definition, HD 171028 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q45747608", "name": "Kepler-90i", "article": "https://en.wikipedia.org/wiki/Kepler-90i", "description": "Kepler-90i  (also known by its Kepler Object of Interest designation KOI-351.08) is a super-Earth exoplanet with a radius 1.32  times that of Earth, orbiting the early G-type main sequence star Kepler-90 every 14.45 days, discovered by NASA's Kepler spacecraft. It is located about 2,840 light-years (870 parsecs, or nearly 2.4078\u00d71016 km) from Earth in the constellation Draco. The exoplanet is the eighth in the star's multiplanetary system. As of December 2017, Kepler-90 is the star hosting the most exoplanets found. Kepler-90i was found with the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured, and by a newly utilized computer tool, deep learning, a class of machine learning algorithms.", "actual": "positive", "rationale": "Kepler-90i fits the definition of a planet as it is a body that revolves around a star, specifically the Kepler-90 star. It is visible due to the reflected light from its star, which is a characteristic mentioned in the definition. It was discovered using the transit method, which measures the dimming effect a planet causes as it crosses in front of its star, further supporting the assertion that Kepler-90i is a planet. Additionally, it is referred to as an exoplanet, which is a term used to describe planets that orbit a star outside the solar system, aligning with the part of the definition that includes bodies revolving around other stars. Therefore, based on the provided definition, Kepler-90i can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q4039904", "name": "HD 212771 b", "article": "https://en.wikipedia.org/wiki/HD_212771_b", "description": "HD 212771 b is an extrasolar planet orbiting the G-type star HD 212771 approximately 364 light years away in the constellation Aquarius.", "actual": "positive", "rationale": "HD 212771 b fits the definition of a planet as it is a body that revolves around a star, in this case, the G-type star HD 212771. The definition does not specify that the star has to be the sun, therefore, HD 212771 b can be considered a planet. Furthermore, the definition includes bodies that revolve around stars other than the sun, which is referred to as an extrasolar planet, which is what HD 212771 b is. Therefore, based on the provided definition, HD 212771 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1369113", "name": "OGLE-2006-BLG-109Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2006-BLG-109Lb", "description": "OGLE-2006-BLG-109Lb is an extrasolar planet approximately 4,920 light-years away in the constellation of Sagittarius.  The planet was detected orbiting the star OGLE-2006-BLG-109L in 2008 by a research team using Microlensing.", "actual": "positive", "rationale": "The definition of a planet includes any rocky or gaseous body that revolves in an orbit around a star and is visible by its reflected light. The description of OGLE-2006-BLG-109Lb states that it is an extrasolar planet that orbits the star OGLE-2006-BLG-109L. Therefore, based on the provided definition, OGLE-2006-BLG-109Lb can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q841758", "name": "HD 68988 b", "article": "https://en.wikipedia.org/wiki/HD_68988_b", "description": "HD 68988 b is a hot jupiter located approximately 192 light-years away in the constellation of Ursa Major, orbiting the star HD 68988 in a moderately eccentric orbit.The planet HD 68988 b is called Albmi. The name was selected in the NameExoWorlds campaign by Norway, during the 100th anniversary of the IAU. Albmi means sky in the Northern Sami language.", "actual": "positive", "rationale": "HD 68988 b fits the definition of a planet as it is a body that revolves around a star, in this case, the star HD 68988. It is visible by the reflected light of its star. Furthermore, it is located in an elliptical orbit, which is a characteristic of a planet as per the definition. Therefore, based on the provided definition, HD 68988 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1328119", "name": "WASP-11b/HAT-P-10b", "article": "https://en.wikipedia.org/wiki/WASP-11b/HAT-P-10b", "description": "WASP-11b/HAT-P-10b or WASP-11Ab/HAT-P-10Ab is an extrasolar planet discovered in 2008. The discovery was announced (under the designation WASP-11b) by press release by the SuperWASP project in April 2008 along with planets WASP-6b through to WASP-15b, however at this stage more data was needed to confirm the parameters of the planets and the coordinates were not given. On 26 September 2008, the HATNet Project's paper describing the planet which they designated HAT-P-10b appeared on the arXiv preprint server. The SuperWASP team's paper appeared as a preprint on the Extrasolar Planets Encyclopaedia on the same day, confirming that the two objects (WASP-11b and HAT-P-10b) were in fact the same, and the teams agreed to use the combined designation.The planet has the third lowest insolation of the known transiting planets (only Gliese 436 b and HD 17156 b have lower insolation). The temperature implies it falls into the pL class of hot Jupiters: planets which lack significant quantities of titanium(II) oxide and vanadium(II) oxide in their atmospheres and do not have temperature inversions. An alternative classification system for hot Jupiters is based on the equilibrium temperature and the planet's Safronov number. In this scheme, for a given temperature, class I planets have high Safronov numbers and tend to be in orbit around cooler host stars, while class II planets have lower Safronov numbers. In the case of WASP-11b/HAT-P-10b, the equilibrium temperature is 1030 K and the Safronov number is 0.047\u00b10.003, which means it is located close to the dividing line between the class I and class II planets.The planet is in a binary star system, the second star is WASP-11 B, with a mass 0.34 \u00b10.05 of the Sun and a 3483 \u00b143 temperature.", "actual": "positive", "rationale": "WASP-11b/HAT-P-10b fits the definition of a planet as it is a body that revolves around a star, in this case, it is in a binary star system with the second star being WASP-11 B. It is visible by its reflected light and has an elliptical orbit. It is also similar to the planets in our solar system, such as Jupiter, in that it is classified as a hot Jupiter, a type of extrasolar planet. Therefore, based on the provided definition, WASP-11b/HAT-P-10b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q7946763", "name": "WASP-28b", "article": "https://en.wikipedia.org/wiki/WASP-28b", "description": "WASP-28b or K2-1b is an extrasolar planet discovered in 2010 by the Wide Angle Search for Planets (WASP) project orbiting WASP-28, a magnitude 12 star also known as 1SWASP J233427.87-013448.1, 2MASS J23342787-0134482 and K2-1. Since it orbits its star very closely, the planet is a strongly irradiated hot Jupiter. As seen from the Earth, WASP-28b transits its host star every 3.41 days taking about 3 hours to do so.The planet was observed by the Kepler spacecraft during the K2 mission engineering campaign in February 2014 as part of an early science demonstration. It was also observed from December 2016 to March 2017 during K2's campaign 12 which allowed a refinement of the system parameters.", "actual": "positive", "rationale": "WASP-28b fits the definition of a planet as it is a body that revolves around a star, in this case, WASP-28. The fact that it is described as an extrasolar planet further supports this assertion. Additionally, it is visible by its reflected light, as evidenced by its observation by the Kepler spacecraft. The planet's orbit is also mentioned, with it transiting its host star every 3.41 days, which aligns with the definition's requirement of an approximately elliptical orbit. Therefore, based on the provided definition, WASP-28b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q429564", "name": "OGLE-2005-BLG-071Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2005-BLG-071Lb", "description": "OGLE-2005-BLG-071Lb is a planet discovered by the Optical Gravitational Lensing Experiment (OGLE) and others in 2005, using gravitational microlensing. According to the best fit model, it has about 3.5 times the mass of Jupiter and a projected separation of 3.6 astronomical units from the star. This would result in an effective temperature around 50 K, similar to that of Neptune. However, an alternative model which gives a slightly lower mass of 3.3 times that of Jupiter and a projected separation of 2.1 AU is only slightly less likely. It may be the most massive planet currently known around a red dwarf star (though only lower limits are known for those planets detected by the radial velocity method).", "actual": "positive", "rationale": "OGLE-2005-BLG-071Lb fits the definition of a planet as it is a body that revolves around a star, in this case, a red dwarf star. It is visible by its reflected light, as it was discovered by the Optical Gravitational Lensing Experiment (OGLE) using gravitational microlensing. Furthermore, it has a mass that is several times that of Jupiter, one of the known planets in our solar system, suggesting it is a similar type of celestial body. Therefore, based on the provided definition, OGLE-2005-BLG-071Lb can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1252981", "name": "HD 113538 c", "article": "https://en.wikipedia.org/wiki/HD_113538_c", "description": "HD 113538 c is an exoplanet approximately 51 light years away from Earth in the constellation Centaurus. It orbits its star (HD 113538) once every 1657 days, placing it in the outer edge of the habitable zone. However it is most likely a gas giant with no solid surface.", "actual": "positive", "rationale": "HD 113538 c fits the definition of a planet as it is a body that revolves around a star, in this case, HD 113538. It is visible by the reflected light from its star. It is also similar to the planets in our solar system, such as Jupiter, in that it is likely a gas giant. Therefore, based on the provided definition, HD 113538 c can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q2593320", "name": "OGLE-2007-BLG-368Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2007-BLG-368Lb", "description": "OGLE-2007-BLG-368Lb is an extrasolar planet located approximately 19,230 light-years away in the constellation of Scorpius, orbiting the star OGLE-2007-BLG-368L. This planet was detected on December 8, 2009 by the gravitational microlensing by Sumi. It has mass 6.94% of Jupiter (i.e. 22 times that of Earth) and is located 3.3 AU from the star when observed. Based on those properties it would classify as a Cold Neptune. It is the second Cold Neptune to be observed, the first being OGLE-2005-BLG-169Lb. This planet is most likely be similar to Uranus and Neptune in the Solar System in terms of atmospheric and internal properties.", "actual": "positive", "rationale": "OGLE-2007-BLG-368Lb fits the definition of a planet as it is a body that revolves in an orbit around a star, specifically the star OGLE-2007-BLG-368L. It is visible due to the reflected light from its star. It is similar to the planets in our solar system, specifically Uranus and Neptune, in terms of its atmospheric and internal properties. Furthermore, it is classified as a Cold Neptune, which is a type of planet. Therefore, based on the provided definition, OGLE-2007-BLG-368Lb can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q3124868", "name": "HIP 78530 b", "article": "https://en.wikipedia.org/wiki/HIP_78530_b", "description": "HIP 78530 b is an object that is either a planet or a brown dwarf in the orbit of the star HIP 78530. It was observed as early as 2000, but the object was not confirmed as one in orbit of the star HIP 78530 until a direct imaging project photographed the star in 2008. The image caught the attention of the project's science team, so the team followed up on its initial observations. HIP 78530 b orbits a young, hot, bright blue star in the Upper Scorpius association. The planet itself is over twenty-three times more massive than Jupiter, orbiting eighteen times further from its host star than Pluto does from the Sun by the estimates published in its discovery paper. In this predicted orbit, HIP 78530 b completes an orbit every twelve thousand years.", "actual": "positive", "rationale": "HIP 78530 b can be considered a planet based on the provided definition because it is a body that revolves in an orbit around a star, specifically the star HIP 78530. This aligns with the definition's requirement that a planet is a body that revolves around the sun or another star. Furthermore, HIP 78530 b is visible by the reflected light of its host star, which is another characteristic of a planet according to the definition. The fact that it is over twenty-three times more massive than Jupiter and orbits eighteen times further from its host star than Pluto does from the Sun does not disqualify it from being a planet, as the definition does not specify a maximum size or distance from the host star for a body to be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q4039960", "name": "HD 85390 b", "article": "https://en.wikipedia.org/wiki/HD_85390_b", "description": "HD 85390 b (also known as HIP 48235 b) is an extrasolar planet which orbits the G-type main sequence star HD 85390, located approximately 106 light years away.\nThe planet HD 85390 b is named Madalitso. The name was selected in the NameExoWorlds campaign by Zambia, during the 100th anniversary of the IAU. Madalitso means blessings in the native language of Nyanja in Zambia.", "actual": "positive", "rationale": "The definition of a planet includes any body that revolves in approximately elliptical orbits around the sun or a similar body revolving around another star. HD 85390 b is described as an extrasolar planet that orbits the G-type main sequence star HD 85390. This aligns with the definition of a planet as it is a body that revolves around a star. Therefore, based on the provided definition, HD 85390 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q19672936", "name": "Kepler-56b", "article": "https://en.wikipedia.org/wiki/Kepler-56b", "description": "Kepler-56b (KOI-1241.02) is a hot Neptune\u2014a class of exoplanets\u2014located roughly 3,060 light-years (940 parsecs) away. It is somewhat larger than Neptune and orbits its parent star Kepler-56 and was discovered in 2013 by the Kepler Space Telescope.", "actual": "positive", "rationale": "Kepler-56b fits the definition of a planet as it is a body that revolves around a star, specifically Kepler-56. It is visible by the reflected light of its parent star. Furthermore, it is similar to Neptune, which is one of the planets listed in the definition. Therefore, based on the provided definition, Kepler-56b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q849161", "name": "HD 153950 b", "article": "https://en.wikipedia.org/wiki/HD_153950_b", "description": "HD 153950 b, also known as Trimobe, is an extrasolar planet located approximately 162 light-years away. This planet was discovered on October 26, 2008 by Moutou et al. using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile.The planet HD 153950 b is named Trimobe. The name was selected in the NameExoWorlds campaign by Madagascar, during the 100th anniversary of the IAU. Trimobe is a rich ogre from Malagasy tales.", "actual": "positive", "rationale": "HD 153950 b fits the definition of a planet as it is a body that revolves around a star, in this case, the star being HD 153950. It is visible by its reflected light and is similar to the bodies that revolve around the sun, such as Mercury, Venus, Earth, etc. Furthermore, it was discovered using a spectrograph on a telescope, which is a common method for discovering planets. Therefore, based on the provided definition, HD 153950 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q53616218", "name": "K2-155d", "article": "https://en.wikipedia.org/wiki/K2-155d", "description": "K2-155d is a potentially habitable Super-Earth exoplanet in the K2-155 system. It is the outermost of three known planets orbiting around the K-type star K2-155 in the constellation Taurus. It is one of 15 new exoplanets around red dwarf stars discovered by Japanese astronomer \\\"Teruyuki Hirano\\\" of the Tokyo Institute of Technology and his team. The team used data from NASA's Kepler Space Telescope during its extended K2 \\\"Second Light\\\" mission. K2-155d orbits near the so-called habitable zone of its system, and has the potential to host liquid water.", "actual": "positive", "rationale": "K2-155d fits the definition of a planet as it is a body that revolves around a star, in this case, the K-type star K2-155. It is visible by the reflected light of its star. It is also similar to the planets in our solar system as it orbits in a system with other planets. Furthermore, it is referred to as an exoplanet, which is a term used to describe planets that orbit around stars other than the sun. Therefore, based on the provided definition, K2-155d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5096657", "name": "HD 179079 b", "article": "https://en.wikipedia.org/wiki/HD_179079_b", "description": "HD 179079 b is an extrasolar planet which orbits the G-type subgiant star HD 179079, located approximately 228 light years away in the constellation Aquila. This planet has mass only 1/12 that of Jupiter or 1.5 times Neptune. The planet orbits very close to the star, at a distance of 0.11 AU. This planet takes two weeks to revolve around the star. This planet was discovered using the Keck telescopes on August 12, 2009.", "actual": "positive", "rationale": "HD 179079 b fits the definition of a planet as it is a body that revolves around a star, in this case, the G-type subgiant star HD 179079. It is visible by the reflected light from its star. It also has a mass, although smaller than Jupiter, it is still significant, and it orbits at a specific distance from its star. Furthermore, it has a specific orbital period, taking two weeks to revolve around the star. Therefore, based on the provided definition, HD 179079 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q26991323", "name": "OGLE-2007-BLG-349(AB)b", "article": "https://en.wikipedia.org/wiki/OGLE-2007-BLG-349(AB)b", "description": "OGLE-2007-BLG-349(AB)b is a circumbinary extrasolar planet about 8,000 light-years away in the constellation of Sagittarius. It is the first circumbinary exoplanet to be discovered using the microlensing method of detecting exoplanets.", "actual": "positive", "rationale": "OGLE-2007-BLG-349(AB)b fits the definition of a planet as it is an extrasolar planet, meaning it revolves around a star other than the sun. The definition of a planet includes bodies that revolve around stars other than the sun. Furthermore, it is described as a circumbinary planet, which means it revolves around two stars, still fitting within the definition of a planet. Therefore, based on the provided definition, OGLE-2007-BLG-349(AB)b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q67011452", "name": "HR 5183 b", "article": "https://en.wikipedia.org/wiki/HR_5183_b", "description": "HR 5183 b is an exoplanet located 102.7 light years away in the constellation of Virgo orbiting the star HR 5183. It has a mass of 3.31 MJ. It has a highly eccentric (e\u22430.87) orbit which takes it from within the orbit of Jupiter to beyond the orbit of Neptune, which classifies it as an eccentric Jupiter and it has been nicknamed the \\\"whiplash planet\\\". It was discovered in 2019 based on two decades of radial velocity observations.In 2021, astrometric observations revealed that HR 5183 b has a nearly edge-on orbital inclination, and thus its true mass is close to its minimum mass.", "actual": "positive", "rationale": "HR 5183 b fits the definition of a planet as it is a body that revolves in an orbit around a star, in this case, the star HR 5183. It is visible by the reflected light of its star. Although it is not one of the planets in our solar system, it is a similar body revolving around another star, which is included in the definition of a planet. Furthermore, its highly eccentric orbit and mass are characteristics often associated with planets. Therefore, based on the provided definition, HR 5183 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5629357", "name": "HD 5319 b", "article": "https://en.wikipedia.org/wiki/HD_5319_b", "description": "HD 5319 b is a gas giant exoplanet discovered in 2007 in the constellation of Cetus. This planet has a minimum mass nearly two times that of Jupiter. The planet has an almost circular orbit, with an eccentricity of only 0.02 and a period of 641 days. An additional planet in the system was discovered in 2015 and may be in a 4:3 mean motion resonance with planet b.", "actual": "positive", "rationale": "HD 5319 b fits the definition of a planet as it is a gaseous body, similar to Jupiter, that revolves in an orbit, specifically around the star HD 5319. It is visible due to the reflected light from its star. Furthermore, it is part of a system with at least one other planet, which aligns with the definition's inclusion of bodies that revolve around other planets or stars. Therefore, based on the provided definition, HD 5319 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q111723950", "name": "Nbu", "article": "https://en.wikipedia.org/wiki/Nbu", "description": "In Mandaeism, \u02bfNbu (Classical Mandaic: \u084f\u084d\u0841\u0845) or Nbu is the Mandaic name for the planet Mercury. Nbu is one of the seven planets (Classical Mandaic: \u0854\u0845\u0841\u0840, romanized: \u0161uba, lit.\u2009'The Seven'), who are part of the entourage of Ruha in the World of Darkness. This name was borrowed from the Mesopotamian god called Nabu.Nbu is associated with learning and scribes, as well as Christ and Christianity. Other names for Nbu include Maqurpiil, M\u0161iha (i.e., Jesus the Messiah), and \u02bfa\u1e6darid (of Arabic origin). Nbu's name is derived from the Akkadian Nab\u00fb.Buckley (2010) suggests a connection between Dinanukht and Nbu. For instance, in the Zrazta \u1e0f-Hibil Ziwa (Drower Collection Ms. 44), Nbu is the Lord of Book and ink and wisdom. Similarly, Dinanukht is called the \\\"ink-book of the gods\\\" in Right Ginza 6.", "actual": "positive", "rationale": "The definition of a planet includes any of various rocky or gaseous bodies that revolve in approximately elliptical orbits around the sun and are visible by its reflected light. This includes the planet Mercury. In the description of the entity Nbu, it is stated that Nbu is the Mandaic name for the planet Mercury. Therefore, based on the provided definition and the information in the description, it can be argued that Nbu is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5371571", "name": "HD 45652 b", "article": "https://en.wikipedia.org/wiki/HD_45652_b", "description": "HD 45652 b, also named Viriato, is a gas giant extrasolar planet orbiting at only 0.23 AU from the star HD 45652, with an orbital period of 44 days.  It has mass at least half that of Jupiter.  As it was detected using the radial velocity method, its true mass is dependent on the inclination of its orbit; if it is low, then the true mass will be larger.  Also, its radius is not known.  This planet was discovered by measurements taken by the ELODIE spectrograph from 2005 and 2006, and later confirmed by CORALIE and SOPHIE between 2006 and 2007.  The discovery was announced in May 2008.", "actual": "positive", "rationale": "HD 45652 b fits the definition of a planet as it is a gaseous body that revolves around a star, in this case, the star HD 45652. It is visible by the reflected light of its star. It has an elliptical orbit with an orbital period of 44 days. Although its radius is not known, it has a mass at least half that of Jupiter, which is a known planet. Therefore, based on the provided definition, HD 45652 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1140454", "name": "HD 80606 b", "article": "https://en.wikipedia.org/wiki/HD_80606_b", "description": "HD 80606 b (also Struve 1341 Bb or HIP 45982 b) is an eccentric hot Jupiter 217 light-years from the Sun in the constellation of Ursa Major. HD 80606 b was discovered orbiting the star HD 80606 in April 2001 by a team led by Michel Mayor and Didier Queloz. With a mass 4 times that of Jupiter, it is a gas giant. Because the planet transits the host star its radius can be determined using the transit method and was found to be slightly smaller than Jupiter's. Its density is slightly less than Earth's. It has an extremely eccentric orbit like a comet, with its orbit taking it very close to its star and then back out very far away from it every 111 days.", "actual": "positive", "rationale": "HD 80606 b fits the definition of a planet as it is a gaseous body that revolves in an orbit around a star, in this case, the star HD 80606. It is visible by the reflected light of its star. Furthermore, it has a mass and radius similar to Jupiter, which is one of the planets in our solar system. Its orbit, although extremely eccentric, still fits within the definition of a planet as it revolves around its star in a manner similar to how the planets in our solar system revolve around the sun. Therefore, based on the provided definition, HD 80606 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5178221", "name": "HD 24040 b", "article": "https://en.wikipedia.org/wiki/HD_24040_b", "description": "HD 24040 b is a long-period exoplanet taking approximately 3500 days to orbit at 4.6 astronomical units in an almost circular orbit. It has a minimum mass 4 times that of Jupiter.", "actual": "positive", "rationale": "HD 24040 b fits the definition of a planet as it is a body that revolves in an orbit around a star, in this case, the star being HD 24040. It is also similar to the planets in our solar system, such as Jupiter, in terms of its mass and its orbit, which is almost circular. Therefore, based on the provided definition, HD 24040 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q849267", "name": "42 Draconis b", "article": "https://en.wikipedia.org/wiki/42_Draconis_b", "description": "42 Draconis b (abbreviated 42 Dra b), formally named Orbitar , is a candidate extrasolar planet located approximately 315 light years from Earth in the constellation of Draco. It orbits the 5th magnitude K-type giant star 42 Draconis with a period of 479 days and 38% orbital eccentricity. The planet was discovered using the radial velocity method on March 20, 2009.Following its discovery the planet was designated 42 Draconis b. In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Orbitar for this planet. The winning name was submitted by the Brevard Astronomical Society of Brevard County, Florida, United States. Orbitar is a contrived word paying homage to the space launch and orbital operations of NASA.A 2021 study found that more recent radial velocity measurements of 42 Draconis were inconsistent with the proposed planetary orbit, casting serious doubt on 42 Draconis b's existence, but with a two-planet solution still being a possibility. The study suggests that the radial velocity signal is likely caused by a yet unknown stellar phenomenon, which might be common in giant stars.", "actual": "positive", "rationale": "42 Draconis b, also known as Orbitar, fits the definition of a planet as it is a body that revolves around a star, in this case, the K-type giant star 42 Draconis. It was discovered using the radial velocity method, which is a common method used to detect extrasolar planets. The planet has an orbital period of 479 days and an orbital eccentricity of 38%, further indicating its planetary nature. Although there is some doubt about its existence due to inconsistent radial velocity measurements, the possibility of it being a planet is still considered. Therefore, based on the provided definition, 42 Draconis b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q89514491", "name": "HD 177565 b", "article": "https://en.wikipedia.org/wiki/HD_177565_b", "description": "HD 177565 b is an extrasolar planet orbiting the G-type main-sequence star HD 177565 55.3 light-years away from the Solar System.", "actual": "positive", "rationale": "The definition of a planet includes any body that revolves in an elliptical orbit around a star and is visible by its reflected light. The description of HD 177565 b states that it is an extrasolar planet that orbits the G-type main-sequence star HD 177565. Therefore, based on the provided definition, HD 177565 b can be classified as a planet because it revolves around a star.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q419934", "name": "HD 125612 d", "article": "https://en.wikipedia.org/wiki/HD_125612_d", "description": "HD 125612 d is an extrasolar planet which orbits the G-type main sequence star HD 125612, located approximately 172 light years away in the constellation Virgo. The discovery of this planet was announced by the HARPS team on October 19, 2009, together with 31 other planets, including HD 125612 c.In 2022, the true mass and inclination of HD 125612 d were measured via astrometry.", "actual": "positive", "rationale": "HD 125612 d fits the definition of a planet as it is a body that revolves around a star, in this case, the G-type main sequence star HD 125612. It is located in the constellation Virgo, which is a specific location in space, similar to how the planets in our solar system are located at specific distances from the sun. The fact that its discovery was announced by the HARPS team, who are known for discovering planets, further supports the assertion that HD 125612 d is a planet. Additionally, its mass and inclination were measured in 2022, which is a characteristic process in the study and classification of planets. Therefore, based on the provided definition, HD 125612 d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q50358884", "name": "WASP-39b", "article": "https://en.wikipedia.org/wiki/WASP-39b", "description": "WASP-39b, officially named  Bocaprins, is a \\\"hot Jupiter\\\" extrasolar planet discovered in February 2011 by the WASP project, notable for containing a substantial amount of water in its atmosphere. In addition WASP-39b was the first exoplanet found to contain carbon dioxide in its atmosphere, and likewise for sulfur dioxide.\nWASP-39b is in the constellation Virgo, and is about 700 light-years from Earth. As part of the NameExoWorlds campaigns at the 100th anniversary of the IAU, the planet was named Bocaprins, after the beach Boca Prins in the Arikok National Park of Aruba.", "actual": "positive", "rationale": "WASP-39b fits the definition of a planet as it is a body that revolves around a star, in this case, a star in the constellation Virgo. It is visible due to the reflected light from its star. Furthermore, it is similar to the planets in our solar system, such as Jupiter, in that it has a substantial atmosphere containing various gases, including water, carbon dioxide, and sulfur dioxide. Therefore, based on the provided definition, WASP-39b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q547497", "name": "HD 69830 b", "article": "https://en.wikipedia.org/wiki/HD_69830_b", "description": "HD 69830 b is a Neptune-mass or super-Earth-mass exoplanet orbiting the star HD 69830. It is at least 10 times more massive than Earth. It also orbits very close to its parent star and takes 82/3 days to complete an orbit.\nBased on theoretical modeling in the 2006 discovery paper, this is likely to be a rocky planet, not a gas giant. However, other work has found that if it had formed as a gas giant, it would have stayed that way, and it is now understood that planets this massive are rarely rocky.If HD 69830 b is a terrestrial planet, models predict that tidal heating would produce a heat flux at the surface of about 55 W/m2. This is 20 times that of Io.", "actual": "positive", "rationale": "HD 69830 b fits the definition of a planet as it is a body that revolves in an orbit around a star, in this case, the star HD 69830. It is visible by the reflected light of its star. It is also similar to the planets in our solar system, such as Neptune, in terms of mass. Furthermore, it is theorized to be a rocky planet, which aligns with the definition's inclusion of rocky bodies. Therefore, based on the provided definition, HD 69830 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1361687", "name": "Gliese 674 b", "article": "https://en.wikipedia.org/wiki/Gliese_674_b", "description": "Gliese 674 b is an extrasolar planet approximately 15 light years away in the constellation of Ara. This planet orbits tightly around Gliese 674. It is a sub-Neptune-or-Uranus-mass planet either gaseous or rocky. It orbits as close as 0.039 AU from the star and takes only 4.6938 days to orbit. This planet has a similar eccentricity to Mercury (e=0.2). The discovery of the planet was announced on January 7, 2007 by using the HARPS spectrograph mounted on the ESO's 3.6 meter telescope at La Silla, Chile.", "actual": "positive", "rationale": "Gliese 674 b fits the definition of a planet as it is a body that revolves in an orbit around a star, in this case, the star being Gliese 674. The description states that it is either gaseous or rocky, which aligns with the definition of a planet being a rocky or gaseous body. Furthermore, it is visible by the reflected light from its star, another characteristic mentioned in the definition of a planet. Therefore, based on the provided definition, Gliese 674 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q50667", "name": "55 Cancri d", "article": "https://en.wikipedia.org/wiki/55_Cancri_d", "description": "55 Cancri d (abbreviated 55 Cnc d), formally named Lipperhey , is an extrasolar planet in a long-period orbit around the Sun-like star 55 Cancri A. Located at a similar distance from its star as Jupiter is from the Sun, it is the fifth and outermost known planet in its planetary system. 55 Cancri d was discovered on June 13, 2002.", "actual": "positive", "rationale": "55 Cancri d fits the definition of a planet as it is an extrasolar planet, meaning it revolves around a star other than the sun, which in this case is the Sun-like star 55 Cancri A. This aligns with the definition's inclusion of bodies that revolve around stars other than the sun. Furthermore, it is located at a similar distance from its star as Jupiter is from the Sun, which aligns with the definition's description of planets' approximately elliptical orbits around the sun. Therefore, based on the provided definition, 55 Cancri d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1204153", "name": "Kepler-8b", "article": "https://en.wikipedia.org/wiki/Kepler-8b", "description": "Kepler-8b is the fifth of the first five exoplanets discovered by NASA's Kepler spacecraft, which aims to discover planets in a region of the sky between the constellations Lyra and Cygnus that transit (cross in front of) their host stars. The planet is the hottest of the five. Kepler-8b was the only planet discovered in Kepler-8's orbit, and is larger (though more diffuse) than Jupiter. It orbits its host star every 3.5 days. The planet also demonstrates the Rossiter\u2013McLaughlin effect, where the planet's orbit affects the redshifting of the spectrum of the host star. Kepler-8b was announced to the public on January 4, 2010 at a conference in Washington, D.C. after radial velocity measurements conducted at the W.M. Keck Observatory confirmed its detection by Kepler.", "actual": "positive", "rationale": "Kepler-8b fits the definition of a planet as it is a body that revolves in an orbit around a star, specifically its host star. It is visible due to the reflected light from its host star, similar to how the planets in our solar system are visible due to reflected light from the sun. Furthermore, it is similar to Jupiter, one of the planets in our solar system, in terms of size, although it is more diffuse. Therefore, based on the provided definition, Kepler-8b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q86686508", "name": "Kepler-1658b", "article": "https://en.wikipedia.org/wiki/Kepler-1658b", "description": "Kepler-1658b (or the Kepler object of interest, KOI-4.01) is a hot Jupiter, a type of gas giant exoplanet, that orbits an F-type star called Kepler 1658, located about 2629 light-years away from the Solar System. It is the first planet identified by the Kepler space telescope after its launch in 2009, but later ruled out as false alarm since its transit could not be confirmed. A study published in 2019 established it as a planet, describing it as \\\"the closest known planet in terms of orbital period to an evolved star.\\\" Analysis of the Transiting Exoplanet Survey Satellite (TESS) data in 2022 showed that it is gradually spiraling into its star.", "actual": "positive", "rationale": "Kepler-1658b fits the definition of a planet as it is a gaseous body, specifically a gas giant exoplanet. It revolves around a star, Kepler 1658, in an orbit, which is a characteristic of a planet. It is also visible by the reflected light of its star. Furthermore, it is similar to the planets in our solar system, such as Jupiter, which is also a gas giant. Therefore, based on the provided definition, Kepler-1658b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q222246", "name": "2MASS J03552337+1133437", "article": "https://en.wikipedia.org/wiki/2MASS_J03552337%2B1133437", "description": "2MASS J03552337+1133437 (2MASS J0355+11) is a nearby brown dwarf of spectral type L5\u03b3, located in constellation Taurus at approximately 29.8 light-years from Earth.", "actual": "positive", "rationale": "The definition provided does not support the assertion that 2MASS J03552337+1133437 is a planet. According to the definition, a planet is a body that revolves in an elliptical orbit around the sun or another star. However, the description of 2MASS J03552337+1133437 identifies it as a brown dwarf, not a planet. A brown dwarf is a type of celestial body that is larger than a planet but not large enough to sustain nuclear fusion like a star. Therefore, based on the provided definition and description, it cannot be argued that 2MASS J03552337+1133437 is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q5281813", "name": "Discoverer 29", "article": "https://en.wikipedia.org/wiki/Discoverer_29", "description": "Discoverer 29, also known as Corona 9023, was an American optical reconnaissance satellite which was launched in 1961. It was the first KH-3 Corona''' satellite, which was based on an Agena-B rocket.The launch of Discoverer 29 occurred at 20:00 UTC on 30 August 1961. A Thor DM-21 Agena-B rocket was used, flying from Launch Complex 75-3-4 at the Vandenberg Air Force Base. Upon successfully reaching orbit, it was assigned the Harvard designation 1961 Psi 1.\nDiscoverer 29 was operated in a low Earth orbit, with a perigee of 138 kilometres (86 mi), an apogee of 511 kilometres (318 mi), 82 degrees of inclination, and a period of 91 minutes. The satellite had a mass of 1,150 kilograms (2,540 lb), and was equipped with a panoramic camera with a focal length of 61 centimetres (24 in), which had a maximum resolution of 7.6 metres (25 ft). Images were recorded onto 70-millimeter (2.8 in) film, and returned in a Satellite Recovery Vehicle two days after launch, but all of the images returned were found to be out of focus. The Satellite Recovery Vehicle used by Discoverer 29 was SRV-554. Once its images had been returned, Discoverer 29 remained in orbit until it decayed on 9 September 1961.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Discoverer 29 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. Discoverer 29, however, is described as an American optical reconnaissance satellite. It was launched and operated in a low Earth orbit, and it does not revolve around the sun in an elliptical orbit. Furthermore, it is not a natural body but a man-made object. Therefore, Discoverer 29 does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q54347", "name": "RazakSAT", "article": "https://en.wikipedia.org/wiki/RazakSAT", "description": "RazakSAT is a Malaysian Earth observation satellite carrying a high-resolution camera. It was launched into low Earth orbit on 14 July 2009. It was placed in a near-equatorial orbit that presents many imaging opportunities for the equatorial region. It weighs over three times as much as TiungSAT-1 and carries a high-resolution Earth observation camera. Developed in conjunction with the Satrec Initiative, the satellite's low inclination (9 degrees) brought it over Malaysia a dozen or more times per day. This was intended to provide greatly increased coverage of Malaysia compared to most other Earth observation satellites. An audit report released in October 2011 revealed that the satellite had failed after one year of operation.RazakSAT was the only operational satellite to be put into orbit by SpaceX's Falcon 1.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that RazakSAT is a planet. The definition of a planet specifies that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. RazakSAT, however, is an artificial satellite made by humans, not a natural celestial body. It orbits the Earth, not the sun, and it does not reflect light in the same way a planet does. Therefore, according to the given definition, RazakSAT cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1166037", "name": "Explorer 15", "article": "https://en.wikipedia.org/wiki/Explorer_15", "description": "Explorer 15, also called EPE-C or Energetic Particles Explorer-C, was a NASA satellite launched as part of the Explorer program. Explorer 15 was launched on 27 October 1962, at Cape Canaveral Air Force Station, Florida, United States, with a Thor-Delta A .", "actual": "negative", "rationale": "There is no valid argument based on the provided definition and information that Explorer 15 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. Explorer 15, on the other hand, is described as a satellite launched by NASA. It does not meet the criteria of being a natural, rocky or gaseous body, nor does it revolve around the sun in an elliptical orbit. Therefore, Explorer 15 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q60760723", "name": "JY1-SAT", "article": "https://en.wikipedia.org/wiki/JY1-SAT", "description": "JY1-SAT is a cubesat that is Jordan's first satellite. It was launched aboard SpaceX's Falcon 9 from the Vandenberg Air Force Base in the United States on 3 December 2018. It is named in tribute of the late King Hussein who was an amateur ham radio operator; his callsign was \\\"JY1\\\". The project was built by Jordanian students from various universities, and was funded by Jordan's Crown Prince Foundation.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that JY1-SAT is a planet. The definition of a planet includes being a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. JY1-SAT is a cubesat, which is a type of miniaturized satellite for space research, and not a natural celestial body. It does not meet the criteria of being a rocky or gaseous body, nor does it revolve around the sun in an elliptical orbit. Therefore, according to the provided definition, JY1-SAT cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q69165", "name": "ChinaSat 12", "article": "https://en.wikipedia.org/wiki/ChinaSat_12", "description": "The ChinaSat 12 (Chinese: \u4e2d\u661f12\u53f7; pinyin: Zh\u014dngx\u012bng 12) communications satellite is wholly owned by China Satellite Communications, with part of its communications payload leased or rented by SupremeSAT, a Sri Lankan company, to be marketed to potential users as SupremeSAT-I. Once operational, it will provide communications services for the China, Sri Lanka, East Asia, South Asia, Middle East, Africa, Australia, and China sea area, the Indian Ocean region.ChinaSat 12 was also known as Apstar 7B (as a backup of Apstar 7), but acquired by China Satellite Communications from its subsidiary APT Satellite Holdings in 2010. However, APT Satellite Holdings was contracted by its parent company as the operator of ChinaSat 12.", "actual": "negative", "rationale": "There is no valid argument based on the provided definition that ChinaSat 12 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. ChinaSat 12, however, is a communications satellite, which is a man-made object and not a natural celestial body. It does not fit the criteria of being a rocky or gaseous body, nor does it revolve around the sun. Therefore, based on the provided definition, ChinaSat 12 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q211655", "name": "2008 TC3", "article": "https://en.wikipedia.org/wiki/2008_TC3", "description": "2008 TC3 (Catalina Sky Survey temporary designation 8TA9D69) was an 80-tonne (80-long-ton; 90-short-ton), 4.1-meter (13 ft) diameter asteroid that entered Earth's atmosphere on October 7, 2008. It exploded at an estimated 37 kilometers (23 mi) above the Nubian Desert in Sudan. Some 600 meteorites, weighing a total of 10.5 kilograms (23.1 lb), were recovered; many of these belonged to a rare type known as ureilites, which contain, among other minerals, nanodiamonds.It was the first time that an asteroid impact had been predicted before its entry into the atmosphere as a meteor.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 2008 TC3 is a planet. The definition states that a planet is a body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. It also includes smaller bodies that revolve around these planets. However, 2008 TC3 was an asteroid that entered Earth's atmosphere and exploded. It did not revolve around the sun in an elliptical orbit, nor did it revolve around a planet. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4537552", "name": "Yamal 201", "article": "https://en.wikipedia.org/wiki/Yamal_201", "description": "Yamal-201 (Russian: \u042f\u043c\u0430\u043b-201) was a geostationary communications satellite operated by Gazprom Space Systems and built by RSC Energia. It was, along with Yamal-202 the second dual launch of the Yamal programme and the second iteration of the USP Bus. It was a 1,360 kg (3,000 lb) satellite with 4,080 watts of power (3.4 kW at end of life) on an unpressurized bus. It had eight SPT-70 electric thrusters by OKB Fakel for station keeping. Its payload was 9 C-band and 6 Ku-band transponders supplied by Space Systems/Loral.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Yamal 201 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in an elliptical orbit around the sun or another star, and is visible by its reflected light. Yamal 201, however, is described as a geostationary communications satellite. It is man-made, not a natural body, and it does not revolve around the sun or another star, but rather orbits the Earth. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q137248", "name": "1240 Centenaria", "article": "https://en.wikipedia.org/wiki/1240_Centenaria", "description": "1240 Centenaria, provisional designation 1932 CD, is a background asteroid from the outer regions of the asteroid belt, approximately 60 kilometers (37 miles) in diameter. It was discovered on 5 February 1932, by astronomer Richard Schorr at the Bergedorf Observatory in Hamburg, Germany. The assumed C-type asteroid has a rotation period of 11.3 hours. It was named for the 100th anniversary of the discovering observatory.", "actual": "negative", "rationale": "The definition of a planet includes \"any of various smaller bodies that revolve around\" the sun. 1240 Centenaria is described as a body from the outer regions of the asteroid belt that revolves around the sun. Therefore, based on this definition, one could argue that 1240 Centenaria is a planet. However, it's important to note that this argument is based on a broad interpretation of the definition, and in common usage, asteroids are typically not classified as planets.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4553351", "name": "178P/Hug\u2013Bell", "article": "https://en.wikipedia.org/wiki/178P/Hug%E2%80%93Bell", "description": "178P/Hug\u2013Bell is a periodic comet in the Solar System. It was discovered by Northeast Kansas Amateur Astronomers' League members Gary Hug and Graham Bell and is thought to be the first periodic comet to be discovered by amateurs. It was declared a comet less than two days after its initial discovery, after having its course confirmed on previous images.Hug-Bell's orbital period is about seven years; its orbit is eccentric, though less so than many comets. Hug-Bell's orbit lies entirely outside the orbit of Mars, but at its aphelion overlaps in solar distance with the orbit of Jupiter. Because it never comes closer to the Sun than about 2 AU, it is never expected to be a very bright comet, with a typical perihelion magnitude of 18-19.", "actual": "negative", "rationale": "Based on the provided definition, it is difficult to argue that 178P/Hug\u2013Bell is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. While 178P/Hug\u2013Bell does revolve around the sun in an elliptical orbit, it is identified as a comet, not a planet. The definition also mentions that planets are typically larger bodies, while 178P/Hug\u2013Bell is described as a periodic comet, which are usually smaller bodies composed of ice, rock, and dust. Therefore, based on the provided definition and description, it would be incorrect to classify 178P/Hug\u2013Bell as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q956514", "name": "3714 Kenrussell", "article": "https://en.wikipedia.org/wiki/3714_Kenrussell", "description": "3714 Kenrussell, provisional designation 1983 TT1, is a Eunomian asteroid from the central regions of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. It was discovered on 12 October 1983, by American astronomer Edward Bowell at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. It was named for Australian astronomer Kenneth S. Russell. The presumably stony asteroid has a rotation period of 5.25 hours.", "actual": "negative", "rationale": "Based on the provided definition, it is difficult to argue that 3714 Kenrussell is a planet. The definition states that a planet is a body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. While 3714 Kenrussell does revolve around the sun, it is not specified whether it is visible by its reflected light. Furthermore, the definition mentions specific planets in our solar system, none of which include 3714 Kenrussell. The definition also refers to smaller bodies that revolve around these planets as satellites, not planets. Therefore, based on the provided definition, it is challenging to assert that 3714 Kenrussell is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q116674440", "name": "S/2021 J 2", "article": "https://en.wikipedia.org/wiki/S/2021_J_2", "description": "S/2021 J 2 is a small outer natural satellite of Jupiter discovered by Scott S. Sheppard on 12 August 2021, using the 6.5-meter Magellan-Baade Telescope at Las Campanas Observatory, Chile. It was announced by the Minor Planet Center on 19 January 2023, after observations were collected over a long enough time span to confirm the satellite's orbit.S/2021 J 2 is part of the Ananke group, a cluster of retrograde irregular moons of Jupiter that follow similar orbits to Ananke at semi-major axes between 19\u201322 million km (12\u201314 million mi), orbital eccentricities between 0.1\u20130.4, and inclinations between 139\u2013155\u00b0. It has a diameter of about 1 km (0.62 mi) for an absolute magnitude of 17.3, making it one of Jupiter's smallest known moons.", "actual": "negative", "rationale": "Based on the provided definition, it would be challenging to argue that S/2021 J 2 is a planet. The definition of a planet states that it is a body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. However, S/2021 J 2 is described as a natural satellite of Jupiter, meaning it orbits Jupiter, not the sun. Furthermore, the definition of a planet includes specific bodies, namely Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, and formerly Pluto. S/2021 J 2 is not included in this list. Therefore, based on the provided definition, S/2021 J 2 does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q28845773", "name": "OV1-4", "article": "https://en.wikipedia.org/wiki/OV1-4", "description": "Orbiting Vehicle 1-4 (also known as OV1-4), launched 30 Mar 1966, was the fourth, and second successful, satellite in the OV1 series of the United States Air Force's Orbiting Vehicle program. OV1-4 was a long-term bioscience and materials science satellite, designed to return data relevant to long-term human presence in space. Its launch marked the first time two satellites (the other being OV1-5) were placed into orbit side by side with each other.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that OV1-4 is a planet. The definition states that a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. OV1-4, however, is described as a satellite launched by the United States Air Force, not a natural body. It was designed for bioscience and materials science research, indicating it is man-made and not a naturally occurring body like a planet. Therefore, using the provided definition and information, OV1-4 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q22084830", "name": "Near-Earth Asteroid Scout", "article": "https://en.wikipedia.org/wiki/Near-Earth_Asteroid_Scout", "description": "The Near-Earth Asteroid Scout (NEA Scout) was a mission by NASA to develop a controllable low-cost CubeSat solar sail spacecraft capable of encountering near-Earth asteroids (NEA). NEA Scout was one of ten CubeSats launched into a heliocentric orbit on Artemis 1, the maiden flight of the Space Launch System, on 16 November 2022.The target for the mission was asteroid 2020 GE, but this could have changed based on launch date or other factors. After deployment, NEA Scout was to perform a series of lunar flybys to achieve optimum departure trajectory before beginning its two-year-long cruise.\nNo contact was ever made, and the mission was lost.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that the Near-Earth Asteroid Scout is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. The Near-Earth Asteroid Scout, however, is a spacecraft developed by NASA, not a natural celestial body. It does not revolve around the sun in an elliptical orbit by its own gravitational pull, but rather it was launched into a heliocentric orbit. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q114646", "name": "696 Leonora", "article": "https://en.wikipedia.org/wiki/696_Leonora", "description": "696 Leonora is a Meliboean asteroid orbiting the Sun in the asteroid belt. It was discovered 10 January 1910 by American astronomer Joel Hastings Metcalf, at Taunton, Massachusetts. It was named by Arthur Snow of the United States Naval Observatory, who computed the orbit for the planet, after his wife, Mary Leonora Snow.", "actual": "negative", "rationale": "The definition of a planet includes \"any of various smaller bodies that revolve around\" the sun. The description of 696 Leonora states that it is an asteroid that orbits the Sun. Therefore, based on this definition, one could argue that 696 Leonora is a planet because it is a smaller body that revolves around the Sun. However, it's important to note that this argument is based on a broad interpretation of the definition, and in common usage, asteroids are typically not classified as planets.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1227405", "name": "T11 (satellite)", "article": "https://en.wikipedia.org/wiki/T11_(satellite)", "description": "T11, formerly known as DirecTV-11, is a Boeing model 702 satellite built by the Boeing Satellite Development Center. Its current name was adopted in 2017.", "actual": "negative", "rationale": "The definition of a planet includes any of various smaller bodies that revolve around these (planets). T11 is a satellite, which by definition is a body that revolves around a planet. Therefore, based on this definition, one could argue that T11 could be considered a type of planet. However, it's important to note that this argument is a stretch as the common understanding of a planet usually refers to natural celestial bodies, not man-made satellites.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q16061296", "name": "Eutelsat I F-2", "article": "https://en.wikipedia.org/wiki/Eutelsat_I_F-2", "description": "Eutelsat I F-2, also known as European Communications Satellite 2 (ECS-2) is a decommissioned communications satellite operated by the European Telecommunications Satellite Organisation (Eutelsat). Launched in 1984, it was operated in geostationary orbit at a longitude of 7\u00b0 East, before moving to several other locations later in its operational life, before it was finally decommissioned in 1993. It was the second of five satellites launched to form the first-generation Eutelsat constellation.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Eutelsat I F-2 is a planet. The definition of a planet specifies that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. Eutelsat I F-2, however, is a man-made communications satellite, not a natural celestial body. It was placed in geostationary orbit around the Earth, not the sun. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q539769", "name": "SCORE (satellite)", "article": "https://en.wikipedia.org/wiki/SCORE_(satellite)", "description": "SCORE (Signal Communications by Orbiting Relay Equipment) was the world's first purpose-built communications satellite. Launched aboard an American Atlas rocket on December 18, 1958, SCORE provided the second test of a communications relay system in space (the first having been provided by the USAF/NASA's Pioneer 1), the first broadcast of a human voice from space, and the first successful use of the Atlas as a launch vehicle. It captured world attention by broadcasting a Christmas message via shortwave radio from U.S. President Dwight D. Eisenhower through an on-board tape recorder. The satellite was popularly dubbed \\\"The Talking Atlas\\\". SCORE, as a geopolitical strategy, placed the United States at an even technological par with the Soviet Union as a highly functional response to the Sputnik 1 and Sputnik 2 satellites.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that SCORE (satellite) is a planet. The definition of a planet specifies that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. SCORE, however, is a man-made object, not a natural body, and it was designed for communication purposes, not as a celestial body. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q6433287", "name": "Kosmos 2478", "article": "https://en.wikipedia.org/wiki/Kosmos_2478", "description": "Kosmos 2478 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 2478 meaning Cosmos 2478) is a  Russian military satellite launched in 2011 as part of the GLONASS satellite navigation system.\nThis satellite is a GLONASS-M satellite, also known as Uragan-M, and is numbered Uragan-M No. 746.Kosmos 2478 was launched from Site 43/4  at Plesetsk Cosmodrome in northern Russia. A Soyuz-2-1b carrier rocket with a Fregat upper stage was used to perform the launch which took place at 08:26 UTC on 28 November 2011. The launch successfully placed the satellite into Medium Earth orbit. It subsequently received its Kosmos designation, and the international designator 2011\u2013071. The United States Space Command assigned it the Satellite Catalog Number 37938.It is in the third orbital plane used by GLONASS, in orbital slot 17.It started operations on 23 December 2011.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 2478 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in an approximately elliptical orbit around the sun and is visible by its reflected light. Kosmos 2478, however, is a man-made satellite that was launched as part of the GLONASS satellite navigation system. It does not naturally revolve around the sun, nor is it a natural body. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2521638", "name": "ViaSat-1", "article": "https://en.wikipedia.org/wiki/ViaSat-1", "description": "ViaSat-1 is a high throughput communications satellite owned by  Viasat Inc. and Telesat Canada. Launched October 19, 2011 aboard a Proton rocket, it held the Guinness record for the world's highest capacity communications satellite with a total capacity in excess of 140 Gbit/s, more than all the satellites covering North America combined, at the time of its launch.ViaSat-1 is capable of two-way communications with small dish antennas at higher speeds and a lower cost-per-bit than any satellite before.The satellite is positioned at 115.1 degrees West longitude geostationary orbit point, with 72 Ka-band spot beams; 63 over the U.S. (Eastern and Western states, Alaska and Hawaii), and nine over Canada.\nThe Canadian beams are owned by satellite operator Telesat and are used for the Xplornet broadband service to consumers in rural Canada. The US beams provide fast Internet access called Exede, Viasat's satellite Internet service.ViaSat-1 is part of a new satellite system architecture created by Viasat Inc. The objective is to create a better satellite broadband user experience, making satellite competitive with DSL and wireless broadband alternatives for the first time.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that ViaSat-1 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. ViaSat-1, however, is a man-made communications satellite, not a natural celestial body. It does not fit the criteria of being rocky or gaseous, and it does not revolve around the sun. Therefore, using the provided definition, ViaSat-1 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q7865651", "name": "USA-132", "article": "https://en.wikipedia.org/wiki/USA-132", "description": "USA-132, also known as GPS IIR-2 and GPS SVN-43, is an American navigation satellite which forms part of the Global Positioning System. It was the second Block IIR GPS satellite to be launched, out of thirteen in the original configuration, and twenty one overall. GPS IIR-1 failed to achieve orbit, so USA-132 was the first successful Block IIR satellite. It was built by Lockheed Martin, using the AS-4000 satellite bus.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that USA-132 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. USA-132, however, is described as a navigation satellite that forms part of the Global Positioning System. It is man-made and does not naturally revolve around the sun. Therefore, according to the given definition, USA-132 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4649953", "name": "AAUSat-3", "article": "https://en.wikipedia.org/wiki/AAUSat-3", "description": "AAUSat-3,  (Aalborg University CubeSat-3), is the third CubeSat built and operated by students from the Aalborg University in Denmark. It was launched on 25 February 2013 from the Satish Dhawan Space Centre in India on a Polar Satellite Launch Vehicle (PSLV) launch vehicle (PSLV-C20). AAUSat-3 carries two Automatic Identification System (AIS-1 and AIS-2) receivers as the main payload.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that AAUSat-3 is a planet. The definition specifies that a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. AAUSat-3, however, is a CubeSat, a type of miniaturized satellite for space research, built and operated by students from the Aalborg University in Denmark. It does not meet the criteria of being a rocky or gaseous body, nor does it revolve around the sun in an elliptical orbit. Therefore, AAUSat-3 cannot be classified as a planet based on the provided definition.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1612589", "name": "Communications Technology Satellite", "article": "https://en.wikipedia.org/wiki/Communications_Technology_Satellite", "description": "The Communications Technology Satellite (CTS), known as Hermes, was an experimental high-power direct broadcast communications satellite. It was a joint effort of Canadian Department of Communications, who designed and built the satellite, NASA who tested, launched and operated the satellite, and European Space Agency (ESA) who provided the 1200 watts solar panels and other devices. The three agencies shared the satellite and the data from the experiments.\nAlthough the launch of the ATS-6 spacecraft in 1974 marked the end of NASA's program of experimental communications satellites. NASA participated in a Canadian satellite venture known initially as \\\"Cooperative Applications Satellite-C\\\" and renamed Hermes. This joint effort involved NASA and the Canadian Department of Communications. NASA's Lewis Research Center provided the satellite's high-power communications payload. Canada designed and built the spacecraft; NASA tested, launched, and operated it. Also, the European Space Agency provided one of the low-power traveling-wave tubes and other equipment. Hermes was launched 17 January 1976 and operated until October 1979.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that the Communications Technology Satellite is a planet. The definition of a planet specifies that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. The Communications Technology Satellite, however, is a man-made object designed for communication purposes, not a natural celestial body. It does not meet the criteria of being a rocky or gaseous body, nor does it revolve around the sun in an elliptical orbit. Therefore, it cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153548", "name": "432 Pythia", "article": "https://en.wikipedia.org/wiki/432_Pythia", "description": "Pythia (minor planet designation: 432 Pythia) is a typical Main belt asteroid.\nIt was discovered by Auguste Charlois on 18 December 1897 in Nice.", "actual": "negative", "rationale": "The definition of a planet includes any of various smaller bodies that revolve around the sun. 432 Pythia is described as a Main belt asteroid, which means it is a smaller body that revolves around the sun. Therefore, based on the provided definition, one could argue that 432 Pythia is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4181082", "name": "Great Comet of 1819", "article": "https://en.wikipedia.org/wiki/Great_Comet_of_1819", "description": "The Great Comet of 1819, officially designated as C/1819 N1, also known as Comet Tralles, was an exceptionally bright and easily visible comet, approaching an apparent magnitude of 1\u20132, discovered July 1, 1819 by the German astronomer Johann Georg Tralles in Berlin. It was the first comet analyzed using polarimetry, by French mathematician Fran\u00e7ois Arago.", "actual": "negative", "rationale": "The assertion that the Great Comet of 1819 is a planet cannot be supported by the given definition. According to the definition, a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. The Great Comet of 1819, however, is described as a comet, not a planet. Comets are typically composed of ice, dust, and rocky material, and they have highly elliptical orbits that bring them close to the sun and then back to the outer parts of the solar system, which is different from the more circular or elliptical orbits of planets. Therefore, based on the provided definition and description, the Great Comet of 1819 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q376628", "name": "CHEOPS", "article": "https://en.wikipedia.org/wiki/CHEOPS", "description": "CHEOPS (CHaracterising ExOPlanets Satellite) is a European space telescope. Its objective is to determine the size of known extrasolar planets, which will allow the estimation of their mass, density, composition and their formation. Launched on 18 December 2019, it is the first Small-class mission in ESA's Cosmic Vision science programme.The small satellite features an optical Ritchey-Chr\u00e9tien telescope with an aperture of 30 cm, mounted on a standard small satellite platform. It was placed into a Sun-synchronous orbit of about 700 km altitude.", "actual": "negative", "rationale": "The assertion that CHEOPS is a planet cannot be supported by the given definition and information. According to the definition, a planet is a rocky or gaseous body that revolves in an elliptical orbit around the sun or another star, and is visible by its reflected light. However, the description of CHEOPS indicates that it is a space telescope launched by the European Space Agency, not a natural celestial body. It is designed to study and characterize extrasolar planets, but it is not a planet itself. Therefore, based on the provided definition and information, CHEOPS cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q17285875", "name": "Hodoyoshi 3", "article": "https://en.wikipedia.org/wiki/Hodoyoshi_3", "description": "Hodoyoshi-3 is a Japanese micro-satellite launched in 2014. The satellite is built in 0.5x0.5x0.65m box-shape bus, optimized for piggy-back launch.\nAll instruments are powered by solar cells mounted on the spacecraft body and two stub wings, with estimated electrical power of 50W. For orbit-keeping, a hydrogen peroxide thruster is used. The satellite was developed under the Funding Program for World-Leading Innovation R&D on Science and Technology.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Hodoyoshi 3 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. Hodoyoshi 3, however, is a man-made satellite, not a natural body, and it revolves around the Earth, not the sun. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q55624488", "name": "NOAA-14", "article": "https://en.wikipedia.org/wiki/NOAA-14", "description": "NOAA-14, also known as NOAA-J before launch, was an American weather satellite operated by the National Oceanic and Atmospheric Administration (NOAA). NOAA-14 continued the third-generation operational, Polar Orbiting Environmental Satellite (POES) series operated by the National Environmental Satellite Service (NESS) of the National Oceanic and Atmospheric Administration (NOAA). NOAA-14 continued the series of Advanced TIROS-N (ATN) spacecraft begun with the launch of NOAA-8 (NOAA-E) in 1983.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that NOAA-14 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. NOAA-14, however, is described as a weather satellite operated by the National Oceanic and Atmospheric Administration (NOAA). It is not described as a rocky or gaseous body, nor does it revolve around the sun. Therefore, according to the provided definition, NOAA-14 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q18239", "name": "Loge (moon)", "article": "https://en.wikipedia.org/wiki/Loge_(moon)", "description": "Loge or Saturn XLVI is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on 26 June 2006, from observations taken between January and April 2006.\nLoge is about 6 kilometres in diameter, and orbits Saturn at an average distance of 23,142,000 km in 1314.364 days, at an inclination of 166.5\u00b0 to the ecliptic (165.3\u00b0 to Saturn's equator), in a retrograde direction and with an eccentricity of 0.1390. It has a tentative rotation period of about 6.9\u00b10.1 hours, but this is highly uncertain as the light curve is the shallowest among all the irregular moons studied by Cassini\u2013Huygens (amplitude about 0.07 magnitudes).It was named in April 2007, after Logi, a fire giant from Norse mythology.", "actual": "negative", "rationale": "Based on the provided definition, it would be difficult to argue that Loge (moon) is a planet. The definition states that a planet is a body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. However, Loge is described as a natural satellite of Saturn, meaning it orbits Saturn, not the sun. Furthermore, the definition specifies certain planets in our solar system, none of which include Loge. Therefore, using the provided definition, it would not be accurate to classify Loge as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q63853", "name": "1509 Esclangona", "article": "https://en.wikipedia.org/wiki/1509_Esclangona", "description": "1509 Esclangona, provisional designation 1938 YG, is a rare-type Hungaria asteroid and binary system from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It is named after French astronomer Ernest Esclangon.", "actual": "negative", "rationale": "The definition of a planet includes any of various rocky bodies that revolve in approximately elliptical orbits around the sun and are visible by its reflected light. The description of 1509 Esclangona states that it is a rare-type Hungaria asteroid from the inner regions of the asteroid belt, which implies that it is a rocky body that revolves around the sun. However, the definition also specifies that a planet is a body that revolves around the sun in an elliptical orbit and is visible by its reflected light. The description does not provide information on whether 1509 Esclangona revolves in an elliptical orbit or if it is visible by its reflected light. Therefore, based solely on the provided definition and description, it cannot be definitively argued that 1509 Esclangona is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153870", "name": "4383 Suruga", "article": "https://en.wikipedia.org/wiki/4383_Suruga", "description": "4383 Suruga, provisional designation 1989 XP, is a Vestian asteroid and binary system from the inner regions of the asteroid belt, approximately 6.5 kilometers in diameter. It was discovered on 1 December 1989, by Japanese astronomer Yoshiaki Oshima at Gekko Observatory, Japan. The asteroid was named after the former Japanese Suruga Province. Its synchronous minor-planet moon, S/2013 (4383) 1, measures approximately 1.33 kilometers and has a period of 16.386 hours.", "actual": "negative", "rationale": "The definition of a planet includes any of various rocky bodies that revolve in orbits around the sun and are visible by its reflected light. The description of 4383 Suruga identifies it as a rocky body (asteroid) from the inner regions of the asteroid belt that revolves around the sun. Therefore, based on this information, one could argue that 4383 Suruga fits the definition of a planet. However, it's important to note that this argument is based on a broad interpretation of the definition, which does not take into account other factors often considered in classifying a celestial body as a planet, such as its size or its ability to clear its orbit of other debris.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q211473", "name": "(613100) 2005 TN74", "article": "https://en.wikipedia.org/wiki/(613100)_2005_TN74", "description": "(613100) 2005 TN74 (also written 2005 TN74) is a trans-Neptunian object (TNO) in a 3:5 resonance with Neptune. It was discovered by Scott S. Sheppard and Chadwick A. Trujillo in 2005.\nIt was initially suspected of being a Neptune trojan since the first observations gave it a semi-major axis of 30 AU and an orbital eccentricity of 0.16, but further observations showed it to have a semi-major axis of 42.7 AU, a perihelion of 32.1 AU, and an aphelion of 53.4 AU.With an absolute magnitude of 7.2, it has an expected diameter in the range of 85 to 240 km.It has been observed 19 times over four oppositions.", "actual": "negative", "rationale": "(613100) 2005 TN74 can be considered a planet based on the provided definition because it is a body that revolves in an elliptical orbit around the sun, which is one of the key characteristics of a planet. It is visible by the sun's reflected light, another characteristic mentioned in the definition. Furthermore, it is a trans-Neptunian object, meaning it is located beyond Neptune, one of the planets listed in the definition. Although its size is smaller than the traditional planets, the definition does not specify a minimum size for a planet, and it includes smaller bodies that revolve around the sun. Therefore, based on the provided definition, (613100) 2005 TN74 can be argued to be a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q136761", "name": "1173 Anchises", "article": "https://en.wikipedia.org/wiki/1173_Anchises", "description": "1173 Anchises  is an unusually elongated Jupiter Trojan from the Trojan camp, approximately 124 kilometers (77 miles) in diameter. It was discovered on 17 October 1930, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany, and was the 9th such body to be discovered.:\u200a2\u200a The primitive P-type asteroid belongs to the largest Jupiter trojans, has an unusually smooth surface texture, the lowest spectral slope of all members of the Trojan camp, and a rotation period of 11.6 hours. It was named after Anchises from Greek mythology.", "actual": "negative", "rationale": "The definition of a planet includes any of various rocky bodies that revolve in approximately elliptical orbits around the sun and are visible by its reflected light. The description of 1173 Anchises states that it is a Jupiter Trojan, which means it orbits the sun in the same path as Jupiter. This would fit the criteria of a planet as defined above. Additionally, it is described as a rocky body, further aligning with the definition of a planet. Therefore, one could argue that 1173 Anchises is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4044978", "name": "NOAA-16", "article": "https://en.wikipedia.org/wiki/NOAA-16", "description": "NOAA-16, also known as NOAA-L before launch, was an operational, polar orbiting, weather satellite series (NOAA K-N) operated by the National Environmental Satellite Service (NESS) of the National Oceanic and Atmospheric Administration (NOAA). NOAA-16 continued the series of Advanced TIROS-N (ATN) spacecraft that began with the launch of NOAA-8 (NOAA-E) in 1983; but it had additional new and improved instrumentation over the NOAA A-K series and a new launch vehicle (Titan 23G). It was launched on 21 September 2000 and, following an unknown anomaly, it was decommissioned on 9 June 2014. In November of 2015 it broke up in orbit, creating more than 200 pieces of debris.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that NOAA-16 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. NOAA-16, however, is described as a weather satellite operated by the National Oceanic and Atmospheric Administration (NOAA). It does not meet the criteria of being a rocky or gaseous body, nor does it revolve around the sun. Therefore, using the provided definition, NOAA-16 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q157514", "name": "867 Kovacia", "article": "https://en.wikipedia.org/wiki/867_Kovacia", "description": "867 Kovacia (prov. designation: A917 DH or 1917 BS) is an elongated, dark asteroid and member of the Hygiea family from the outer regions of the asteroid belt. It was discovered on 25 February 1917, by astronomer Johann Palisa at the Vienna Observatory in Austria. The carbonaceous C/B-type asteroid has a rotation period of 8.7 hours and measures approximately 24 kilometers (15 miles) in diameter. It was named after Austrian physician Friedrich Kovacs (1861\u20131931).", "actual": "negative", "rationale": "The definition of a planet includes \"any of various smaller bodies that revolve around these (the sun or other stars)\". 867 Kovacia is described as a body from the outer regions of the asteroid belt that revolves around the sun. Therefore, based on this part of the definition, one could argue that 867 Kovacia is a planet. However, it's important to note that this argument is based on a very broad interpretation of the definition, and in common usage, asteroids like 867 Kovacia are not typically classified as planets.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2402418", "name": "Galaxy 25", "article": "https://en.wikipedia.org/wiki/Galaxy_25", "description": "Galaxy 25 (G-25) launched in 1997, the launch was contracted by International Launch Services (ILS), (formerly known as Intelsat Americas 5 (IA-5) until 15 February 2007 when it was renamed as result of the merger between owner Intelsat and PanAmSat or Telstar 5) is a medium-powered communications satellite formerly in a geostationary orbit at 97\u00b0 West, above a point in the Pacific Ocean several hundred miles west of the Galapagos Islands. It was manufactured by Space Systems/Loral, part of its LS-1300 satellite bus, and is currently owned and operated by Intelsat. The satellite's main C-band transponder cluster covers the United States, Canada, and Mexico; its main Ku-band transponder cluster covers the United States, Mexico, and the Northern Caribbean Sea. An additional C-band and a Ku-band transponder pair targets Hawaii.\nGalaxy 25 has a projected life of 12 years. It was replaced by Galaxy 19 (formerly IA-9) in late 2008. When it was last in service at 97.1\u00b0 West, Galaxy 25 transmitted both Free-to-air (FTA) direct-to-home (DTH) broadcasting and encrypted subscription channels / services. The replacement satellite, Galaxy 19 was successfully launched on September 24, 2008. Galaxy 25 has been moved to a different orbital position at 93.1\u00b0 West where it is currently broadcasting several services on its Ku band transponders.", "actual": "negative", "rationale": "Based on the provided definition and information, there is no valid argument to assert that Galaxy 25 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in an elliptical orbit around the sun, and is visible by its reflected light. Galaxy 25, however, is described as a medium-powered communications satellite. It was manufactured, launched, and is operated by human entities, and its primary function is to transmit signals for communication purposes. It does not naturally revolve around the sun, nor is it visible by reflected sunlight. Therefore, according to the provided definition, Galaxy 25 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1119672", "name": "Kosmos 52", "article": "https://en.wikipedia.org/wiki/Kosmos_52", "description": "Kosmos 52 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 52 meaning Cosmos 52) or Zenit-2 No.26 was a Soviet, first generation, low resolution, optical film-return reconnaissance satellite launched in 1965. A Zenit-2 spacecraft, Kosmos 52 was the twenty-fifth of eighty-one such satellites to be launched and had a mass of 4,730 kilograms (10,430 lb).\nKosmos 52 was launched by a Vostok-2 rocket, serial number R15002-03, flying from Site 31/6 at the Baikonur Cosmodrome. The launch took place at 09:36 GMT on 11 January 1965, with the spacecraft receiving its Kosmos designation - along with the International Designator 1965-001A and the Satellite Catalog Number 00968 - upon its successful insertion into orbit. It was the first satellite to be launched in the year 1965.\nKosmos 52 was operated in a low Earth orbit. On 11 January 1965 it had a perigee of 203 kilometres (126 mi), an apogee of 298 kilometres (185 mi), an inclination of 65.0\u00b0 and an orbital period of 89.5 minutes. On 19 January 1965, eight days after launch, Kosmos 52 was deorbited so that its return capsule could be recovered by Soviet forces and its photos developed and analysed.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 52 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. Kosmos 52, however, is a man-made satellite that was launched into a low Earth orbit. It does not revolve around the sun, but rather around the Earth. Furthermore, it is not a natural body, but a piece of technology created for reconnaissance purposes. Therefore, according to the given definition, Kosmos 52 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q3399309", "name": "Kosmos 1317", "article": "https://en.wikipedia.org/wiki/Kosmos_1317", "description": "Kosmos 1317 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 1317 meaning Cosmos 1317) was a Soviet US-K missile early warning satellite which was launched in 1981 as part of the Soviet military's Oko programme. The satellite was designed to identify missile launches using optical telescopes and infrared sensors.Kosmos 1317 was launched from Site 16/2 at Plesetsk Cosmodrome in the Russian SSR. A Molniya-M carrier rocket with a 2BL upper stage was used to perform the launch, which took place at 22:54 UTC on 31 October 1981. The launch successfully placed the satellite into a molniya orbit. It subsequently received its Kosmos designation, and the international designator 1981-108A . The United States Space Command assigned it the Satellite Catalog Number 12933.Kosmos 1317 was a US-K satellite like Kosmos 862 that self-destructed in orbit, NASA believe deliberately. The first debris elements were\nspotted on 25 May 1981. All of the resultant debris is still in orbit.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 1317 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. Kosmos 1317, however, is a man-made satellite launched by the Soviet Union for the purpose of missile early warning. It does not naturally revolve around the sun, nor is it a natural body of rock or gas. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q102701", "name": "Hydra (moon)", "article": "https://en.wikipedia.org/wiki/Hydra_(moon)", "description": "Hydra is a natural satellite of Pluto, with a diameter of approximately 51 km (32 mi) across its longest dimension. It is the second-largest moon of Pluto, being slightly larger than Nix. Hydra was discovered along with Nix by astronomers using the Hubble Space Telescope on 15 May 2005, and was named after the Hydra, the nine-headed underworld serpent in Greek mythology. By distance, Hydra is the fifth and outermost moon of Pluto, orbiting beyond Pluto's fourth moon Kerberos.Hydra has a highly reflective surface caused by the presence of water ice, similar to other Plutonian moons. Hydra's reflectivity is intermediate, in between those of Pluto and Charon. The New Horizons spacecraft imaged Pluto and its moons in July 2015 and returned multiple images of Hydra.", "actual": "negative", "rationale": "Based on the provided definition, it would be challenging to argue that Hydra (moon) is a planet. The definition states that a planet is a body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. However, Hydra is described as a natural satellite of Pluto, meaning it orbits Pluto, not the sun. Furthermore, the definition specifies certain planets in our solar system, none of which include Hydra. Therefore, using the provided definition and information, it would not be accurate to classify Hydra as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q650661", "name": "FTV-1126", "article": "https://en.wikipedia.org/wiki/FTV-1126", "description": "FTV-1126, also known as Corona 9034A, was an American area survey optical reconnaissance satellite  launched in 1962. It was a KH-5 Argon satellite, based on an Agena-B. It was also unofficially known as Discoverer 41, a continuation of the designation sequence used for previous US reconnaissance satellites, which had officially been discontinued after Discoverer 38. It was the first KH-5 satellite to complete its mission successfully.The launch of FTV-1126 occurred at 19:36 UTC on 15 May 1962. A Thor DM-21 Agena-B rocket was used, flying from Launch Complex 75-3-5 at the Vandenberg Air Force Base. Upon successfully reaching orbit, it was assigned the Harvard designation 1962 Sigma 1.\nFTV-1126 was operated in a low Earth orbit, with a perigee of 284 kilometres (176 mi), an apogee of 632 kilometres (393 mi), 82.3 degrees of inclination, and a period of 93.75 minutes. The satellite had a mass of 1,150 kilograms (2,540 lb), and was equipped with a frame camera with a focal length of 76 millimetres (3.0 in), which had a maximum resolution of 140 metres (460 ft). Images were recorded onto 127-millimeter (5.0 in) film, and returned in a Satellite Recovery Vehicle, before the satellite ceased operations. The Satellite Recovery Vehicle used by FTV-1126 was 582. Once its images had been returned, the inactive FTV-1126 decayed from orbit on 26 November 1963.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that FTV-1126 is a planet. The definition of a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. FTV-1126, however, is described as a reconnaissance satellite launched by the United States in 1962. It was operated in a low Earth orbit and was equipped with a camera for recording images. It does not meet the criteria of being a natural body, nor does it revolve around the sun. Therefore, FTV-1126 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153133", "name": "424 Gratia", "article": "https://en.wikipedia.org/wiki/424_Gratia", "description": "Gratia (minor planet designation: 424 Gratia) is a large Main belt asteroid.\nIt was discovered by Auguste Charlois on 31 December 1896 in Nice.\nIt was named after the Gratiae from Greek mythology.", "actual": "negative", "rationale": "The definition of a planet includes any of various rocky bodies that revolve in approximately elliptical orbits around the sun and are visible by its reflected light. The entity 424 Gratia is described as a large Main belt asteroid, which implies that it is a rocky body that revolves around the sun. Therefore, based on the provided definition, one could argue that 424 Gratia is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q13561416", "name": "2010 GB174", "article": "https://en.wikipedia.org/wiki/2010_GB174", "description": "2010 GB174 is a detached object, discovered on 12 April 2010 on data taken at the Canada France Hawaii Telescope as part of the Next Generation Virgo Cluster Survey. It never gets closer than 48.5 AU from the Sun (about the outer edge of the Kuiper belt). Its large eccentricity strongly suggests that it was gravitationally scattered onto its current orbit. It is, like all detached objects, outside the current influence of Neptune, so how it got its current orbit is unknown. 2010 GB174 has the third highest Tisserand parameter relative to Jupiter of any Trans-Neptunian object, after Sedna and 2012 VP113. It has not been observed since 2015. It comes to opposition in late March each year in the constellation of Virgo.\nPrecovery images have been found back to 26 June 2009.It reached perihelion (closest approach to the Sun) in mid-1951 and has moved beyond 70 AU in September 2014. It is possibly a dwarf planet.", "actual": "negative", "rationale": "2010 GB174 could be considered a planet based on the provided definition. The definition states that a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. 2010 GB174 fits this description as it revolves around the sun, albeit at a great distance, and is visible by its reflected light. The definition also includes smaller bodies that revolve around these planets, which could potentially include 2010 GB174. Furthermore, the definition mentions that a planet can be a similar body revolving around another star, which leaves room for objects like 2010 GB174 that are outside the current influence of Neptune. Lastly, the definition does not exclude the possibility of a planet having a large eccentricity or being gravitationally scattered onto its current orbit, both characteristics of 2010 GB174. Therefore, based on the provided definition, one could argue that 2010 GB174 is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q280068", "name": "Soil Moisture and Ocean Salinity", "article": "https://en.wikipedia.org/wiki/Soil_Moisture_and_Ocean_Salinity", "description": "Soil Moisture and Ocean Salinity (SMOS) is a satellite which forms part of ESA's Living Planet Programme. It is intended to provide new insights into Earth's water cycle and climate. In addition, it is intended to provide improved weather forecasting and monitoring of snow and ice accumulation.", "actual": "negative", "rationale": "The assertion that Soil Moisture and Ocean Salinity (SMOS) is a planet cannot be supported by the given definition. According to the definition, a planet is a rocky or gaseous body that revolves in an elliptical orbit around the sun or another star, and is visible by its reflected light. SMOS, however, is described as a satellite that is part of ESA's Living Planet Programme. It is intended to provide insights into Earth's water cycle and climate, and improve weather forecasting and monitoring of snow and ice accumulation. Therefore, based on the provided information, SMOS does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q539098", "name": "9950 ESA", "article": "https://en.wikipedia.org/wiki/9950_ESA", "description": "9950 ESA, provisional designation 1990 VB, is an eccentric asteroid and elongated near-Earth object of the Amor group, approximately 1.7 kilometers in diameter. It was discovered on 8 November 1990, by French astronomer Christian Pollas at the Centre de recherches en g\u00e9odynamique et astrom\u00e9trie (Cerga) at Caussols in southeastern France. It was named for the European Space Agency (ESA).", "actual": "negative", "rationale": "The definition provided for a planet states that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. The description of 9950 ESA identifies it as an asteroid and a near-Earth object that revolves around the sun. It is also stated to be approximately 1.7 kilometers in diameter, which implies that it is a physical body. Therefore, based on the provided definition, one could argue that 9950 ESA fits the criteria of being a planet as it is a rocky body that revolves around the sun. However, it is important to note that this argument is based solely on the provided definition, and does not take into account other widely accepted criteria for what constitutes a planet, such as the need to have cleared its orbit of other debris.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q3272131", "name": "168P/Hergenrother", "article": "https://en.wikipedia.org/wiki/168P/Hergenrother", "description": "168P/Hergenrother is a periodic comet in the Solar System. The comet originally named P/1998 W2 returned in 2005 and got the temporary name P/2005 N2. The comet was last observed in January 2020, and may have continued fragmenting after the 2012 outburst.", "actual": "negative", "rationale": "The assertion that 168P/Hergenrother is a planet cannot be supported by the given definition. According to the definition, a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. While 168P/Hergenrother does revolve around the sun, it is identified as a comet, not a planet. Comets are typically composed of ice, dust, and rocky material, not just rock or gas as specified in the definition of a planet. Furthermore, the definition of a planet does not include bodies that are known to fragment, as 168P/Hergenrother is described to do. Therefore, based on the provided definition, 168P/Hergenrother cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q568802", "name": "20461 Dioretsa", "article": "https://en.wikipedia.org/wiki/20461_Dioretsa", "description": "20461 Dioretsa  is a centaur and damocloid on a retrograde, cometary-like orbit from the outer Solar System. It was discovered on 8 June 1999, by members of the LINEAR team at the Lincoln Laboratory Experimental Test Site near Socorro, New Mexico, United States. The highly eccentric unusual object measures approximately 14 kilometers (8.7 miles) in diameter. It was named Dioretsa, the word \\\"asteroid\\\" spelled backwards.", "actual": "negative", "rationale": "20461 Dioretsa can be considered a planet based on the definition provided. The definition states that a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. 20461 Dioretsa is described as a body from the outer Solar System that is on a retrograde, cometary-like orbit. This suggests that it revolves around the sun in an elliptical orbit. Furthermore, it is visible due to its reflected light, as it was discovered by the LINEAR team. Therefore, based on the provided definition, one could argue that 20461 Dioretsa is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2581556", "name": "(35671) 1998 SN165", "article": "https://en.wikipedia.org/wiki/(35671)_1998_SN165", "description": "(35671) 1998 SN165, prov. designation: 1998 SN165, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt object is a dwarf planet candidate, as it measures approximately 400 kilometers (250 miles) in diameter. It has a grey-blue color (BB) and a rotation period of 8.8 hours. As of 2021, it has not been named.", "actual": "negative", "rationale": "(35671) 1998 SN165 can be considered a planet based on the provided definition. The definition states that a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. (35671) 1998 SN165 fits this description as it is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System, meaning it revolves around the sun. It is also visible by its reflected light, as indicated by its grey-blue color. Furthermore, the definition includes smaller bodies that revolve around these planets, which could potentially include (35671) 1998 SN165 as it is a dwarf planet candidate. Therefore, based on the provided definition, one could argue that (35671) 1998 SN165 is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q22084849", "name": "Whipple (spacecraft)", "article": "https://en.wikipedia.org/wiki/Whipple_(spacecraft)", "description": "Whipple was a proposed space observatory in the NASA Discovery Program. The observatory would try to search for objects in the Kuiper belt and the theorized Oort cloud by conducting blind occultation observations. Although the Oort cloud was hypothesized in the 1950s, it has not yet been directly observed. The mission would attempt to detect Oort cloud objects by scanning for brief moments where the objects would block the light of background stars.In 2011, three finalists were selected for the 2016 Discovery Program, and Whipple was not among them, but it was awarded funding to continue its technological development efforts.", "actual": "negative", "rationale": "Based on the provided definition and information, there is no valid argument to assert that Whipple (spacecraft) is a planet. The definition of a planet involves being a rocky or gaseous body that revolves in approximately elliptical orbits around the sun or another star, and is visible by its reflected light. The Whipple spacecraft, however, is a man-made object designed for space exploration and observation, not a natural celestial body. It does not meet the criteria set out in the definition of a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q734423", "name": "Kosmos 17", "article": "https://en.wikipedia.org/wiki/Kosmos_17", "description": "Kosmos 17 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 17 meaning Cosmos 17), also known as DS-A1 No.2 was a technology demonstration satellite which was launched by the Soviet Union in 1963. It was launched as part of the Dnepropetrovsk Sputnik programme. Its primary mission was to demonstrate technologies for future Soviet military satellites. It also conducted radiation experiments.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 17 is a planet. The definition states that a planet is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. Kosmos 17, however, is described as a technology demonstration satellite launched by the Soviet Union. It does not meet the criteria of being a natural, rocky or gaseous body, nor does it revolve around the sun. Instead, it was man-made and launched for specific technological and experimental purposes. Therefore, using the provided definition, Kosmos 17 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q30739729", "name": "CSES Mission", "article": "https://en.wikipedia.org/wiki/CSES_Mission", "description": "CSES (China Seismo-Electromagnetic Satellite), or Zhangheng, is a Chinese\u2013Italian space mission dedicated to monitoring electromagnetic field and waves, plasma parameters and particle fluxes induced by natural sources and artificial emitters in the near-Earth space. Austria contributes to one of the magnetometers.\nThe first CSES Satellite was launched from the Jiuquan Satellite Launch Center in the Gobi Desert (Inner Mongolia) on February 2, 2018. The expected mission lifetime is 5 years.", "actual": "negative", "rationale": "The assertion that the CSES Mission is a planet cannot be supported by the given definition and information. According to the definition, a planet is a natural celestial body that revolves in an elliptical orbit around the sun or another star, and is visible by its reflected light. The CSES Mission, however, is a man-made satellite launched for the purpose of monitoring electromagnetic fields and waves, plasma parameters, and particle fluxes in near-Earth space. It does not fit the criteria of being a natural body, nor does it revolve around the sun or another star. Therefore, based on the provided definition and information, the CSES Mission cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q8616", "name": "19P/Borrelly", "article": "https://en.wikipedia.org/wiki/19P/Borrelly", "description": "Comet Borrelly  or Borrelly's Comet (official designation: 19P/Borrelly) is a periodic comet, which was visited by the spacecraft Deep Space 1 in 2001. The comet last came to perihelion (closest approach to the Sun) on February 1, 2022 and will next come to perihelion on December 11, 2028.\nDeep Space 1 returned images of the comet's nucleus from 3400 kilometers away. At 45 meters per pixel, it was the highest resolution view ever seen of a comet.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 19P/Borrelly is a planet. The definition of a planet specifies that it is a rocky or gaseous body that revolves in approximately elliptical orbits around the sun and is visible by its reflected light. While 19P/Borrelly does revolve around the sun, it is specifically identified as a comet, not a planet. Comets and planets are distinct categories of celestial bodies, with comets typically being composed of ice, dust, and rocky material, rather than being primarily rocky or gaseous. Furthermore, the definition of a planet includes specific examples, all of which are larger bodies than 19P/Borrelly. Therefore, based on the provided definition, 19P/Borrelly cannot be classified as a planet.", "predicted": "negative"}]}, {"classification_procedure": {"id": "IAU 2006-08-16", "term": "planet", "definition": "A planet is a celestial body that (a) has sufficient mass for its self-gravity to \novercome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, \nand (b) is in orbit around a star, and is neither a star nor a satellite of a planet.", "reference": "https://www.iau.org/news/pressreleases/detail/iau0601/", "model_name": "gpt-4", "temperature": 0.1}, "results": [{"id": "http://www.wikidata.org/entity/Q18649725", "name": "CoRoT-19b", "article": "https://en.wikipedia.org/wiki/CoRoT-19b", "description": "CoRoT-19b is a transiting exoplanet found by the CoRoT space telescope in 2011.", "actual": "positive", "rationale": "The description of CoRoT-19b states that it is a transiting exoplanet. An exoplanet is a planet that orbits a star outside the solar system, which aligns with part (b) of the definition of a planet that it should be in orbit around a star. The term \"planet\" in \"exoplanet\" also implies that it has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, which aligns with part (a) of the definition. Therefore, based on the provided definition, CoRoT-19b can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q85765171", "name": "HIP 65426 b", "article": "https://en.wikipedia.org/wiki/HIP_65426_b", "description": "HIP 65426 b, formally named Najsakopajk, is a super-Jupiter exoplanet orbiting the star HIP 65426. It was discovered on 6 July 2017 by the SPHERE consortium using the Spectro-Polarimetric High-Contrast Exoplanet Research (SPHERE) instrument belonging to the European Southern Observatory (ESO). It is 385 light-years from Earth. It is the first planet discovered by ESO's SPHERE instrument.", "actual": "positive", "rationale": "HIP 65426 b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically the star HIP 65426. The description does not explicitly state that HIP 65426 b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but this can be inferred from the fact that it is classified as a super-Jupiter exoplanet, which implies a large mass. Furthermore, it is not a star itself nor is it a satellite of another planet. Therefore, based on the provided definition, HIP 65426 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q42956220", "name": "OGLE-2016-BLG-1190Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2016-BLG-1190Lb", "description": "OGLE-2016-BLG-1190Lb is an extremely massive exoplanet, with a mass about 13.4 times that of Jupiter (MJ), or is, possibly, a low mass brown dwarf, orbiting the G-dwarf star OGLE-2016-BLG-1190L, located about 22,000 light years from Earth, in the constellation of Sagittarius, in the galactic bulge of the Milky Way.\u201cSince the existence of the brown dwarf desert is the signature of different formation mechanisms for stars and planets, the extremely close proximity of OGLE-2016-BLG-1190Lb to this desert raises the question of whether it is truly a \u2018planet\u2019 (by formation mechanism) and therefore reacts back upon its role tracing the galactic distribution of planets,\\\" according to astronomers reporting the findings.", "actual": "positive", "rationale": "OGLE-2016-BLG-1190Lb can be considered a planet based on the provided definition. Firstly, it has a mass that is 13.4 times that of Jupiter, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Secondly, it is in orbit around a star, specifically the G-dwarf star OGLE-2016-BLG-1190L. Lastly, it is neither a star itself nor a satellite of a planet. Therefore, according to the given definition, OGLE-2016-BLG-1190Lb can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q19672944", "name": "Kepler-56c", "article": "https://en.wikipedia.org/wiki/Kepler-56c", "description": "Kepler-56c is a hot Jupiter (a class of exoplanets) orbiting the star Kepler-56, located in the constellation Cygnus. It was discovered by the Kepler telescope in October 2013. It orbits its parent star only 0.17 AU (16 million mi; 25 million km) away; at its distance, it completes an orbit once every 21.4 days. Its orbit is significantly misaligned with its parent star's equator.Both Kepler-56b and Kepler-56c will be devoured by their parent star in about 130 and 155 million years, respectively. Further research shows that it will have its atmosphere boiled away by intense heat from the star, and it will be stretched by the strengthening stellar tides.", "actual": "positive", "rationale": "Kepler-56c fits the definition of a planet as it is a celestial body that has sufficient mass to assume a hydrostatic equilibrium (nearly round) shape, as indicated by its classification as a hot Jupiter, a type of exoplanet. Additionally, it is in orbit around a star, specifically Kepler-56, and is not a star itself or a satellite of another planet. Therefore, based on the provided definition, Kepler-56c can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q597170", "name": "HD 28185 b", "article": "https://en.wikipedia.org/wiki/HD_28185_b", "description": "HD 28185 b is an extrasolar planet 128 light-years away from Earth in the constellation of Eridanus. The planet was discovered orbiting the Sun-like star HD 28185 in April 2001 as a part of the CORALIE survey for southern extrasolar planets, and its existence was independently confirmed by the Magellan Planet Search Survey in 2008. HD 28185 b orbits its sun in a circular orbit that is at the inner edge of its star's habitable zone.", "actual": "positive", "rationale": "HD 28185 b fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically the Sun-like star HD 28185. The description does not explicitly state that HD 28185 b has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, but it is implied by the fact that it is referred to as a planet and not a star or a satellite of a planet. Furthermore, its existence was confirmed by the Magellan Planet Search Survey, which is specifically designed to find planets. Therefore, based on the provided definition and the information given, it can be argued that HD 28185 b is indeed a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5629302", "name": "HD 16175 b", "article": "https://en.wikipedia.org/wiki/HD_16175_b", "description": "HD 16175 b is an exoplanet located approximately 195.7 light-years away in the constellation of Andromeda, orbiting the star HD 16175. This planet has a minimum mass 4.8 times that of Jupiter; the true mass was initially unknown since the inclination of the orbit was unknown. This planet orbits at about 2.2 astronomical units, taking 2.73 years to revolve around the star. The orbit of the planet is highly elliptical with an eccentricity of 0.64. In 2023, the inclination and true mass of HD 16175 b were determined via astrometry.The planet HD 16175 b is named Abol. The name was selected in the NameExoWorlds campaign by Ethiopia, during the 100th anniversary of the IAU. Abol is the first of three rounds of coffee in the Ethiopian traditional coffee ceremony.", "actual": "positive", "rationale": "HD 16175 b fits the definition of a planet because it is a celestial body that orbits a star, specifically the star HD 16175. It is not a star itself, nor is it a satellite of another planet. Additionally, it has a mass that is 4.8 times that of Jupiter, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. The fact that it takes 2.73 years to revolve around its star also indicates that it is in a stable orbit. Therefore, based on the provided definition, HD 16175 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1074458", "name": "HD 155358 c", "article": "https://en.wikipedia.org/wiki/HD_155358_c", "description": "HD 155358 c is an extrasolar planet orbiting the star HD 155358 located 142 light years away in the constellation Hercules. This is a gas giant which orbits at 1.224 AU and takes 530.3 days to orbit HD 155358. This planet orbits in an eccentric orbit. This planet has at least half the mass of Jupiter.", "actual": "positive", "rationale": "HD 155358 c fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically the star HD 155358. It is not a star itself, nor is it a satellite of another planet. Additionally, it is described as a gas giant, which suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium (nearly round) shape. Therefore, based on the provided definition, HD 155358 c can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1146974", "name": "HAT-P-9b", "article": "https://en.wikipedia.org/wiki/HAT-P-9b", "description": "HAT-P-9b, formally named Alef, is an exoplanet approximately 1500 light years away in the constellation Auriga. This planet was found by the transit method on June 26, 2008. It has a mass 78% that of Jupiter and a radius 140% that of Jupiter. As with most transiting planets, this planet is a hot Jupiter, meaning this Jupiter-like planet orbits extremely close to its parent star, taking only 3.92 days to orbit.The study in 2012, utilizing a Rossiter\u2013McLaughlin effect, have determined the planetary orbit is mildly misaligned with the rotational axis of the star, misalignment equal to -16\u00b18\u00b0.The name Alef was selected in the NameExoWorlds campaign by Israel, during the 100th anniversary of the IAU. Alef is the first letter in the Hebrew alphabet and also means bull.", "actual": "positive", "rationale": "HAT-P-9b, or Alef, fits the definition of a planet as it is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces, which is evident from its nearly round shape. This is indicated by its comparison to Jupiter in terms of mass and radius. Additionally, it is in orbit around a star, as it takes only 3.92 days to orbit its parent star. It is neither a star itself nor a satellite of a planet, as there is no information suggesting that it is either of these. Therefore, based on the provided definition, HAT-P-9b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1039917", "name": "HD 49674 b", "article": "https://en.wikipedia.org/wiki/HD_49674_b", "description": "HD 49674 b, formally named Eburonia, is an extrasolar planet located approximately 134 light-years away in the constellation of Auriga, orbiting the star HD 49674. This planet was discovered orbiting the star in 2002. The planet is a gas giant and orbits extremely close to its star, which takes only 4.95 days to revolve.HD 49674 b, along with its parent star, was chosen as part of the 2019 NameExoWorlds campaign organised by the International Astronomical Union in which each country was assigned a star and planet to be named.  The HD 49674 system was assigned to Belgium.  The winning proposal named HD 49674 b Eburonia and the parent star Nervia, both after prominent Belgic tribes, the Eburones and Nervii respectively.", "actual": "positive", "rationale": "HD 49674 b fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically the star HD 49674. The description does not explicitly state that HD 49674 b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but it is referred to as a gas giant, which implies that it has a significant mass and is likely nearly round in shape. Furthermore, it is not a star itself, nor is it a satellite of another planet. Therefore, based on the provided definition, HD 49674 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q85058985", "name": "HAT-P-11c", "article": "https://en.wikipedia.org/wiki/HAT-P-11c", "description": "HAT-P-11c is a gas giant exoplanet that orbits HAT-P-11, a K-type star. Its mass is 2.3 Jupiters, it takes 9.3 years to complete one orbit of its star, and is 4.13 AU from its star. Its discovery was announced in 2018.", "actual": "positive", "rationale": "HAT-P-11c fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically a K-type star called HAT-P-11. The description does not specify its shape, but as a gas giant, it can be inferred that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium (nearly round) shape. It is also not described as a star or a satellite of another planet, further supporting its classification as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q11717218", "name": "Kepler-62d", "article": "https://en.wikipedia.org/wiki/Kepler-62d", "description": "Kepler-62d (also known by its Kepler Object of Interest designation KOI-701.01) is the third innermost and the largest exoplanet discovered orbiting the star Kepler-62, with a size roughly twice the diameter of Earth. It was found using the transit method, in which the dimming that a planet causes as it crosses in front of its star is measured. Its stellar flux is 15 \u00b1 2 times Earth's. Due to its closer orbit to its star, it is a super-Venus or, if it has a volatile composition, a hot Neptune, with an estimated equilibrium temperature of 510 K (237 \u00b0C; 458 \u00b0F), too hot to sustain life on its surface.", "actual": "positive", "rationale": "Kepler-62d fits the definition of a planet because it is a celestial body that has sufficient mass to assume a nearly round shape, as indicated by its description as the largest exoplanet discovered orbiting the star Kepler-62. Furthermore, it is in orbit around a star, specifically Kepler-62, and is not a star itself or a satellite of another planet. Therefore, based on the provided definition, Kepler-62d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5177665", "name": "HD 164604 b", "article": "https://en.wikipedia.org/wiki/HD_164604_b", "description": "HD 164604 b is an extrasolar planet discovered in January 2010 in association with the Magellan Planet Search Program. It has a minimum mass 2.7 times the mass of Jupiter and an orbital period of 606.4 days. Its star is classified as a K2 V dwarf and is roughly 124 light-years away from Earth.HD 164604 b is named Caleuche. The name was selected in the NameExoWorlds campaign by Chile, during the 100th anniversary of the IAU. Caleuche is a large ghost ship from southern Chilean mythology which sails the seas around the island of Chilo\u00e9 at night.An astrometric measurement of the planet's inclination and true mass was published in 2022 as part of Gaia DR3.", "actual": "positive", "rationale": "HD 164604 b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically a K2 V dwarf star. The description does not explicitly state that HD 164604 b has a nearly round shape due to its self-gravity overcoming rigid body forces, but it can be inferred from the fact that it has a minimum mass 2.7 times the mass of Jupiter, which is a known planet with a round shape. Furthermore, HD 164604 b is not described as being a star or a satellite of a planet, further supporting the assertion that it is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q391576", "name": "HD 40307 f", "article": "https://en.wikipedia.org/wiki/HD_40307_f", "description": "HD 40307 f is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus  by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of G\u00f6ttingen, Germany. The existence of planet was confirmed in 2015.", "actual": "positive", "rationale": "HD 40307 f fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically the star HD 40307. The fact that it was discovered by the radial velocity method suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, although the description does not explicitly state this. It is also stated that HD 40307 f is not a star itself, and there is no information suggesting that it is a satellite of another planet. Therefore, based on the provided definition and information, HD 40307 f can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q842110", "name": "Gliese 436 b", "article": "https://en.wikipedia.org/wiki/Gliese_436_b", "description": "Gliese 436 b  (sometimes called GJ 436 b, formally named Awohali) is a Neptune-sized exoplanet orbiting the red dwarf Gliese 436. It was the first hot Neptune discovered with certainty (in 2007) and was among the smallest-known transiting planets in mass and radius, until the much smaller Kepler exoplanet discoveries began circa 2010.\nIn December 2013, NASA reported that clouds may have been detected in the atmosphere of GJ 436 b.", "actual": "positive", "rationale": "Gliese 436 b fits the definition of a planet because it is a celestial body that has sufficient mass to assume a hydrostatic equilibrium shape, as indicated by its description as a Neptune-sized exoplanet. This suggests that its self-gravity has overcome rigid body forces to form a nearly round shape. Additionally, Gliese 436 b is in orbit around a star, specifically the red dwarf Gliese 436, which aligns with the second part of the planet definition. Finally, it is neither a star itself nor a satellite of another planet, as it is described as an exoplanet, which is a planet located outside of our solar system. Therefore, based on the provided definition, Gliese 436 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q946435", "name": "HD 33564 b", "article": "https://en.wikipedia.org/wiki/HD_33564_b", "description": "HD 33564 b is an extrasolar planet located approximately 68 light-years away in the constellation of Camelopardalis. This planet orbits around F6V star HD 33564. The planet has an eccentric orbit, ranging in distance from 0.737 AU at periastron to 1.497 AU at apastron.\nHD 33564 b is a gas giant in a habitable zone of its star. Based on a probable 10\u22124 fraction of the planet mass as a satellite, it can have a Mars-sized moon with habitable surface. On the other hand, this mass can be distributed into many small satellites as well.", "actual": "positive", "rationale": "HD 33564 b fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically the F6V star HD 33564. The description does not explicitly state that HD 33564 b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but it is implied by the fact that it is referred to as a gas giant, a term typically used to describe large, round planets. Furthermore, it is not a star itself, nor is it a satellite of another planet, as it orbits a star directly. Therefore, based on the provided definition, HD 33564 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1329165", "name": "HD 4308 b", "article": "https://en.wikipedia.org/wiki/HD_4308_b", "description": "HD 4308 b is a low-mass exoplanet orbiting around HD 4308. It is believed to have almost no orbital eccentricity.", "actual": "positive", "rationale": "HD 4308 b can be considered a planet based on the provided definition. The description states that HD 4308 b is a celestial body that orbits around a star, HD 4308, which aligns with part (b) of the definition. Although the description does not explicitly state that HD 4308 b has sufficient mass to overcome rigid body forces and assume a nearly round shape, the term \"exoplanet\" implies that it meets this criterion, as exoplanets are a type of planet. Furthermore, the description does not suggest that HD 4308 b is a star or a satellite of a planet, which means it does not fall into the categories excluded by the definition. Therefore, based on the information provided, it is reasonable to assert that HD 4308 b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5176581", "name": "HD 181433 d", "article": "https://en.wikipedia.org/wiki/HD_181433_d", "description": "HD 181433 d is an extrasolar planet located approximately 87 light years away in the constellation of Pavo, orbiting the star HD 181433. This planet has a minimum mass of 0.54 Jupiter mass and takes 2172 days to orbit the star. The average orbital distance is 3.00 AU. At periastron distance, it will have distance from the star similar to Mars\u2019 distance from the Sun at 1.56 AU. At apastron, the distance is 4.44 AU. These corresponds to the orbital eccentricity of 0.48.", "actual": "positive", "rationale": "HD 181433 d fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically the star HD 181433. The description does not explicitly state that HD 181433 d has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but it does mention that it has a minimum mass of 0.54 Jupiter mass, which suggests that it is likely to have sufficient mass to meet this criterion. Furthermore, the description does not indicate that HD 181433 d is a star or a satellite of a planet, which further supports the assertion that it is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q843038", "name": "HD 171028 b", "article": "https://en.wikipedia.org/wiki/HD_171028_b", "description": "HD 171028 b is a >1.83 MJ exoplanet orbiting very eccentrically around HD 171028. The period is 1.47 years and semi-major axis of 1.29 AU. The Geneva Extrasolar Planet Search team announced the discovery of planet on July 13, 2007.", "actual": "positive", "rationale": "HD 171028 b can be considered a planet based on the provided definition. Firstly, it is a celestial body with a mass greater than 1.83 MJ, which suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Secondly, it is in orbit around a star, specifically HD 171028, which aligns with the second part of the definition. Lastly, there is no information suggesting that HD 171028 b is a star or a satellite of a planet, thus it can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q45747608", "name": "Kepler-90i", "article": "https://en.wikipedia.org/wiki/Kepler-90i", "description": "Kepler-90i  (also known by its Kepler Object of Interest designation KOI-351.08) is a super-Earth exoplanet with a radius 1.32  times that of Earth, orbiting the early G-type main sequence star Kepler-90 every 14.45 days, discovered by NASA's Kepler spacecraft. It is located about 2,840 light-years (870 parsecs, or nearly 2.4078\u00d71016 km) from Earth in the constellation Draco. The exoplanet is the eighth in the star's multiplanetary system. As of December 2017, Kepler-90 is the star hosting the most exoplanets found. Kepler-90i was found with the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured, and by a newly utilized computer tool, deep learning, a class of machine learning algorithms.", "actual": "positive", "rationale": "Kepler-90i fits the definition of a planet as it is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces, assuming a nearly round shape. This is indicated by its description as a super-Earth exoplanet with a radius 1.32 times that of Earth. Additionally, Kepler-90i is in orbit around a star, specifically the early G-type main sequence star Kepler-90. It is neither a star itself nor a satellite of a planet, as it is described as an exoplanet, which is a planet located outside of our solar system. Therefore, based on the provided definition, Kepler-90i can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q4039904", "name": "HD 212771 b", "article": "https://en.wikipedia.org/wiki/HD_212771_b", "description": "HD 212771 b is an extrasolar planet orbiting the G-type star HD 212771 approximately 364 light years away in the constellation Aquarius.", "actual": "positive", "rationale": "The definition of a planet states that it is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it orbits around a star without being a star itself or a satellite of another planet. The description of HD 212771 b indicates that it is an extrasolar planet orbiting a star (HD 212771), and it is not mentioned to be a star itself or a satellite of another planet. Therefore, based on the provided definition, HD 212771 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1369113", "name": "OGLE-2006-BLG-109Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2006-BLG-109Lb", "description": "OGLE-2006-BLG-109Lb is an extrasolar planet approximately 4,920 light-years away in the constellation of Sagittarius.  The planet was detected orbiting the star OGLE-2006-BLG-109L in 2008 by a research team using Microlensing.", "actual": "positive", "rationale": "OGLE-2006-BLG-109Lb fits the definition of a planet because it is in orbit around a star, specifically the star OGLE-2006-BLG-109L. The description does not provide information about its shape or whether it has sufficient mass for self-gravity to overcome rigid body forces, but it does not contradict these aspects of the definition either. Furthermore, it is not described as a star or a satellite of a planet, which also aligns with the definition of a planet. Therefore, based on the provided information, it can be argued that OGLE-2006-BLG-109Lb is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q841758", "name": "HD 68988 b", "article": "https://en.wikipedia.org/wiki/HD_68988_b", "description": "HD 68988 b is a hot jupiter located approximately 192 light-years away in the constellation of Ursa Major, orbiting the star HD 68988 in a moderately eccentric orbit.The planet HD 68988 b is called Albmi. The name was selected in the NameExoWorlds campaign by Norway, during the 100th anniversary of the IAU. Albmi means sky in the Northern Sami language.", "actual": "positive", "rationale": "The description of HD 68988 b indicates that it is a celestial body that is in orbit around a star, specifically the star HD 68988. This aligns with part (b) of the definition of a planet. While the description does not explicitly state that HD 68988 b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, the fact that it is referred to as a \"hot jupiter\" suggests that it is a large, gaseous body, which typically have sufficient mass to meet this criterion. Therefore, it can be argued that HD 68988 b fits the definition of a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1328119", "name": "WASP-11b/HAT-P-10b", "article": "https://en.wikipedia.org/wiki/WASP-11b/HAT-P-10b", "description": "WASP-11b/HAT-P-10b or WASP-11Ab/HAT-P-10Ab is an extrasolar planet discovered in 2008. The discovery was announced (under the designation WASP-11b) by press release by the SuperWASP project in April 2008 along with planets WASP-6b through to WASP-15b, however at this stage more data was needed to confirm the parameters of the planets and the coordinates were not given. On 26 September 2008, the HATNet Project's paper describing the planet which they designated HAT-P-10b appeared on the arXiv preprint server. The SuperWASP team's paper appeared as a preprint on the Extrasolar Planets Encyclopaedia on the same day, confirming that the two objects (WASP-11b and HAT-P-10b) were in fact the same, and the teams agreed to use the combined designation.The planet has the third lowest insolation of the known transiting planets (only Gliese 436 b and HD 17156 b have lower insolation). The temperature implies it falls into the pL class of hot Jupiters: planets which lack significant quantities of titanium(II) oxide and vanadium(II) oxide in their atmospheres and do not have temperature inversions. An alternative classification system for hot Jupiters is based on the equilibrium temperature and the planet's Safronov number. In this scheme, for a given temperature, class I planets have high Safronov numbers and tend to be in orbit around cooler host stars, while class II planets have lower Safronov numbers. In the case of WASP-11b/HAT-P-10b, the equilibrium temperature is 1030 K and the Safronov number is 0.047\u00b10.003, which means it is located close to the dividing line between the class I and class II planets.The planet is in a binary star system, the second star is WASP-11 B, with a mass 0.34 \u00b10.05 of the Sun and a 3483 \u00b143 temperature.", "actual": "positive", "rationale": "WASP-11b/HAT-P-10b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically, it is in a binary star system with the second star being WASP-11 B. The description does not explicitly state that it has a nearly round shape due to its self-gravity overcoming rigid body forces, but it is implied as it is classified as a hot Jupiter, which are known to be gas giants with a round shape. Furthermore, it is neither a star nor a satellite of a planet, as it is clearly identified as an extrasolar planet. Therefore, based on the provided definition, WASP-11b/HAT-P-10b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q7946763", "name": "WASP-28b", "article": "https://en.wikipedia.org/wiki/WASP-28b", "description": "WASP-28b or K2-1b is an extrasolar planet discovered in 2010 by the Wide Angle Search for Planets (WASP) project orbiting WASP-28, a magnitude 12 star also known as 1SWASP J233427.87-013448.1, 2MASS J23342787-0134482 and K2-1. Since it orbits its star very closely, the planet is a strongly irradiated hot Jupiter. As seen from the Earth, WASP-28b transits its host star every 3.41 days taking about 3 hours to do so.The planet was observed by the Kepler spacecraft during the K2 mission engineering campaign in February 2014 as part of an early science demonstration. It was also observed from December 2016 to March 2017 during K2's campaign 12 which allowed a refinement of the system parameters.", "actual": "positive", "rationale": "WASP-28b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically WASP-28. The description does not explicitly state that WASP-28b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but it is implied as it is referred to as a planet and not a star or a satellite of a planet. Furthermore, it is not a star itself as it orbits around WASP-28, and it is not a satellite of a planet as it is not mentioned to be orbiting any planet. Therefore, based on the provided definition and the information given, WASP-28b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q429564", "name": "OGLE-2005-BLG-071Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2005-BLG-071Lb", "description": "OGLE-2005-BLG-071Lb is a planet discovered by the Optical Gravitational Lensing Experiment (OGLE) and others in 2005, using gravitational microlensing. According to the best fit model, it has about 3.5 times the mass of Jupiter and a projected separation of 3.6 astronomical units from the star. This would result in an effective temperature around 50 K, similar to that of Neptune. However, an alternative model which gives a slightly lower mass of 3.3 times that of Jupiter and a projected separation of 2.1 AU is only slightly less likely. It may be the most massive planet currently known around a red dwarf star (though only lower limits are known for those planets detected by the radial velocity method).", "actual": "positive", "rationale": "OGLE-2005-BLG-071Lb fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically a red dwarf star. The description does not explicitly state that it has a nearly round shape due to its self-gravity overcoming rigid body forces, but this can be inferred from the fact that it has a mass of about 3.5 times that of Jupiter, which is a known planet with a round shape. Furthermore, it is not described as a star or a satellite of a planet, further supporting the assertion that OGLE-2005-BLG-071Lb is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1252981", "name": "HD 113538 c", "article": "https://en.wikipedia.org/wiki/HD_113538_c", "description": "HD 113538 c is an exoplanet approximately 51 light years away from Earth in the constellation Centaurus. It orbits its star (HD 113538) once every 1657 days, placing it in the outer edge of the habitable zone. However it is most likely a gas giant with no solid surface.", "actual": "positive", "rationale": "HD 113538 c fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically HD 113538. The description does not provide information about its shape or whether it has overcome rigid body forces to assume a hydrostatic equilibrium shape, but it does not contradict these criteria either. It is also stated that HD 113538 c is not a star, and there is no information suggesting that it is a satellite of another planet. Therefore, based on the information provided, it can be argued that HD 113538 c is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q2593320", "name": "OGLE-2007-BLG-368Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2007-BLG-368Lb", "description": "OGLE-2007-BLG-368Lb is an extrasolar planet located approximately 19,230 light-years away in the constellation of Scorpius, orbiting the star OGLE-2007-BLG-368L. This planet was detected on December 8, 2009 by the gravitational microlensing by Sumi. It has mass 6.94% of Jupiter (i.e. 22 times that of Earth) and is located 3.3 AU from the star when observed. Based on those properties it would classify as a Cold Neptune. It is the second Cold Neptune to be observed, the first being OGLE-2005-BLG-169Lb. This planet is most likely be similar to Uranus and Neptune in the Solar System in terms of atmospheric and internal properties.", "actual": "positive", "rationale": "OGLE-2007-BLG-368Lb fits the definition of a planet on several counts. Firstly, it has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, as indicated by its mass of 6.94% of Jupiter, or 22 times that of Earth. This suggests that it is nearly round in shape. Secondly, it is in orbit around a star, specifically the star OGLE-2007-BLG-368L. Thirdly, it is neither a star itself nor a satellite of a planet, as it is described as an extrasolar planet. Therefore, based on the provided definition, OGLE-2007-BLG-368Lb can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q3124868", "name": "HIP 78530 b", "article": "https://en.wikipedia.org/wiki/HIP_78530_b", "description": "HIP 78530 b is an object that is either a planet or a brown dwarf in the orbit of the star HIP 78530. It was observed as early as 2000, but the object was not confirmed as one in orbit of the star HIP 78530 until a direct imaging project photographed the star in 2008. The image caught the attention of the project's science team, so the team followed up on its initial observations. HIP 78530 b orbits a young, hot, bright blue star in the Upper Scorpius association. The planet itself is over twenty-three times more massive than Jupiter, orbiting eighteen times further from its host star than Pluto does from the Sun by the estimates published in its discovery paper. In this predicted orbit, HIP 78530 b completes an orbit every twelve thousand years.", "actual": "positive", "rationale": "HIP 78530 b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, specifically the star HIP 78530. This satisfies the second part of the definition. Secondly, while the description does not explicitly state that HIP 78530 b has a nearly round shape due to its self-gravity overcoming rigid body forces, it is implied by the fact that it is either a planet or a brown dwarf. Both of these types of celestial bodies typically have this characteristic. Lastly, it is not a star itself nor is it a satellite of a planet, which aligns with the final part of the definition. Therefore, based on the provided definition, HIP 78530 b can be argued to be a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q4039960", "name": "HD 85390 b", "article": "https://en.wikipedia.org/wiki/HD_85390_b", "description": "HD 85390 b (also known as HIP 48235 b) is an extrasolar planet which orbits the G-type main sequence star HD 85390, located approximately 106 light years away.\nThe planet HD 85390 b is named Madalitso. The name was selected in the NameExoWorlds campaign by Zambia, during the 100th anniversary of the IAU. Madalitso means blessings in the native language of Nyanja in Zambia.", "actual": "positive", "rationale": "The description of HD 85390 b aligns with the definition of a planet. It is an extrasolar planet, which implies that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Additionally, it is stated that HD 85390 b orbits the G-type main sequence star HD 85390, which satisfies the condition of being in orbit around a star. Lastly, there is no information suggesting that HD 85390 b is a star or a satellite of a planet, thus it fits the definition of a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q19672936", "name": "Kepler-56b", "article": "https://en.wikipedia.org/wiki/Kepler-56b", "description": "Kepler-56b (KOI-1241.02) is a hot Neptune\u2014a class of exoplanets\u2014located roughly 3,060 light-years (940 parsecs) away. It is somewhat larger than Neptune and orbits its parent star Kepler-56 and was discovered in 2013 by the Kepler Space Telescope.", "actual": "positive", "rationale": "Kepler-56b can be considered a planet based on the provided definition. Firstly, it is a celestial body that has a nearly round shape, indicating that it has sufficient mass for its self-gravity to overcome rigid body forces and achieve hydrostatic equilibrium. Secondly, it is in orbit around a star, specifically its parent star Kepler-56. Lastly, it is neither a star itself nor a satellite of another planet. Therefore, according to the given definition, Kepler-56b qualifies as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q849161", "name": "HD 153950 b", "article": "https://en.wikipedia.org/wiki/HD_153950_b", "description": "HD 153950 b, also known as Trimobe, is an extrasolar planet located approximately 162 light-years away. This planet was discovered on October 26, 2008 by Moutou et al. using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile.The planet HD 153950 b is named Trimobe. The name was selected in the NameExoWorlds campaign by Madagascar, during the 100th anniversary of the IAU. Trimobe is a rich ogre from Malagasy tales.", "actual": "positive", "rationale": "HD 153950 b can be considered a planet based on the provided definition. The description states that HD 153950 b is an extrasolar planet, which implies that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Additionally, it is mentioned that HD 153950 b is in orbit around a star, which aligns with the second part of the definition. There is no information suggesting that HD 153950 b is a star or a satellite of a planet, therefore it can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q53616218", "name": "K2-155d", "article": "https://en.wikipedia.org/wiki/K2-155d", "description": "K2-155d is a potentially habitable Super-Earth exoplanet in the K2-155 system. It is the outermost of three known planets orbiting around the K-type star K2-155 in the constellation Taurus. It is one of 15 new exoplanets around red dwarf stars discovered by Japanese astronomer \\\"Teruyuki Hirano\\\" of the Tokyo Institute of Technology and his team. The team used data from NASA's Kepler Space Telescope during its extended K2 \\\"Second Light\\\" mission. K2-155d orbits near the so-called habitable zone of its system, and has the potential to host liquid water.", "actual": "positive", "rationale": "K2-155d can be classified as a planet based on the provided definition. Firstly, it is a celestial body that has a nearly round shape, indicating that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium. Secondly, it is in orbit around a star, specifically the K-type star K2-155. Lastly, it is neither a star itself nor a satellite of a planet, as it is described as an exoplanet, which is a planet located outside of our solar system. Therefore, based on these characteristics, K2-155d meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5096657", "name": "HD 179079 b", "article": "https://en.wikipedia.org/wiki/HD_179079_b", "description": "HD 179079 b is an extrasolar planet which orbits the G-type subgiant star HD 179079, located approximately 228 light years away in the constellation Aquila. This planet has mass only 1/12 that of Jupiter or 1.5 times Neptune. The planet orbits very close to the star, at a distance of 0.11 AU. This planet takes two weeks to revolve around the star. This planet was discovered using the Keck telescopes on August 12, 2009.", "actual": "positive", "rationale": "HD 179079 b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically the G-type subgiant star HD 179079. The description does not provide information about its shape, but given that it has a mass 1/12 that of Jupiter or 1.5 times Neptune, it can be inferred that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium (nearly round) shape. It is also stated that HD 179079 b is not a star itself, and there is no information suggesting that it is a satellite of another planet. Therefore, based on the provided definition and the information given, HD 179079 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q26991323", "name": "OGLE-2007-BLG-349(AB)b", "article": "https://en.wikipedia.org/wiki/OGLE-2007-BLG-349(AB)b", "description": "OGLE-2007-BLG-349(AB)b is a circumbinary extrasolar planet about 8,000 light-years away in the constellation of Sagittarius. It is the first circumbinary exoplanet to be discovered using the microlensing method of detecting exoplanets.", "actual": "positive", "rationale": "OGLE-2007-BLG-349(AB)b fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically, it is a circumbinary extrasolar planet, meaning it orbits two stars. The description does not explicitly state that it has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but this can be inferred from the fact that it is classified as a planet. Furthermore, it is neither a star nor a satellite of a planet, which aligns with the definition of a planet. Therefore, OGLE-2007-BLG-349(AB)b can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q67011452", "name": "HR 5183 b", "article": "https://en.wikipedia.org/wiki/HR_5183_b", "description": "HR 5183 b is an exoplanet located 102.7 light years away in the constellation of Virgo orbiting the star HR 5183. It has a mass of 3.31 MJ. It has a highly eccentric (e\u22430.87) orbit which takes it from within the orbit of Jupiter to beyond the orbit of Neptune, which classifies it as an eccentric Jupiter and it has been nicknamed the \\\"whiplash planet\\\". It was discovered in 2019 based on two decades of radial velocity observations.In 2021, astrometric observations revealed that HR 5183 b has a nearly edge-on orbital inclination, and thus its true mass is close to its minimum mass.", "actual": "positive", "rationale": "HR 5183 b can be classified as a planet based on the provided definition for several reasons. Firstly, it has sufficient mass, as indicated by its mass of 3.31 MJ, which allows it to overcome rigid body forces and assume a hydrostatic equilibrium shape. Secondly, it is in orbit around a star, specifically the star HR 5183. Lastly, it is neither a star itself nor a satellite of another planet. Therefore, according to the given definition, HR 5183 b can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5629357", "name": "HD 5319 b", "article": "https://en.wikipedia.org/wiki/HD_5319_b", "description": "HD 5319 b is a gas giant exoplanet discovered in 2007 in the constellation of Cetus. This planet has a minimum mass nearly two times that of Jupiter. The planet has an almost circular orbit, with an eccentricity of only 0.02 and a period of 641 days. An additional planet in the system was discovered in 2015 and may be in a 4:3 mean motion resonance with planet b.", "actual": "positive", "rationale": "HD 5319 b fits the definition of a planet as it is a celestial body that has sufficient mass to assume a nearly round shape, as indicated by its classification as a gas giant. Additionally, it is in orbit around a star, as evidenced by its location in the constellation of Cetus. It is not a star itself, nor is it a satellite of a planet, as it has its own orbit and there is no mention of it being a moon of another planet. Therefore, based on the provided definition, HD 5319 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q111723950", "name": "Nbu", "article": "https://en.wikipedia.org/wiki/Nbu", "description": "In Mandaeism, \u02bfNbu (Classical Mandaic: \u084f\u084d\u0841\u0845) or Nbu is the Mandaic name for the planet Mercury. Nbu is one of the seven planets (Classical Mandaic: \u0854\u0845\u0841\u0840, romanized: \u0161uba, lit.\u2009'The Seven'), who are part of the entourage of Ruha in the World of Darkness. This name was borrowed from the Mesopotamian god called Nabu.Nbu is associated with learning and scribes, as well as Christ and Christianity. Other names for Nbu include Maqurpiil, M\u0161iha (i.e., Jesus the Messiah), and \u02bfa\u1e6darid (of Arabic origin). Nbu's name is derived from the Akkadian Nab\u00fb.Buckley (2010) suggests a connection between Dinanukht and Nbu. For instance, in the Zrazta \u1e0f-Hibil Ziwa (Drower Collection Ms. 44), Nbu is the Lord of Book and ink and wisdom. Similarly, Dinanukht is called the \\\"ink-book of the gods\\\" in Right Ginza 6.", "actual": "positive", "rationale": "The description of Nbu clearly states that it is the Mandaic name for the planet Mercury. This directly aligns with the definition of a planet as a celestial body in orbit around a star. Furthermore, the description does not suggest that Nbu is a star or a satellite of a planet, which further supports the assertion that Nbu is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5371571", "name": "HD 45652 b", "article": "https://en.wikipedia.org/wiki/HD_45652_b", "description": "HD 45652 b, also named Viriato, is a gas giant extrasolar planet orbiting at only 0.23 AU from the star HD 45652, with an orbital period of 44 days.  It has mass at least half that of Jupiter.  As it was detected using the radial velocity method, its true mass is dependent on the inclination of its orbit; if it is low, then the true mass will be larger.  Also, its radius is not known.  This planet was discovered by measurements taken by the ELODIE spectrograph from 2005 and 2006, and later confirmed by CORALIE and SOPHIE between 2006 and 2007.  The discovery was announced in May 2008.", "actual": "positive", "rationale": "HD 45652 b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically the star HD 45652. It is not a star itself, nor is it a satellite of another planet. It is also assumed to have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, as it is described as a gas giant, which are known to be nearly round in shape. The fact that its mass is at least half that of Jupiter further supports this. Therefore, based on the provided definition, HD 45652 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1140454", "name": "HD 80606 b", "article": "https://en.wikipedia.org/wiki/HD_80606_b", "description": "HD 80606 b (also Struve 1341 Bb or HIP 45982 b) is an eccentric hot Jupiter 217 light-years from the Sun in the constellation of Ursa Major. HD 80606 b was discovered orbiting the star HD 80606 in April 2001 by a team led by Michel Mayor and Didier Queloz. With a mass 4 times that of Jupiter, it is a gas giant. Because the planet transits the host star its radius can be determined using the transit method and was found to be slightly smaller than Jupiter's. Its density is slightly less than Earth's. It has an extremely eccentric orbit like a comet, with its orbit taking it very close to its star and then back out very far away from it every 111 days.", "actual": "positive", "rationale": "HD 80606 b fits the definition of a planet as it is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces, which is evident from its nearly round shape. It is also in orbit around a star, specifically the star HD 80606. It is not a star itself, nor is it a satellite of a planet, but a gas giant with a mass 4 times that of Jupiter. Therefore, based on the provided definition, HD 80606 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5178221", "name": "HD 24040 b", "article": "https://en.wikipedia.org/wiki/HD_24040_b", "description": "HD 24040 b is a long-period exoplanet taking approximately 3500 days to orbit at 4.6 astronomical units in an almost circular orbit. It has a minimum mass 4 times that of Jupiter.", "actual": "positive", "rationale": "HD 24040 b fits the definition of a planet because it meets both criteria outlined in the definition. Firstly, it has a minimum mass 4 times that of Jupiter, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Secondly, it is in orbit around a star, taking approximately 3500 days to complete one orbit. The description does not suggest that HD 24040 b is a star or a satellite of a planet, therefore it can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q849267", "name": "42 Draconis b", "article": "https://en.wikipedia.org/wiki/42_Draconis_b", "description": "42 Draconis b (abbreviated 42 Dra b), formally named Orbitar , is a candidate extrasolar planet located approximately 315 light years from Earth in the constellation of Draco. It orbits the 5th magnitude K-type giant star 42 Draconis with a period of 479 days and 38% orbital eccentricity. The planet was discovered using the radial velocity method on March 20, 2009.Following its discovery the planet was designated 42 Draconis b. In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Orbitar for this planet. The winning name was submitted by the Brevard Astronomical Society of Brevard County, Florida, United States. Orbitar is a contrived word paying homage to the space launch and orbital operations of NASA.A 2021 study found that more recent radial velocity measurements of 42 Draconis were inconsistent with the proposed planetary orbit, casting serious doubt on 42 Draconis b's existence, but with a two-planet solution still being a possibility. The study suggests that the radial velocity signal is likely caused by a yet unknown stellar phenomenon, which might be common in giant stars.", "actual": "positive", "rationale": "42 Draconis b, also known as Orbitar, fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically the K-type giant star 42 Draconis. It was discovered using the radial velocity method, which is a technique used to detect extrasolar planets and measure their velocity. This suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Although there is some doubt about its existence due to inconsistent radial velocity measurements, the possibility of it being a planet is still considered. Therefore, based on the provided definition, 42 Draconis b can be argued to be a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q89514491", "name": "HD 177565 b", "article": "https://en.wikipedia.org/wiki/HD_177565_b", "description": "HD 177565 b is an extrasolar planet orbiting the G-type main-sequence star HD 177565 55.3 light-years away from the Solar System.", "actual": "positive", "rationale": "The definition of a planet states that it must be a celestial body that has sufficient mass to maintain a nearly round shape due to its self-gravity, and it must be in orbit around a star without being a star itself or a satellite of another planet. The description of HD 177565 b indicates that it is an extrasolar planet orbiting a star (HD 177565). Therefore, based on the provided definition and the information about HD 177565 b, it can be argued that HD 177565 b is indeed a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q419934", "name": "HD 125612 d", "article": "https://en.wikipedia.org/wiki/HD_125612_d", "description": "HD 125612 d is an extrasolar planet which orbits the G-type main sequence star HD 125612, located approximately 172 light years away in the constellation Virgo. The discovery of this planet was announced by the HARPS team on October 19, 2009, together with 31 other planets, including HD 125612 c.In 2022, the true mass and inclination of HD 125612 d were measured via astrometry.", "actual": "positive", "rationale": "HD 125612 d fits the definition of a planet because it is a celestial body that is in orbit around a star, specifically the G-type main sequence star HD 125612. The description does not explicitly state that HD 125612 d has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but it is implied by the term \"planet\" used to describe it. Furthermore, it is not described as a star or a satellite of a planet, which aligns with the definition of a planet. Therefore, based on the provided definition and the information given, HD 125612 d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q50358884", "name": "WASP-39b", "article": "https://en.wikipedia.org/wiki/WASP-39b", "description": "WASP-39b, officially named  Bocaprins, is a \\\"hot Jupiter\\\" extrasolar planet discovered in February 2011 by the WASP project, notable for containing a substantial amount of water in its atmosphere. In addition WASP-39b was the first exoplanet found to contain carbon dioxide in its atmosphere, and likewise for sulfur dioxide.\nWASP-39b is in the constellation Virgo, and is about 700 light-years from Earth. As part of the NameExoWorlds campaigns at the 100th anniversary of the IAU, the planet was named Bocaprins, after the beach Boca Prins in the Arikok National Park of Aruba.", "actual": "positive", "rationale": "WASP-39b fits the definition of a planet because it is a celestial body that is in orbit around a star, as indicated by its discovery by the WASP project and its location in the constellation Virgo. The description does not explicitly state that WASP-39b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but this can be inferred from the fact that it has a substantial amount of water and other gases in its atmosphere, which would require a significant gravitational pull to retain. Furthermore, it is not described as a star or a satellite of a planet, which further supports the assertion that WASP-39b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q547497", "name": "HD 69830 b", "article": "https://en.wikipedia.org/wiki/HD_69830_b", "description": "HD 69830 b is a Neptune-mass or super-Earth-mass exoplanet orbiting the star HD 69830. It is at least 10 times more massive than Earth. It also orbits very close to its parent star and takes 82/3 days to complete an orbit.\nBased on theoretical modeling in the 2006 discovery paper, this is likely to be a rocky planet, not a gas giant. However, other work has found that if it had formed as a gas giant, it would have stayed that way, and it is now understood that planets this massive are rarely rocky.If HD 69830 b is a terrestrial planet, models predict that tidal heating would produce a heat flux at the surface of about 55 W/m2. This is 20 times that of Io.", "actual": "positive", "rationale": "HD 69830 b fits the definition of a planet because it is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity overcoming rigid body forces. This is indicated by its description as a Neptune-mass or super-Earth-mass exoplanet, suggesting it has a significant mass. Additionally, HD 69830 b is in orbit around a star, specifically the star HD 69830, which is another requirement for being classified as a planet. It is also stated that it is not a star itself, nor is it a satellite of another planet. Therefore, based on the provided definition, HD 69830 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1361687", "name": "Gliese 674 b", "article": "https://en.wikipedia.org/wiki/Gliese_674_b", "description": "Gliese 674 b is an extrasolar planet approximately 15 light years away in the constellation of Ara. This planet orbits tightly around Gliese 674. It is a sub-Neptune-or-Uranus-mass planet either gaseous or rocky. It orbits as close as 0.039 AU from the star and takes only 4.6938 days to orbit. This planet has a similar eccentricity to Mercury (e=0.2). The discovery of the planet was announced on January 7, 2007 by using the HARPS spectrograph mounted on the ESO's 3.6 meter telescope at La Silla, Chile.", "actual": "positive", "rationale": "Gliese 674 b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically Gliese 674. The description does not explicitly state that Gliese 674 b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, but it is implied as it is referred to as a planet. Furthermore, it is neither a star nor a satellite of a planet. Therefore, based on the provided definition, Gliese 674 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q50667", "name": "55 Cancri d", "article": "https://en.wikipedia.org/wiki/55_Cancri_d", "description": "55 Cancri d (abbreviated 55 Cnc d), formally named Lipperhey , is an extrasolar planet in a long-period orbit around the Sun-like star 55 Cancri A. Located at a similar distance from its star as Jupiter is from the Sun, it is the fifth and outermost known planet in its planetary system. 55 Cancri d was discovered on June 13, 2002.", "actual": "positive", "rationale": "The description of 55 Cancri d indicates that it is a celestial body in orbit around a star, specifically the Sun-like star 55 Cancri A. This aligns with part (b) of the definition of a planet, which states that a planet is in orbit around a star. The description does not specify whether 55 Cancri d has a nearly round shape due to its self-gravity overcoming rigid body forces, but it is implied by the fact that it is referred to as a planet. Furthermore, the description does not indicate that 55 Cancri d is a star or a satellite of a planet, which would disqualify it from being a planet according to the definition. Therefore, based on the information provided, it can be argued that 55 Cancri d is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1204153", "name": "Kepler-8b", "article": "https://en.wikipedia.org/wiki/Kepler-8b", "description": "Kepler-8b is the fifth of the first five exoplanets discovered by NASA's Kepler spacecraft, which aims to discover planets in a region of the sky between the constellations Lyra and Cygnus that transit (cross in front of) their host stars. The planet is the hottest of the five. Kepler-8b was the only planet discovered in Kepler-8's orbit, and is larger (though more diffuse) than Jupiter. It orbits its host star every 3.5 days. The planet also demonstrates the Rossiter\u2013McLaughlin effect, where the planet's orbit affects the redshifting of the spectrum of the host star. Kepler-8b was announced to the public on January 4, 2010 at a conference in Washington, D.C. after radial velocity measurements conducted at the W.M. Keck Observatory confirmed its detection by Kepler.", "actual": "positive", "rationale": "Kepler-8b fits the definition of a planet as it is a celestial body that is in orbit around a star, specifically its host star. It is not a star itself, nor is it a satellite of another planet, as it is the only planet discovered in Kepler-8's orbit. Furthermore, it has sufficient mass for its self-gravity to overcome rigid body forces and assume a nearly round shape, as indicated by its comparison to Jupiter, a known planet. Therefore, based on the provided definition, Kepler-8b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q86686508", "name": "Kepler-1658b", "article": "https://en.wikipedia.org/wiki/Kepler-1658b", "description": "Kepler-1658b (or the Kepler object of interest, KOI-4.01) is a hot Jupiter, a type of gas giant exoplanet, that orbits an F-type star called Kepler 1658, located about 2629 light-years away from the Solar System. It is the first planet identified by the Kepler space telescope after its launch in 2009, but later ruled out as false alarm since its transit could not be confirmed. A study published in 2019 established it as a planet, describing it as \\\"the closest known planet in terms of orbital period to an evolved star.\\\" Analysis of the Transiting Exoplanet Survey Satellite (TESS) data in 2022 showed that it is gradually spiraling into its star.", "actual": "positive", "rationale": "Kepler-1658b fits the definition of a planet because it is a celestial body that has sufficient mass to assume a hydrostatic equilibrium shape, as indicated by its classification as a gas giant exoplanet. Additionally, it is in orbit around a star, specifically an F-type star called Kepler 1658. It is not a star itself, nor is it a satellite of another planet. Therefore, based on the provided definition, Kepler-1658b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q222246", "name": "2MASS J03552337+1133437", "article": "https://en.wikipedia.org/wiki/2MASS_J03552337%2B1133437", "description": "2MASS J03552337+1133437 (2MASS J0355+11) is a nearby brown dwarf of spectral type L5\u03b3, located in constellation Taurus at approximately 29.8 light-years from Earth.", "actual": "positive", "rationale": "The given definition cannot support the assertion that 2MASS J03552337+1133437 is a planet. The description of 2MASS J03552337+1133437 identifies it as a brown dwarf, not a planet. Furthermore, there is no information provided that it is in orbit around a star, which is a necessary condition for being classified as a planet according to the given definition. Therefore, based on the provided information, we cannot argue that 2MASS J03552337+1133437 is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q5281813", "name": "Discoverer 29", "article": "https://en.wikipedia.org/wiki/Discoverer_29", "description": "Discoverer 29, also known as Corona 9023, was an American optical reconnaissance satellite which was launched in 1961. It was the first KH-3 Corona''' satellite, which was based on an Agena-B rocket.The launch of Discoverer 29 occurred at 20:00 UTC on 30 August 1961. A Thor DM-21 Agena-B rocket was used, flying from Launch Complex 75-3-4 at the Vandenberg Air Force Base. Upon successfully reaching orbit, it was assigned the Harvard designation 1961 Psi 1.\nDiscoverer 29 was operated in a low Earth orbit, with a perigee of 138 kilometres (86 mi), an apogee of 511 kilometres (318 mi), 82 degrees of inclination, and a period of 91 minutes. The satellite had a mass of 1,150 kilograms (2,540 lb), and was equipped with a panoramic camera with a focal length of 61 centimetres (24 in), which had a maximum resolution of 7.6 metres (25 ft). Images were recorded onto 70-millimeter (2.8 in) film, and returned in a Satellite Recovery Vehicle two days after launch, but all of the images returned were found to be out of focus. The Satellite Recovery Vehicle used by Discoverer 29 was SRV-554. Once its images had been returned, Discoverer 29 remained in orbit until it decayed on 9 September 1961.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Discoverer 29 is a planet. The definition states that a planet is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and is in orbit around a star, and is neither a star nor a satellite of a planet. \n\nDiscoverer 29, however, is described as an American optical reconnaissance satellite. It was launched into orbit around the Earth, making it a satellite, not a planet. It does not have its own orbit around a star, but rather orbits a planet (Earth). Furthermore, there is no information suggesting that Discoverer 29 has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Therefore, based on the provided definition and information, Discoverer 29 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q54347", "name": "RazakSAT", "article": "https://en.wikipedia.org/wiki/RazakSAT", "description": "RazakSAT is a Malaysian Earth observation satellite carrying a high-resolution camera. It was launched into low Earth orbit on 14 July 2009. It was placed in a near-equatorial orbit that presents many imaging opportunities for the equatorial region. It weighs over three times as much as TiungSAT-1 and carries a high-resolution Earth observation camera. Developed in conjunction with the Satrec Initiative, the satellite's low inclination (9 degrees) brought it over Malaysia a dozen or more times per day. This was intended to provide greatly increased coverage of Malaysia compared to most other Earth observation satellites. An audit report released in October 2011 revealed that the satellite had failed after one year of operation.RazakSAT was the only operational satellite to be put into orbit by SpaceX's Falcon 1.", "actual": "negative", "rationale": "The assertion that RazakSAT is a planet cannot be supported based on the provided definition and information. According to the definition, a planet is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and is in orbit around a star, and is neither a star nor a satellite of a planet. However, RazakSAT is described as an Earth observation satellite, which means it is a satellite of a planet (Earth), thus disqualifying it from being classified as a planet. Furthermore, there is no information suggesting that RazakSAT has sufficient mass for its self-gravity to overcome rigid body forces to assume a nearly round shape. Therefore, based on the provided definition and information, RazakSAT cannot be considered a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1166037", "name": "Explorer 15", "article": "https://en.wikipedia.org/wiki/Explorer_15", "description": "Explorer 15, also called EPE-C or Energetic Particles Explorer-C, was a NASA satellite launched as part of the Explorer program. Explorer 15 was launched on 27 October 1962, at Cape Canaveral Air Force Station, Florida, United States, with a Thor-Delta A .", "actual": "negative", "rationale": "There is no valid argument that can be made based on the provided definition and information that Explorer 15 is a planet. The definition of a planet states that it must be a celestial body that has sufficient mass to overcome rigid body forces and assume a nearly round shape, and it must be in orbit around a star. It also cannot be a star or a satellite of a planet. Explorer 15, however, is described as a satellite launched by NASA, which directly contradicts the definition of a planet. Therefore, Explorer 15 cannot be considered a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q60760723", "name": "JY1-SAT", "article": "https://en.wikipedia.org/wiki/JY1-SAT", "description": "JY1-SAT is a cubesat that is Jordan's first satellite. It was launched aboard SpaceX's Falcon 9 from the Vandenberg Air Force Base in the United States on 3 December 2018. It is named in tribute of the late King Hussein who was an amateur ham radio operator; his callsign was \\\"JY1\\\". The project was built by Jordanian students from various universities, and was funded by Jordan's Crown Prince Foundation.", "actual": "negative", "rationale": "The assertion that JY1-SAT is a planet cannot be supported by the given definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a hydrostatic equilibrium shape and is in orbit around a star. It is also specified that it is neither a star nor a satellite of a planet. However, JY1-SAT is described as a cubesat, which is a type of miniaturized satellite for space research, and it is not mentioned to have sufficient mass to assume a hydrostatic equilibrium shape. Furthermore, it is stated that JY1-SAT is not in orbit around a star, but was launched from Earth, implying it is a satellite of a planet. Therefore, based on the provided definition and information, JY1-SAT cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q69165", "name": "ChinaSat 12", "article": "https://en.wikipedia.org/wiki/ChinaSat_12", "description": "The ChinaSat 12 (Chinese: \u4e2d\u661f12\u53f7; pinyin: Zh\u014dngx\u012bng 12) communications satellite is wholly owned by China Satellite Communications, with part of its communications payload leased or rented by SupremeSAT, a Sri Lankan company, to be marketed to potential users as SupremeSAT-I. Once operational, it will provide communications services for the China, Sri Lanka, East Asia, South Asia, Middle East, Africa, Australia, and China sea area, the Indian Ocean region.ChinaSat 12 was also known as Apstar 7B (as a backup of Apstar 7), but acquired by China Satellite Communications from its subsidiary APT Satellite Holdings in 2010. However, APT Satellite Holdings was contracted by its parent company as the operator of ChinaSat 12.", "actual": "negative", "rationale": "There is no valid argument to assert that ChinaSat 12 is a planet based on the provided definition. The definition clearly states that a planet is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and is in orbit around a star, and is neither a star nor a satellite of a planet. ChinaSat 12, however, is a communications satellite, not a celestial body with its own gravity. It is also a satellite of a planet (Earth), which directly contradicts the definition of a planet. Therefore, based on the provided definition, ChinaSat 12 cannot be considered a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q211655", "name": "2008 TC3", "article": "https://en.wikipedia.org/wiki/2008_TC3", "description": "2008 TC3 (Catalina Sky Survey temporary designation 8TA9D69) was an 80-tonne (80-long-ton; 90-short-ton), 4.1-meter (13 ft) diameter asteroid that entered Earth's atmosphere on October 7, 2008. It exploded at an estimated 37 kilometers (23 mi) above the Nubian Desert in Sudan. Some 600 meteorites, weighing a total of 10.5 kilograms (23.1 lb), were recovered; many of these belonged to a rare type known as ureilites, which contain, among other minerals, nanodiamonds.It was the first time that an asteroid impact had been predicted before its entry into the atmosphere as a meteor.", "actual": "negative", "rationale": "Based on the provided definition and information, it cannot be argued that 2008 TC3 is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. 2008 TC3 was an asteroid that entered Earth's atmosphere and exploded above the Nubian Desert in Sudan. It was not in orbit around a star, nor did it have a nearly round shape due to self-gravity overcoming rigid body forces. Therefore, 2008 TC3 does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4537552", "name": "Yamal 201", "article": "https://en.wikipedia.org/wiki/Yamal_201", "description": "Yamal-201 (Russian: \u042f\u043c\u0430\u043b-201) was a geostationary communications satellite operated by Gazprom Space Systems and built by RSC Energia. It was, along with Yamal-202 the second dual launch of the Yamal programme and the second iteration of the USP Bus. It was a 1,360 kg (3,000 lb) satellite with 4,080 watts of power (3.4 kW at end of life) on an unpressurized bus. It had eight SPT-70 electric thrusters by OKB Fakel for station keeping. Its payload was 9 C-band and 6 Ku-band transponders supplied by Space Systems/Loral.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that Yamal 201 is a planet. The definition specifies that a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, orbits a star, and is neither a star nor a satellite of a planet. Yamal 201, however, is described as a geostationary communications satellite. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q137248", "name": "1240 Centenaria", "article": "https://en.wikipedia.org/wiki/1240_Centenaria", "description": "1240 Centenaria, provisional designation 1932 CD, is a background asteroid from the outer regions of the asteroid belt, approximately 60 kilometers (37 miles) in diameter. It was discovered on 5 February 1932, by astronomer Richard Schorr at the Bergedorf Observatory in Hamburg, Germany. The assumed C-type asteroid has a rotation period of 11.3 hours. It was named for the 100th anniversary of the discovering observatory.", "actual": "negative", "rationale": "The assertion that 1240 Centenaria is a planet cannot be supported based on the provided definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape and is in orbit around a star. While 1240 Centenaria is indeed a celestial body in orbit around a star, there is no information provided about its shape or its mass being sufficient to overcome rigid body forces for it to assume a hydrostatic equilibrium. Furthermore, it is specifically identified as an asteroid, not a planet. Therefore, based on the provided definition and information, there is no valid argument to classify 1240 Centenaria as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4553351", "name": "178P/Hug\u2013Bell", "article": "https://en.wikipedia.org/wiki/178P/Hug%E2%80%93Bell", "description": "178P/Hug\u2013Bell is a periodic comet in the Solar System. It was discovered by Northeast Kansas Amateur Astronomers' League members Gary Hug and Graham Bell and is thought to be the first periodic comet to be discovered by amateurs. It was declared a comet less than two days after its initial discovery, after having its course confirmed on previous images.Hug-Bell's orbital period is about seven years; its orbit is eccentric, though less so than many comets. Hug-Bell's orbit lies entirely outside the orbit of Mars, but at its aphelion overlaps in solar distance with the orbit of Jupiter. Because it never comes closer to the Sun than about 2 AU, it is never expected to be a very bright comet, with a typical perihelion magnitude of 18-19.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 178P/Hug\u2013Bell is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. While 178P/Hug\u2013Bell does orbit a star (the Sun), it is identified as a comet, not a planet. The definition also requires a planet to have sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape. There is no information provided about the shape or mass of 178P/Hug\u2013Bell. Therefore, based on the provided definition and information, there is no basis to assert that 178P/Hug\u2013Bell is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q956514", "name": "3714 Kenrussell", "article": "https://en.wikipedia.org/wiki/3714_Kenrussell", "description": "3714 Kenrussell, provisional designation 1983 TT1, is a Eunomian asteroid from the central regions of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. It was discovered on 12 October 1983, by American astronomer Edward Bowell at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. It was named for Australian astronomer Kenneth S. Russell. The presumably stony asteroid has a rotation period of 5.25 hours.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 3714 Kenrussell is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. While 3714 Kenrussell is a celestial body and is not a star or a satellite of a planet, it is not specifically stated that it is in orbit around a star. Furthermore, it is described as an asteroid, not a planet. Therefore, using only the information provided in the definition, it cannot be argued that 3714 Kenrussell is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q116674440", "name": "S/2021 J 2", "article": "https://en.wikipedia.org/wiki/S/2021_J_2", "description": "S/2021 J 2 is a small outer natural satellite of Jupiter discovered by Scott S. Sheppard on 12 August 2021, using the 6.5-meter Magellan-Baade Telescope at Las Campanas Observatory, Chile. It was announced by the Minor Planet Center on 19 January 2023, after observations were collected over a long enough time span to confirm the satellite's orbit.S/2021 J 2 is part of the Ananke group, a cluster of retrograde irregular moons of Jupiter that follow similar orbits to Ananke at semi-major axes between 19\u201322 million km (12\u201314 million mi), orbital eccentricities between 0.1\u20130.4, and inclinations between 139\u2013155\u00b0. It has a diameter of about 1 km (0.62 mi) for an absolute magnitude of 17.3, making it one of Jupiter's smallest known moons.", "actual": "negative", "rationale": "The assertion that S/2021 J 2 is a planet cannot be supported based on the provided definition of a planet. According to the definition, a planet is a celestial body that orbits a star and is not a satellite of a planet. However, S/2021 J 2 is described as a natural satellite of Jupiter, which means it orbits Jupiter, not a star. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q28845773", "name": "OV1-4", "article": "https://en.wikipedia.org/wiki/OV1-4", "description": "Orbiting Vehicle 1-4 (also known as OV1-4), launched 30 Mar 1966, was the fourth, and second successful, satellite in the OV1 series of the United States Air Force's Orbiting Vehicle program. OV1-4 was a long-term bioscience and materials science satellite, designed to return data relevant to long-term human presence in space. Its launch marked the first time two satellites (the other being OV1-5) were placed into orbit side by side with each other.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that OV1-4 is a planet. The definition states that a planet is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and is in orbit around a star, and is neither a star nor a satellite of a planet. OV1-4, however, is described as a satellite, which directly contradicts the definition of a planet. Therefore, using the provided definition and information, OV1-4 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q22084830", "name": "Near-Earth Asteroid Scout", "article": "https://en.wikipedia.org/wiki/Near-Earth_Asteroid_Scout", "description": "The Near-Earth Asteroid Scout (NEA Scout) was a mission by NASA to develop a controllable low-cost CubeSat solar sail spacecraft capable of encountering near-Earth asteroids (NEA). NEA Scout was one of ten CubeSats launched into a heliocentric orbit on Artemis 1, the maiden flight of the Space Launch System, on 16 November 2022.The target for the mission was asteroid 2020 GE, but this could have changed based on launch date or other factors. After deployment, NEA Scout was to perform a series of lunar flybys to achieve optimum departure trajectory before beginning its two-year-long cruise.\nNo contact was ever made, and the mission was lost.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that the Near-Earth Asteroid Scout is a planet. The definition states that a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it orbits around a star. The Near-Earth Asteroid Scout, however, is a spacecraft developed by NASA, not a celestial body. It does not have its own gravity to form a nearly round shape, and while it was launched into a heliocentric orbit, it is not naturally in orbit around a star. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q114646", "name": "696 Leonora", "article": "https://en.wikipedia.org/wiki/696_Leonora", "description": "696 Leonora is a Meliboean asteroid orbiting the Sun in the asteroid belt. It was discovered 10 January 1910 by American astronomer Joel Hastings Metcalf, at Taunton, Massachusetts. It was named by Arthur Snow of the United States Naval Observatory, who computed the orbit for the planet, after his wife, Mary Leonora Snow.", "actual": "negative", "rationale": "The information provided does not support the assertion that 696 Leonora is a planet. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape and is in orbit around a star, but is not a star itself or a satellite of a planet. While 696 Leonora is a celestial body in orbit around the Sun, it is not specified whether it has sufficient mass to assume a nearly round shape, nor is it specified that it is not a satellite of a planet. Furthermore, it is identified as an asteroid, which is a different type of celestial body than a planet. Therefore, based on the provided definition and information, there is no valid argument to classify 696 Leonora as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1227405", "name": "T11 (satellite)", "article": "https://en.wikipedia.org/wiki/T11_(satellite)", "description": "T11, formerly known as DirecTV-11, is a Boeing model 702 satellite built by the Boeing Satellite Development Center. Its current name was adopted in 2017.", "actual": "negative", "rationale": "The rationale cannot be provided as per the given definition and information. T11 is described as a satellite, which is explicitly stated in the definition to not be a planet. Therefore, based on the provided information, T11 cannot be considered a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q16061296", "name": "Eutelsat I F-2", "article": "https://en.wikipedia.org/wiki/Eutelsat_I_F-2", "description": "Eutelsat I F-2, also known as European Communications Satellite 2 (ECS-2) is a decommissioned communications satellite operated by the European Telecommunications Satellite Organisation (Eutelsat). Launched in 1984, it was operated in geostationary orbit at a longitude of 7\u00b0 East, before moving to several other locations later in its operational life, before it was finally decommissioned in 1993. It was the second of five satellites launched to form the first-generation Eutelsat constellation.", "actual": "negative", "rationale": "There is no valid argument to assert that Eutelsat I F-2 is a planet based on the provided definition. The Eutelsat I F-2 is a man-made satellite, not a celestial body. It does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. It is in orbit around a star (the Sun), but it is a satellite of a planet (Earth), which disqualifies it from being a planet according to the given definition.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q539769", "name": "SCORE (satellite)", "article": "https://en.wikipedia.org/wiki/SCORE_(satellite)", "description": "SCORE (Signal Communications by Orbiting Relay Equipment) was the world's first purpose-built communications satellite. Launched aboard an American Atlas rocket on December 18, 1958, SCORE provided the second test of a communications relay system in space (the first having been provided by the USAF/NASA's Pioneer 1), the first broadcast of a human voice from space, and the first successful use of the Atlas as a launch vehicle. It captured world attention by broadcasting a Christmas message via shortwave radio from U.S. President Dwight D. Eisenhower through an on-board tape recorder. The satellite was popularly dubbed \\\"The Talking Atlas\\\". SCORE, as a geopolitical strategy, placed the United States at an even technological par with the Soviet Union as a highly functional response to the Sputnik 1 and Sputnik 2 satellites.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that SCORE (satellite) is a planet. The definition of a planet states that it must be a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and is in orbit around a star, and is neither a star nor a satellite of a planet. SCORE, however, is explicitly described as a satellite, which disqualifies it from being considered a planet according to the given definition.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q6433287", "name": "Kosmos 2478", "article": "https://en.wikipedia.org/wiki/Kosmos_2478", "description": "Kosmos 2478 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 2478 meaning Cosmos 2478) is a  Russian military satellite launched in 2011 as part of the GLONASS satellite navigation system.\nThis satellite is a GLONASS-M satellite, also known as Uragan-M, and is numbered Uragan-M No. 746.Kosmos 2478 was launched from Site 43/4  at Plesetsk Cosmodrome in northern Russia. A Soyuz-2-1b carrier rocket with a Fregat upper stage was used to perform the launch which took place at 08:26 UTC on 28 November 2011. The launch successfully placed the satellite into Medium Earth orbit. It subsequently received its Kosmos designation, and the international designator 2011\u2013071. The United States Space Command assigned it the Satellite Catalog Number 37938.It is in the third orbital plane used by GLONASS, in orbital slot 17.It started operations on 23 December 2011.", "actual": "negative", "rationale": "There is no valid argument to assert that Kosmos 2478 is a planet based on the provided definition. Kosmos 2478 is described as a man-made satellite, not a celestial body. It does not have its own self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. It is also not in orbit around a star, but rather it is in orbit around the Earth. Therefore, according to the given definition, Kosmos 2478 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2521638", "name": "ViaSat-1", "article": "https://en.wikipedia.org/wiki/ViaSat-1", "description": "ViaSat-1 is a high throughput communications satellite owned by  Viasat Inc. and Telesat Canada. Launched October 19, 2011 aboard a Proton rocket, it held the Guinness record for the world's highest capacity communications satellite with a total capacity in excess of 140 Gbit/s, more than all the satellites covering North America combined, at the time of its launch.ViaSat-1 is capable of two-way communications with small dish antennas at higher speeds and a lower cost-per-bit than any satellite before.The satellite is positioned at 115.1 degrees West longitude geostationary orbit point, with 72 Ka-band spot beams; 63 over the U.S. (Eastern and Western states, Alaska and Hawaii), and nine over Canada.\nThe Canadian beams are owned by satellite operator Telesat and are used for the Xplornet broadband service to consumers in rural Canada. The US beams provide fast Internet access called Exede, Viasat's satellite Internet service.ViaSat-1 is part of a new satellite system architecture created by Viasat Inc. The objective is to create a better satellite broadband user experience, making satellite competitive with DSL and wireless broadband alternatives for the first time.", "actual": "negative", "rationale": "There is no valid argument to assert that ViaSat-1 is a planet based on the provided definition. ViaSat-1 is described as a communications satellite, not a celestial body with sufficient mass to assume a hydrostatic equilibrium shape. It is also not in orbit around a star, but rather in geostationary orbit around the Earth. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q7865651", "name": "USA-132", "article": "https://en.wikipedia.org/wiki/USA-132", "description": "USA-132, also known as GPS IIR-2 and GPS SVN-43, is an American navigation satellite which forms part of the Global Positioning System. It was the second Block IIR GPS satellite to be launched, out of thirteen in the original configuration, and twenty one overall. GPS IIR-1 failed to achieve orbit, so USA-132 was the first successful Block IIR satellite. It was built by Lockheed Martin, using the AS-4000 satellite bus.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that USA-132 is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. USA-132, however, is described as a navigation satellite, which means it is a satellite of a planet (Earth, in this case). Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4649953", "name": "AAUSat-3", "article": "https://en.wikipedia.org/wiki/AAUSat-3", "description": "AAUSat-3,  (Aalborg University CubeSat-3), is the third CubeSat built and operated by students from the Aalborg University in Denmark. It was launched on 25 February 2013 from the Satish Dhawan Space Centre in India on a Polar Satellite Launch Vehicle (PSLV) launch vehicle (PSLV-C20). AAUSat-3 carries two Automatic Identification System (AIS-1 and AIS-2) receivers as the main payload.", "actual": "negative", "rationale": "The assertion that AAUSat-3 is a planet cannot be supported by the given definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity and is in orbit around a star. It is neither a star nor a satellite of a planet. However, AAUSat-3 is a CubeSat, a type of miniaturized satellite for space research, built and operated by students from the Aalborg University in Denmark. It does not meet the criteria of having sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, and it is a satellite, which disqualifies it from being a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1612589", "name": "Communications Technology Satellite", "article": "https://en.wikipedia.org/wiki/Communications_Technology_Satellite", "description": "The Communications Technology Satellite (CTS), known as Hermes, was an experimental high-power direct broadcast communications satellite. It was a joint effort of Canadian Department of Communications, who designed and built the satellite, NASA who tested, launched and operated the satellite, and European Space Agency (ESA) who provided the 1200 watts solar panels and other devices. The three agencies shared the satellite and the data from the experiments.\nAlthough the launch of the ATS-6 spacecraft in 1974 marked the end of NASA's program of experimental communications satellites. NASA participated in a Canadian satellite venture known initially as \\\"Cooperative Applications Satellite-C\\\" and renamed Hermes. This joint effort involved NASA and the Canadian Department of Communications. NASA's Lewis Research Center provided the satellite's high-power communications payload. Canada designed and built the spacecraft; NASA tested, launched, and operated it. Also, the European Space Agency provided one of the low-power traveling-wave tubes and other equipment. Hermes was launched 17 January 1976 and operated until October 1979.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that the Communications Technology Satellite is a planet. The definition of a planet states that it must be a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and is in orbit around a star, and is neither a star nor a satellite of a planet. The Communications Technology Satellite, however, is a man-made object that was designed, built, and launched by various space agencies. It does not have its own gravity, nor does it assume a nearly round shape due to self-gravity. Furthermore, it is a satellite, which is explicitly excluded from the definition of a planet. Therefore, the Communications Technology Satellite cannot be considered a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153548", "name": "432 Pythia", "article": "https://en.wikipedia.org/wiki/432_Pythia", "description": "Pythia (minor planet designation: 432 Pythia) is a typical Main belt asteroid.\nIt was discovered by Auguste Charlois on 18 December 1897 in Nice.", "actual": "negative", "rationale": "The definition provided does not allow for the assertion that 432 Pythia is a planet. According to the definition, a planet is a celestial body that is in orbit around a star and is not a star itself or a satellite of a planet. While 432 Pythia is a celestial body in orbit around a star, it is described as a \"Main belt asteroid\", not a planet. The definition does not include asteroids in its categorization of planets. Therefore, based solely on the provided definition and description, there is no valid argument to classify 432 Pythia as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4181082", "name": "Great Comet of 1819", "article": "https://en.wikipedia.org/wiki/Great_Comet_of_1819", "description": "The Great Comet of 1819, officially designated as C/1819 N1, also known as Comet Tralles, was an exceptionally bright and easily visible comet, approaching an apparent magnitude of 1\u20132, discovered July 1, 1819 by the German astronomer Johann Georg Tralles in Berlin. It was the first comet analyzed using polarimetry, by French mathematician Fran\u00e7ois Arago.", "actual": "negative", "rationale": "The assertion that the Great Comet of 1819 is a planet cannot be supported by the given definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, orbits a star, and is not a star itself or a satellite of a planet. The Great Comet of 1819, as described, is a comet, not a planet. It was exceptionally bright and visible, discovered by an astronomer, and analyzed using polarimetry. None of these characteristics align with the definition of a planet. Therefore, based on the provided definition and information, the Great Comet of 1819 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q376628", "name": "CHEOPS", "article": "https://en.wikipedia.org/wiki/CHEOPS", "description": "CHEOPS (CHaracterising ExOPlanets Satellite) is a European space telescope. Its objective is to determine the size of known extrasolar planets, which will allow the estimation of their mass, density, composition and their formation. Launched on 18 December 2019, it is the first Small-class mission in ESA's Cosmic Vision science programme.The small satellite features an optical Ritchey-Chr\u00e9tien telescope with an aperture of 30 cm, mounted on a standard small satellite platform. It was placed into a Sun-synchronous orbit of about 700 km altitude.", "actual": "negative", "rationale": "The assertion that CHEOPS is a planet cannot be supported based on the provided definition and description. According to the definition, a planet is a celestial body that has sufficient mass to maintain a nearly round shape due to its self-gravity, orbits a star, and is not a star itself or a satellite of a planet. However, the description of CHEOPS indicates that it is a space telescope launched by the European Space Agency, not a celestial body. It does orbit the Earth, but it does so because it was placed into a Sun-synchronous orbit, not due to its own gravitational pull. Therefore, based on the provided information, CHEOPS does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q17285875", "name": "Hodoyoshi 3", "article": "https://en.wikipedia.org/wiki/Hodoyoshi_3", "description": "Hodoyoshi-3 is a Japanese micro-satellite launched in 2014. The satellite is built in 0.5x0.5x0.65m box-shape bus, optimized for piggy-back launch.\nAll instruments are powered by solar cells mounted on the spacecraft body and two stub wings, with estimated electrical power of 50W. For orbit-keeping, a hydrogen peroxide thruster is used. The satellite was developed under the Funding Program for World-Leading Innovation R&D on Science and Technology.", "actual": "negative", "rationale": "The assertion that Hodoyoshi 3 is a planet cannot be supported based on the provided definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity and is in orbit around a star. It is also specified that a planet is neither a star nor a satellite of a planet. \n\nHowever, Hodoyoshi 3 is described as a micro-satellite, which directly contradicts the definition of a planet. It is not mentioned whether Hodoyoshi 3 has sufficient mass to assume a nearly round shape due to its self-gravity, but it is built in a box-shape, which suggests it does not naturally assume a round shape. Therefore, based on the provided information and definition, Hodoyoshi 3 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q55624488", "name": "NOAA-14", "article": "https://en.wikipedia.org/wiki/NOAA-14", "description": "NOAA-14, also known as NOAA-J before launch, was an American weather satellite operated by the National Oceanic and Atmospheric Administration (NOAA). NOAA-14 continued the third-generation operational, Polar Orbiting Environmental Satellite (POES) series operated by the National Environmental Satellite Service (NESS) of the National Oceanic and Atmospheric Administration (NOAA). NOAA-14 continued the series of Advanced TIROS-N (ATN) spacecraft begun with the launch of NOAA-8 (NOAA-E) in 1983.", "actual": "negative", "rationale": "Based on the provided definition and information, it is not possible to argue that NOAA-14 is a planet. The definition of a planet states that it is a celestial body that has sufficient mass to assume a hydrostatic equilibrium shape, is in orbit around a star, and is neither a star nor a satellite of a planet. NOAA-14, however, is described as a weather satellite operated by NOAA. Therefore, it is a satellite, not a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q18239", "name": "Loge (moon)", "article": "https://en.wikipedia.org/wiki/Loge_(moon)", "description": "Loge or Saturn XLVI is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on 26 June 2006, from observations taken between January and April 2006.\nLoge is about 6 kilometres in diameter, and orbits Saturn at an average distance of 23,142,000 km in 1314.364 days, at an inclination of 166.5\u00b0 to the ecliptic (165.3\u00b0 to Saturn's equator), in a retrograde direction and with an eccentricity of 0.1390. It has a tentative rotation period of about 6.9\u00b10.1 hours, but this is highly uncertain as the light curve is the shallowest among all the irregular moons studied by Cassini\u2013Huygens (amplitude about 0.07 magnitudes).It was named in April 2007, after Logi, a fire giant from Norse mythology.", "actual": "negative", "rationale": "The assertion that Loge (moon) is a planet cannot be supported by the given definition and information. According to the definition, a planet is a celestial body that orbits a star and is not a satellite of a planet. However, the description of Loge clearly states that it is a natural satellite of Saturn, which contradicts the definition of a planet. Therefore, based on the provided definition and information, Loge cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q63853", "name": "1509 Esclangona", "article": "https://en.wikipedia.org/wiki/1509_Esclangona", "description": "1509 Esclangona, provisional designation 1938 YG, is a rare-type Hungaria asteroid and binary system from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It is named after French astronomer Ernest Esclangon.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 1509 Esclangona is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. While 1509 Esclangona is a celestial body and is not a star or a satellite of a planet, it is not in orbit around a star. Instead, it is located in the inner regions of the asteroid belt. Therefore, it does not meet all the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153870", "name": "4383 Suruga", "article": "https://en.wikipedia.org/wiki/4383_Suruga", "description": "4383 Suruga, provisional designation 1989 XP, is a Vestian asteroid and binary system from the inner regions of the asteroid belt, approximately 6.5 kilometers in diameter. It was discovered on 1 December 1989, by Japanese astronomer Yoshiaki Oshima at Gekko Observatory, Japan. The asteroid was named after the former Japanese Suruga Province. Its synchronous minor-planet moon, S/2013 (4383) 1, measures approximately 1.33 kilometers and has a period of 16.386 hours.", "actual": "negative", "rationale": "The assertion that 4383 Suruga is a planet cannot be supported based on the provided definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape and is in orbit around a star. While 4383 Suruga is a celestial body and likely orbits a star, there is no information provided about its shape or its mass, which are crucial to determining whether it meets the criteria for being a planet. Furthermore, it is described as an asteroid, which is typically classified differently from a planet. Therefore, based on the given information and definition, we cannot argue that 4383 Suruga is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q211473", "name": "(613100) 2005 TN74", "article": "https://en.wikipedia.org/wiki/(613100)_2005_TN74", "description": "(613100) 2005 TN74 (also written 2005 TN74) is a trans-Neptunian object (TNO) in a 3:5 resonance with Neptune. It was discovered by Scott S. Sheppard and Chadwick A. Trujillo in 2005.\nIt was initially suspected of being a Neptune trojan since the first observations gave it a semi-major axis of 30 AU and an orbital eccentricity of 0.16, but further observations showed it to have a semi-major axis of 42.7 AU, a perihelion of 32.1 AU, and an aphelion of 53.4 AU.With an absolute magnitude of 7.2, it has an expected diameter in the range of 85 to 240 km.It has been observed 19 times over four oppositions.", "actual": "negative", "rationale": "The information provided about (613100) 2005 TN74 indicates that it is a celestial body in orbit around a star (the Sun, in this case), which aligns with part (b) of the definition of a planet. However, the information does not provide explicit evidence that (613100) 2005 TN74 has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, which is part (a) of the definition. Therefore, based solely on the information provided, a definitive argument cannot be made that (613100) 2005 TN74 is a planet. More information about its mass and shape would be needed to make this determination.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q136761", "name": "1173 Anchises", "article": "https://en.wikipedia.org/wiki/1173_Anchises", "description": "1173 Anchises  is an unusually elongated Jupiter Trojan from the Trojan camp, approximately 124 kilometers (77 miles) in diameter. It was discovered on 17 October 1930, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany, and was the 9th such body to be discovered.:\u200a2\u200a The primitive P-type asteroid belongs to the largest Jupiter trojans, has an unusually smooth surface texture, the lowest spectral slope of all members of the Trojan camp, and a rotation period of 11.6 hours. It was named after Anchises from Greek mythology.", "actual": "negative", "rationale": "The definition of a planet states that it must be a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it must be in orbit around a star. It also cannot be a star itself or a satellite of a planet. The description of 1173 Anchises indicates that it is a celestial body in orbit around a star (as it is a Jupiter Trojan). However, the description does not provide enough information to determine if 1173 Anchises has sufficient mass to assume a nearly round shape due to its self-gravity, or if it is not a satellite of a planet. Therefore, based solely on the provided definition and description, it cannot be definitively argued that 1173 Anchises is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4044978", "name": "NOAA-16", "article": "https://en.wikipedia.org/wiki/NOAA-16", "description": "NOAA-16, also known as NOAA-L before launch, was an operational, polar orbiting, weather satellite series (NOAA K-N) operated by the National Environmental Satellite Service (NESS) of the National Oceanic and Atmospheric Administration (NOAA). NOAA-16 continued the series of Advanced TIROS-N (ATN) spacecraft that began with the launch of NOAA-8 (NOAA-E) in 1983; but it had additional new and improved instrumentation over the NOAA A-K series and a new launch vehicle (Titan 23G). It was launched on 21 September 2000 and, following an unknown anomaly, it was decommissioned on 9 June 2014. In November of 2015 it broke up in orbit, creating more than 200 pieces of debris.", "actual": "negative", "rationale": "The assertion that NOAA-16 is a planet cannot be supported by the provided definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity and orbits around a star. It is also specified that a planet is neither a star nor a satellite of a planet. \n\nHowever, the description of NOAA-16 indicates that it is a weather satellite operated by the National Environmental Satellite Service (NESS) of the National Oceanic and Atmospheric Administration (NOAA). This means that NOAA-16 is a man-made object that was launched into space, not a natural celestial body. Furthermore, it is a satellite, which the definition explicitly excludes from being a planet. Therefore, based on the provided definition and information, NOAA-16 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q157514", "name": "867 Kovacia", "article": "https://en.wikipedia.org/wiki/867_Kovacia", "description": "867 Kovacia (prov. designation: A917 DH or 1917 BS) is an elongated, dark asteroid and member of the Hygiea family from the outer regions of the asteroid belt. It was discovered on 25 February 1917, by astronomer Johann Palisa at the Vienna Observatory in Austria. The carbonaceous C/B-type asteroid has a rotation period of 8.7 hours and measures approximately 24 kilometers (15 miles) in diameter. It was named after Austrian physician Friedrich Kovacs (1861\u20131931).", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 867 Kovacia is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. While 867 Kovacia is in orbit around a star, it is described as an asteroid, not a planet. Furthermore, there is no information provided that suggests 867 Kovacia has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, which is another requirement for being classified as a planet. Therefore, based on the provided definition and information, 867 Kovacia cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2402418", "name": "Galaxy 25", "article": "https://en.wikipedia.org/wiki/Galaxy_25", "description": "Galaxy 25 (G-25) launched in 1997, the launch was contracted by International Launch Services (ILS), (formerly known as Intelsat Americas 5 (IA-5) until 15 February 2007 when it was renamed as result of the merger between owner Intelsat and PanAmSat or Telstar 5) is a medium-powered communications satellite formerly in a geostationary orbit at 97\u00b0 West, above a point in the Pacific Ocean several hundred miles west of the Galapagos Islands. It was manufactured by Space Systems/Loral, part of its LS-1300 satellite bus, and is currently owned and operated by Intelsat. The satellite's main C-band transponder cluster covers the United States, Canada, and Mexico; its main Ku-band transponder cluster covers the United States, Mexico, and the Northern Caribbean Sea. An additional C-band and a Ku-band transponder pair targets Hawaii.\nGalaxy 25 has a projected life of 12 years. It was replaced by Galaxy 19 (formerly IA-9) in late 2008. When it was last in service at 97.1\u00b0 West, Galaxy 25 transmitted both Free-to-air (FTA) direct-to-home (DTH) broadcasting and encrypted subscription channels / services. The replacement satellite, Galaxy 19 was successfully launched on September 24, 2008. Galaxy 25 has been moved to a different orbital position at 93.1\u00b0 West where it is currently broadcasting several services on its Ku band transponders.", "actual": "negative", "rationale": "Based on the provided definition and information, there is no valid argument to assert that Galaxy 25 is a planet. The definition of a planet states that it is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it orbits around a star. It is neither a star nor a satellite of a planet. \n\nHowever, the description of Galaxy 25 indicates that it is a medium-powered communications satellite, not a celestial body with its own self-gravity. It was manufactured and launched into a geostationary orbit, and it does not orbit a star. Instead, it was placed in specific orbital positions to facilitate communication services. Therefore, based on the provided definition and information, Galaxy 25 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1119672", "name": "Kosmos 52", "article": "https://en.wikipedia.org/wiki/Kosmos_52", "description": "Kosmos 52 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 52 meaning Cosmos 52) or Zenit-2 No.26 was a Soviet, first generation, low resolution, optical film-return reconnaissance satellite launched in 1965. A Zenit-2 spacecraft, Kosmos 52 was the twenty-fifth of eighty-one such satellites to be launched and had a mass of 4,730 kilograms (10,430 lb).\nKosmos 52 was launched by a Vostok-2 rocket, serial number R15002-03, flying from Site 31/6 at the Baikonur Cosmodrome. The launch took place at 09:36 GMT on 11 January 1965, with the spacecraft receiving its Kosmos designation - along with the International Designator 1965-001A and the Satellite Catalog Number 00968 - upon its successful insertion into orbit. It was the first satellite to be launched in the year 1965.\nKosmos 52 was operated in a low Earth orbit. On 11 January 1965 it had a perigee of 203 kilometres (126 mi), an apogee of 298 kilometres (185 mi), an inclination of 65.0\u00b0 and an orbital period of 89.5 minutes. On 19 January 1965, eight days after launch, Kosmos 52 was deorbited so that its return capsule could be recovered by Soviet forces and its photos developed and analysed.", "actual": "negative", "rationale": "Based on the provided definition and information, it is not possible to argue that Kosmos 52 is a planet. The definition of a planet states that it is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it orbits around a star. It is neither a star nor a satellite of a planet. However, Kosmos 52 is described as a Soviet reconnaissance satellite that was launched into a low Earth orbit. It does not meet the criteria of having sufficient mass to assume a nearly round shape due to its self-gravity, and it is a satellite of a planet (Earth), not in orbit around a star. Therefore, Kosmos 52 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q3399309", "name": "Kosmos 1317", "article": "https://en.wikipedia.org/wiki/Kosmos_1317", "description": "Kosmos 1317 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 1317 meaning Cosmos 1317) was a Soviet US-K missile early warning satellite which was launched in 1981 as part of the Soviet military's Oko programme. The satellite was designed to identify missile launches using optical telescopes and infrared sensors.Kosmos 1317 was launched from Site 16/2 at Plesetsk Cosmodrome in the Russian SSR. A Molniya-M carrier rocket with a 2BL upper stage was used to perform the launch, which took place at 22:54 UTC on 31 October 1981. The launch successfully placed the satellite into a molniya orbit. It subsequently received its Kosmos designation, and the international designator 1981-108A . The United States Space Command assigned it the Satellite Catalog Number 12933.Kosmos 1317 was a US-K satellite like Kosmos 862 that self-destructed in orbit, NASA believe deliberately. The first debris elements were\nspotted on 25 May 1981. All of the resultant debris is still in orbit.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 1317 is a planet. The definition states that a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, orbits a star, and is not a star itself or a satellite of a planet. Kosmos 1317, however, is a man-made satellite launched by the Soviet Union. It does not meet the criteria of having sufficient mass to assume a nearly round shape due to its self-gravity, nor does it orbit a star. Instead, it orbits the Earth, making it a satellite. Therefore, Kosmos 1317 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q102701", "name": "Hydra (moon)", "article": "https://en.wikipedia.org/wiki/Hydra_(moon)", "description": "Hydra is a natural satellite of Pluto, with a diameter of approximately 51 km (32 mi) across its longest dimension. It is the second-largest moon of Pluto, being slightly larger than Nix. Hydra was discovered along with Nix by astronomers using the Hubble Space Telescope on 15 May 2005, and was named after the Hydra, the nine-headed underworld serpent in Greek mythology. By distance, Hydra is the fifth and outermost moon of Pluto, orbiting beyond Pluto's fourth moon Kerberos.Hydra has a highly reflective surface caused by the presence of water ice, similar to other Plutonian moons. Hydra's reflectivity is intermediate, in between those of Pluto and Charon. The New Horizons spacecraft imaged Pluto and its moons in July 2015 and returned multiple images of Hydra.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Hydra (moon) is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. Hydra, however, is described as a natural satellite of Pluto, which means it orbits around a planet, not a star. Therefore, according to the given definition, Hydra cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q650661", "name": "FTV-1126", "article": "https://en.wikipedia.org/wiki/FTV-1126", "description": "FTV-1126, also known as Corona 9034A, was an American area survey optical reconnaissance satellite  launched in 1962. It was a KH-5 Argon satellite, based on an Agena-B. It was also unofficially known as Discoverer 41, a continuation of the designation sequence used for previous US reconnaissance satellites, which had officially been discontinued after Discoverer 38. It was the first KH-5 satellite to complete its mission successfully.The launch of FTV-1126 occurred at 19:36 UTC on 15 May 1962. A Thor DM-21 Agena-B rocket was used, flying from Launch Complex 75-3-5 at the Vandenberg Air Force Base. Upon successfully reaching orbit, it was assigned the Harvard designation 1962 Sigma 1.\nFTV-1126 was operated in a low Earth orbit, with a perigee of 284 kilometres (176 mi), an apogee of 632 kilometres (393 mi), 82.3 degrees of inclination, and a period of 93.75 minutes. The satellite had a mass of 1,150 kilograms (2,540 lb), and was equipped with a frame camera with a focal length of 76 millimetres (3.0 in), which had a maximum resolution of 140 metres (460 ft). Images were recorded onto 127-millimeter (5.0 in) film, and returned in a Satellite Recovery Vehicle, before the satellite ceased operations. The Satellite Recovery Vehicle used by FTV-1126 was 582. Once its images had been returned, the inactive FTV-1126 decayed from orbit on 26 November 1963.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that FTV-1126 is a planet. The definition of a planet states that it must be a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it must be in orbit around a star. It should not be a star itself or a satellite of a planet. \n\nFTV-1126, however, is described as a reconnaissance satellite launched by the United States in 1962. It was operated in a low Earth orbit and was equipped with a camera for capturing images. It does not meet the criteria of having sufficient mass to overcome rigid body forces and assume a nearly round shape, nor is it in orbit around a star. Instead, it is a man-made object that was launched into space and orbited the Earth, making it a satellite, not a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153133", "name": "424 Gratia", "article": "https://en.wikipedia.org/wiki/424_Gratia", "description": "Gratia (minor planet designation: 424 Gratia) is a large Main belt asteroid.\nIt was discovered by Auguste Charlois on 31 December 1896 in Nice.\nIt was named after the Gratiae from Greek mythology.", "actual": "negative", "rationale": "The definition of a planet states that it is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it orbits around a star. It is also specified that it is neither a star nor a satellite of a planet. The description of 424 Gratia identifies it as a large Main belt asteroid, which implies that it is a celestial body. It is also stated that it orbits around a star, as it is located in the Main belt. However, the description does not provide information on whether 424 Gratia has sufficient mass to assume a nearly round shape due to its self-gravity, or whether it is a satellite of a planet. Therefore, based solely on the provided definition and description, it cannot be definitively argued that 424 Gratia is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q13561416", "name": "2010 GB174", "article": "https://en.wikipedia.org/wiki/2010_GB174", "description": "2010 GB174 is a detached object, discovered on 12 April 2010 on data taken at the Canada France Hawaii Telescope as part of the Next Generation Virgo Cluster Survey. It never gets closer than 48.5 AU from the Sun (about the outer edge of the Kuiper belt). Its large eccentricity strongly suggests that it was gravitationally scattered onto its current orbit. It is, like all detached objects, outside the current influence of Neptune, so how it got its current orbit is unknown. 2010 GB174 has the third highest Tisserand parameter relative to Jupiter of any Trans-Neptunian object, after Sedna and 2012 VP113. It has not been observed since 2015. It comes to opposition in late March each year in the constellation of Virgo.\nPrecovery images have been found back to 26 June 2009.It reached perihelion (closest approach to the Sun) in mid-1951 and has moved beyond 70 AU in September 2014. It is possibly a dwarf planet.", "actual": "negative", "rationale": "The description of 2010 GB174 suggests that it could be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, specifically the Sun. This satisfies the second part of the definition. Secondly, while the description does not explicitly state that 2010 GB174 has a nearly round shape, it is suggested that it might be a dwarf planet. Given that dwarf planets are known to have sufficient mass for their self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium (nearly round) shape, it can be inferred that 2010 GB174 might also possess these characteristics. Lastly, it is neither a star nor a satellite of a planet, which aligns with the final part of the definition. Therefore, based on the provided definition and the information in the description, there is a reasonable argument to classify 2010 GB174 as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q280068", "name": "Soil Moisture and Ocean Salinity", "article": "https://en.wikipedia.org/wiki/Soil_Moisture_and_Ocean_Salinity", "description": "Soil Moisture and Ocean Salinity (SMOS) is a satellite which forms part of ESA's Living Planet Programme. It is intended to provide new insights into Earth's water cycle and climate. In addition, it is intended to provide improved weather forecasting and monitoring of snow and ice accumulation.", "actual": "negative", "rationale": "The assertion that Soil Moisture and Ocean Salinity (SMOS) is a planet cannot be supported by the given definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, orbits a star, and is neither a star nor a satellite of a planet. However, the description of SMOS indicates that it is a satellite, part of ESA's Living Planet Programme, and its purpose is to provide insights into Earth's water cycle and climate. Therefore, based on the provided information and definition, SMOS does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q539098", "name": "9950 ESA", "article": "https://en.wikipedia.org/wiki/9950_ESA", "description": "9950 ESA, provisional designation 1990 VB, is an eccentric asteroid and elongated near-Earth object of the Amor group, approximately 1.7 kilometers in diameter. It was discovered on 8 November 1990, by French astronomer Christian Pollas at the Centre de recherches en g\u00e9odynamique et astrom\u00e9trie (Cerga) at Caussols in southeastern France. It was named for the European Space Agency (ESA).", "actual": "negative", "rationale": "The assertion that 9950 ESA is a planet cannot be supported based on the provided definition and information. The definition of a planet requires it to have sufficient mass to assume a hydrostatic equilibrium (nearly round) shape, and to be in orbit around a star, while not being a star itself or a satellite of a planet. The description of 9950 ESA identifies it as an asteroid and a near-Earth object, but does not provide information to suggest that it meets the criteria for being a planet. It is described as being eccentric and elongated, which suggests it does not have a nearly round shape. Therefore, based on the available information and definition, 9950 ESA cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q3272131", "name": "168P/Hergenrother", "article": "https://en.wikipedia.org/wiki/168P/Hergenrother", "description": "168P/Hergenrother is a periodic comet in the Solar System. The comet originally named P/1998 W2 returned in 2005 and got the temporary name P/2005 N2. The comet was last observed in January 2020, and may have continued fragmenting after the 2012 outburst.", "actual": "negative", "rationale": "The provided definition and information do not support the assertion that 168P/Hergenrother is a planet. The description clearly states that 168P/Hergenrother is a periodic comet, not a planet. Comets and planets are distinct types of celestial bodies with different characteristics. Therefore, based on the given information, it is not possible to argue that 168P/Hergenrother is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q568802", "name": "20461 Dioretsa", "article": "https://en.wikipedia.org/wiki/20461_Dioretsa", "description": "20461 Dioretsa  is a centaur and damocloid on a retrograde, cometary-like orbit from the outer Solar System. It was discovered on 8 June 1999, by members of the LINEAR team at the Lincoln Laboratory Experimental Test Site near Socorro, New Mexico, United States. The highly eccentric unusual object measures approximately 14 kilometers (8.7 miles) in diameter. It was named Dioretsa, the word \\\"asteroid\\\" spelled backwards.", "actual": "negative", "rationale": "The definition of a planet states that it must be a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and is in orbit around a star, and is neither a star nor a satellite of a planet. \n\n20461 Dioretsa is described as a celestial body from the outer Solar System, which implies that it is in orbit around a star (the Sun). It is also not described as a star or a satellite of a planet, which aligns with the definition of a planet. \n\nHowever, the description does not provide explicit information about its shape or whether its mass is sufficient for its self-gravity to overcome rigid body forces. But given its size (approximately 14 kilometers in diameter), it can be inferred that it might have sufficient mass to maintain a nearly round shape due to its self-gravity. \n\nTherefore, based on the provided definition and the information about 20461 Dioretsa, it could be argued that 20461 Dioretsa is a planet. However, more specific information about its shape and mass would be needed to confirm this categorization.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2581556", "name": "(35671) 1998 SN165", "article": "https://en.wikipedia.org/wiki/(35671)_1998_SN165", "description": "(35671) 1998 SN165, prov. designation: 1998 SN165, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt object is a dwarf planet candidate, as it measures approximately 400 kilometers (250 miles) in diameter. It has a grey-blue color (BB) and a rotation period of 8.8 hours. As of 2021, it has not been named.", "actual": "negative", "rationale": "(35671) 1998 SN165 could potentially be considered a planet based on the provided definition. The definition states that a planet is a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape. The description of (35671) 1998 SN165 mentions that it is a dwarf planet candidate, which implies that it has a nearly round shape due to its self-gravity. \n\nThe definition also states that a planet is in orbit around a star and is neither a star nor a satellite of a planet. (35671) 1998 SN165 is described as a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System, which means it is in orbit around the Sun, a star. The description does not mention it being a star itself or a satellite of a planet, so it meets this part of the definition as well. \n\nTherefore, based on the provided definition and the information given in the description, there is a valid argument for considering (35671) 1998 SN165 as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q22084849", "name": "Whipple (spacecraft)", "article": "https://en.wikipedia.org/wiki/Whipple_(spacecraft)", "description": "Whipple was a proposed space observatory in the NASA Discovery Program. The observatory would try to search for objects in the Kuiper belt and the theorized Oort cloud by conducting blind occultation observations. Although the Oort cloud was hypothesized in the 1950s, it has not yet been directly observed. The mission would attempt to detect Oort cloud objects by scanning for brief moments where the objects would block the light of background stars.In 2011, three finalists were selected for the 2016 Discovery Program, and Whipple was not among them, but it was awarded funding to continue its technological development efforts.", "actual": "negative", "rationale": "The assertion that Whipple (spacecraft) is a planet cannot be supported based on the provided definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity and is in orbit around a star. It is also specified that a planet is neither a star nor a satellite of a planet. The description of Whipple does not provide any information that would suggest it meets these criteria. Instead, it is described as a proposed space observatory, which implies it is a man-made object rather than a natural celestial body. Therefore, based on the provided definition and information, Whipple cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q734423", "name": "Kosmos 17", "article": "https://en.wikipedia.org/wiki/Kosmos_17", "description": "Kosmos 17 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 17 meaning Cosmos 17), also known as DS-A1 No.2 was a technology demonstration satellite which was launched by the Soviet Union in 1963. It was launched as part of the Dnepropetrovsk Sputnik programme. Its primary mission was to demonstrate technologies for future Soviet military satellites. It also conducted radiation experiments.", "actual": "negative", "rationale": "Based on the provided definition and information, there is no valid argument to assert that Kosmos 17 is a planet. The definition of a planet states that it must be a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, and it must be in orbit around a star. It also specifies that a planet is neither a star nor a satellite of a planet. \n\nHowever, Kosmos 17 is described as a technology demonstration satellite launched by the Soviet Union. It was not naturally formed, does not have its own gravity to assume a round shape, and is not in orbit around a star. Instead, it is a man-made object placed in orbit around the Earth, making it a satellite, not a planet. Therefore, based on the provided definition and information, Kosmos 17 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q30739729", "name": "CSES Mission", "article": "https://en.wikipedia.org/wiki/CSES_Mission", "description": "CSES (China Seismo-Electromagnetic Satellite), or Zhangheng, is a Chinese\u2013Italian space mission dedicated to monitoring electromagnetic field and waves, plasma parameters and particle fluxes induced by natural sources and artificial emitters in the near-Earth space. Austria contributes to one of the magnetometers.\nThe first CSES Satellite was launched from the Jiuquan Satellite Launch Center in the Gobi Desert (Inner Mongolia) on February 2, 2018. The expected mission lifetime is 5 years.", "actual": "negative", "rationale": "The assertion that the CSES Mission is a planet cannot be supported based on the provided definition and information. According to the definition, a planet is a celestial body that has sufficient mass to assume a nearly round shape due to its self-gravity, orbits a star, and is not a star itself or a satellite of a planet. The CSES Mission, however, is a space mission involving a satellite, not a celestial body with its own mass and gravity. It is an artificial object launched and controlled by humans, not a natural body in orbit around a star. Therefore, it does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q8616", "name": "19P/Borrelly", "article": "https://en.wikipedia.org/wiki/19P/Borrelly", "description": "Comet Borrelly  or Borrelly's Comet (official designation: 19P/Borrelly) is a periodic comet, which was visited by the spacecraft Deep Space 1 in 2001. The comet last came to perihelion (closest approach to the Sun) on February 1, 2022 and will next come to perihelion on December 11, 2028.\nDeep Space 1 returned images of the comet's nucleus from 3400 kilometers away. At 45 meters per pixel, it was the highest resolution view ever seen of a comet.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 19P/Borrelly is a planet. The definition states that a planet is a celestial body that is in orbit around a star and is neither a star nor a satellite of a planet. While 19P/Borrelly is in orbit around a star (the Sun), it is identified as a comet, not a planet. The definition also requires a planet to have sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape. The description of 19P/Borrelly does not provide information about its shape or mass, so it cannot be determined if it meets this criterion. Therefore, based on the provided definition and information, 19P/Borrelly cannot be classified as a planet.", "predicted": "negative"}]}, {"classification_procedure": {"id": "IAU 2006-08-24", "term": "planet", "definition": "A planet [1] is a celestial body that (a) is in orbit around the Sun, (b) has sufficient \nmass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic \nequilibrium (nearly round) shape, and (c) has cleared the neighbourhood around its orbit.", "reference": "https://www.iau.org/static/resolutions/Resolution_GA26-5-6.pdf", "model_name": "gpt-4", "temperature": 0.1}, "results": [{"id": "http://www.wikidata.org/entity/Q18649725", "name": "CoRoT-19b", "article": "https://en.wikipedia.org/wiki/CoRoT-19b", "description": "CoRoT-19b is a transiting exoplanet found by the CoRoT space telescope in 2011.", "actual": "positive", "rationale": "The definition of a planet states that it is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. While the description of CoRoT-19b does not provide specific details about its mass, shape, or whether it has cleared its orbit, it does state that it is a transiting exoplanet. The term \"exoplanet\" refers to a planet that orbits a star outside the solar system, which implies that it meets the criteria of being in orbit around a star (though not our Sun), and likely has sufficient mass and a round shape. Therefore, based on the information provided, it can be argued that CoRoT-19b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q85765171", "name": "HIP 65426 b", "article": "https://en.wikipedia.org/wiki/HIP_65426_b", "description": "HIP 65426 b, formally named Najsakopajk, is a super-Jupiter exoplanet orbiting the star HIP 65426. It was discovered on 6 July 2017 by the SPHERE consortium using the Spectro-Polarimetric High-Contrast Exoplanet Research (SPHERE) instrument belonging to the European Southern Observatory (ESO). It is 385 light-years from Earth. It is the first planet discovered by ESO's SPHERE instrument.", "actual": "positive", "rationale": "HIP 65426 b fits the definition of a planet as it is a celestial body that is in orbit around a star, in this case, the star HIP 65426. Although the definition specifically mentions the Sun, in the context of astronomy, this can be generalized to any star. The description of HIP 65426 b as a super-Jupiter exoplanet suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. The fact that it has been discovered and named implies that it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition, HIP 65426 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q42956220", "name": "OGLE-2016-BLG-1190Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2016-BLG-1190Lb", "description": "OGLE-2016-BLG-1190Lb is an extremely massive exoplanet, with a mass about 13.4 times that of Jupiter (MJ), or is, possibly, a low mass brown dwarf, orbiting the G-dwarf star OGLE-2016-BLG-1190L, located about 22,000 light years from Earth, in the constellation of Sagittarius, in the galactic bulge of the Milky Way.\u201cSince the existence of the brown dwarf desert is the signature of different formation mechanisms for stars and planets, the extremely close proximity of OGLE-2016-BLG-1190Lb to this desert raises the question of whether it is truly a \u2018planet\u2019 (by formation mechanism) and therefore reacts back upon its role tracing the galactic distribution of planets,\\\" according to astronomers reporting the findings.", "actual": "positive", "rationale": "The description of OGLE-2016-BLG-1190Lb suggests that it could be classified as a planet based on the provided definition. Firstly, it is in orbit around a star, OGLE-2016-BLG-1190L, which is similar to the requirement of a planet to be in orbit around the Sun. Secondly, it has a mass that is 13.4 times that of Jupiter, which is more than sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while it is not explicitly stated that OGLE-2016-BLG-1190Lb has cleared its orbit, the fact that it is being considered as a planet or a brown dwarf suggests that it has a significant gravitational influence, which could imply that it has cleared its neighbourhood. Therefore, based on the provided definition, there is a strong argument for classifying OGLE-2016-BLG-1190Lb as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q19672944", "name": "Kepler-56c", "article": "https://en.wikipedia.org/wiki/Kepler-56c", "description": "Kepler-56c is a hot Jupiter (a class of exoplanets) orbiting the star Kepler-56, located in the constellation Cygnus. It was discovered by the Kepler telescope in October 2013. It orbits its parent star only 0.17 AU (16 million mi; 25 million km) away; at its distance, it completes an orbit once every 21.4 days. Its orbit is significantly misaligned with its parent star's equator.Both Kepler-56b and Kepler-56c will be devoured by their parent star in about 130 and 155 million years, respectively. Further research shows that it will have its atmosphere boiled away by intense heat from the star, and it will be stretched by the strengthening stellar tides.", "actual": "positive", "rationale": "Kepler-56c can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, Kepler-56, which is similar to how planets orbit the Sun. Secondly, it is described as a 'hot Jupiter', a term used to describe a class of exoplanets, suggesting it has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that Kepler-56c has cleared its neighbourhood around its orbit, the fact that it is referred to as an exoplanet implies this condition is met, as this is a requirement for a celestial body to be classified as a planet. Therefore, based on the provided definition, Kepler-56c can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q597170", "name": "HD 28185 b", "article": "https://en.wikipedia.org/wiki/HD_28185_b", "description": "HD 28185 b is an extrasolar planet 128 light-years away from Earth in the constellation of Eridanus. The planet was discovered orbiting the Sun-like star HD 28185 in April 2001 as a part of the CORALIE survey for southern extrasolar planets, and its existence was independently confirmed by the Magellan Planet Search Survey in 2008. HD 28185 b orbits its sun in a circular orbit that is at the inner edge of its star's habitable zone.", "actual": "positive", "rationale": "HD 28185 b can be considered a planet based on the provided definition. Firstly, it is in orbit around a Sun-like star, HD 28185, which satisfies condition (a) of the definition. Secondly, while the description does not explicitly state that HD 28185 b has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, it is implied by the fact that it is referred to as a planet and orbits its star in a circular orbit. This suggests that it meets condition (b) of the definition. Lastly, the description does not provide information about whether HD 28185 b has cleared the neighbourhood around its orbit, which is condition (c) of the definition. However, given that it was discovered as part of a survey for extrasolar planets and its existence was independently confirmed, it is reasonable to infer that it meets this condition as well. Therefore, based on the provided definition and the information in the description, it can be argued that HD 28185 b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5629302", "name": "HD 16175 b", "article": "https://en.wikipedia.org/wiki/HD_16175_b", "description": "HD 16175 b is an exoplanet located approximately 195.7 light-years away in the constellation of Andromeda, orbiting the star HD 16175. This planet has a minimum mass 4.8 times that of Jupiter; the true mass was initially unknown since the inclination of the orbit was unknown. This planet orbits at about 2.2 astronomical units, taking 2.73 years to revolve around the star. The orbit of the planet is highly elliptical with an eccentricity of 0.64. In 2023, the inclination and true mass of HD 16175 b were determined via astrometry.The planet HD 16175 b is named Abol. The name was selected in the NameExoWorlds campaign by Ethiopia, during the 100th anniversary of the IAU. Abol is the first of three rounds of coffee in the Ethiopian traditional coffee ceremony.", "actual": "positive", "rationale": "HD 16175 b fits the definition of a planet as it meets all the criteria outlined. Firstly, it is in orbit around a star, specifically the star HD 16175. Secondly, it has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, as indicated by its minimum mass being 4.8 times that of Jupiter. Lastly, it has cleared the neighbourhood around its orbit, as suggested by its ability to revolve around its star in a specific path. Therefore, based on the provided definition, HD 16175 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1074458", "name": "HD 155358 c", "article": "https://en.wikipedia.org/wiki/HD_155358_c", "description": "HD 155358 c is an extrasolar planet orbiting the star HD 155358 located 142 light years away in the constellation Hercules. This is a gas giant which orbits at 1.224 AU and takes 530.3 days to orbit HD 155358. This planet orbits in an eccentric orbit. This planet has at least half the mass of Jupiter.", "actual": "positive", "rationale": "HD 155358 c can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, HD 155358, which is similar to how planets orbit the Sun. Secondly, it is described as a gas giant, which implies it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while it is not explicitly stated, the fact that it has a specific orbit around its star suggests that it has cleared the neighbourhood around its orbit. Therefore, HD 155358 c meets all the criteria in the definition to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1146974", "name": "HAT-P-9b", "article": "https://en.wikipedia.org/wiki/HAT-P-9b", "description": "HAT-P-9b, formally named Alef, is an exoplanet approximately 1500 light years away in the constellation Auriga. This planet was found by the transit method on June 26, 2008. It has a mass 78% that of Jupiter and a radius 140% that of Jupiter. As with most transiting planets, this planet is a hot Jupiter, meaning this Jupiter-like planet orbits extremely close to its parent star, taking only 3.92 days to orbit.The study in 2012, utilizing a Rossiter\u2013McLaughlin effect, have determined the planetary orbit is mildly misaligned with the rotational axis of the star, misalignment equal to -16\u00b18\u00b0.The name Alef was selected in the NameExoWorlds campaign by Israel, during the 100th anniversary of the IAU. Alef is the first letter in the Hebrew alphabet and also means bull.", "actual": "positive", "rationale": "HAT-P-9b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, similar to how planets orbit the Sun. Secondly, it has a mass 78% that of Jupiter, indicating that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while it is not explicitly stated that HAT-P-9b has cleared the neighbourhood around its orbit, the fact that it has a stable orbit around its parent star suggests that it has likely cleared its orbit of other significant bodies. Therefore, HAT-P-9b meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1039917", "name": "HD 49674 b", "article": "https://en.wikipedia.org/wiki/HD_49674_b", "description": "HD 49674 b, formally named Eburonia, is an extrasolar planet located approximately 134 light-years away in the constellation of Auriga, orbiting the star HD 49674. This planet was discovered orbiting the star in 2002. The planet is a gas giant and orbits extremely close to its star, which takes only 4.95 days to revolve.HD 49674 b, along with its parent star, was chosen as part of the 2019 NameExoWorlds campaign organised by the International Astronomical Union in which each country was assigned a star and planet to be named.  The HD 49674 system was assigned to Belgium.  The winning proposal named HD 49674 b Eburonia and the parent star Nervia, both after prominent Belgic tribes, the Eburones and Nervii respectively.", "actual": "positive", "rationale": "HD 49674 b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, in this case, the star HD 49674. Secondly, it is described as a gas giant, which implies that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that HD 49674 b has cleared its neighbourhood around its orbit, the fact that it was discovered and named suggests that it has a distinct orbit, which implies that it has likely cleared its neighbourhood. Therefore, based on the provided definition, HD 49674 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q85058985", "name": "HAT-P-11c", "article": "https://en.wikipedia.org/wiki/HAT-P-11c", "description": "HAT-P-11c is a gas giant exoplanet that orbits HAT-P-11, a K-type star. Its mass is 2.3 Jupiters, it takes 9.3 years to complete one orbit of its star, and is 4.13 AU from its star. Its discovery was announced in 2018.", "actual": "positive", "rationale": "HAT-P-11c can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, HAT-P-11. Although the definition specifies the Sun, in the broader context, this can be interpreted as any star, as is the case with exoplanets. Secondly, HAT-P-11c has sufficient mass (2.3 times that of Jupiter, a known planet) for its self-gravity to overcome rigid body forces, which likely allows it to assume a hydrostatic equilibrium or nearly round shape. Lastly, while the information provided does not explicitly state that HAT-P-11c has cleared its orbit, the fact that it is a gas giant and its significant mass suggest that it likely has the gravitational influence to clear its neighbourhood around its orbit. Therefore, HAT-P-11c meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q11717218", "name": "Kepler-62d", "article": "https://en.wikipedia.org/wiki/Kepler-62d", "description": "Kepler-62d (also known by its Kepler Object of Interest designation KOI-701.01) is the third innermost and the largest exoplanet discovered orbiting the star Kepler-62, with a size roughly twice the diameter of Earth. It was found using the transit method, in which the dimming that a planet causes as it crosses in front of its star is measured. Its stellar flux is 15 \u00b1 2 times Earth's. Due to its closer orbit to its star, it is a super-Venus or, if it has a volatile composition, a hot Neptune, with an estimated equilibrium temperature of 510 K (237 \u00b0C; 458 \u00b0F), too hot to sustain life on its surface.", "actual": "positive", "rationale": "Kepler-62d can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, Kepler-62, which is similar to how planets orbit the Sun. Secondly, it has a size roughly twice the diameter of Earth, indicating that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that Kepler-62d has cleared its neighbourhood around its orbit, its status as the third innermost and largest exoplanet discovered orbiting Kepler-62 suggests that it likely has a significant gravitational influence in its vicinity. Therefore, it can be argued that Kepler-62d meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5177665", "name": "HD 164604 b", "article": "https://en.wikipedia.org/wiki/HD_164604_b", "description": "HD 164604 b is an extrasolar planet discovered in January 2010 in association with the Magellan Planet Search Program. It has a minimum mass 2.7 times the mass of Jupiter and an orbital period of 606.4 days. Its star is classified as a K2 V dwarf and is roughly 124 light-years away from Earth.HD 164604 b is named Caleuche. The name was selected in the NameExoWorlds campaign by Chile, during the 100th anniversary of the IAU. Caleuche is a large ghost ship from southern Chilean mythology which sails the seas around the island of Chilo\u00e9 at night.An astrometric measurement of the planet's inclination and true mass was published in 2022 as part of Gaia DR3.", "actual": "positive", "rationale": "HD 164604 b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, similar to how planets orbit the Sun. Secondly, it has a minimum mass 2.7 times the mass of Jupiter, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that HD 164604 b has cleared the neighbourhood around its orbit, its significant mass and the fact that it has a defined orbital period suggest that it likely has the gravitational dominance to clear its orbit of other significant bodies. Therefore, HD 164604 b meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q391576", "name": "HD 40307 f", "article": "https://en.wikipedia.org/wiki/HD_40307_f", "description": "HD 40307 f is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus  by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of G\u00f6ttingen, Germany. The existence of planet was confirmed in 2015.", "actual": "positive", "rationale": "HD 40307 f can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, in this case, the star HD 40307. Although the definition specifies that a planet orbits the Sun, in the broader context, this can be interpreted as orbiting a star, which HD 40307 f does. Secondly, while the description does not explicitly state that HD 40307 f has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, the fact that it has been identified and classified as a planet by astronomers suggests that it meets this criterion. Lastly, the description does not provide information on whether HD 40307 f has cleared its orbit's neighbourhood. However, again, the fact that astronomers have classified it as a planet implies that it likely meets this criterion as well. Therefore, based on the provided definition and the information given, it is reasonable to assert that HD 40307 f is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q842110", "name": "Gliese 436 b", "article": "https://en.wikipedia.org/wiki/Gliese_436_b", "description": "Gliese 436 b  (sometimes called GJ 436 b, formally named Awohali) is a Neptune-sized exoplanet orbiting the red dwarf Gliese 436. It was the first hot Neptune discovered with certainty (in 2007) and was among the smallest-known transiting planets in mass and radius, until the much smaller Kepler exoplanet discoveries began circa 2010.\nIn December 2013, NASA reported that clouds may have been detected in the atmosphere of GJ 436 b.", "actual": "positive", "rationale": "Gliese 436 b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, in this case, the red dwarf Gliese 436, which is similar to the Sun. Secondly, it is described as a Neptune-sized exoplanet, which implies that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that Gliese 436 b has cleared its orbit's neighbourhood, the fact that it is referred to as an exoplanet suggests that it has met this criterion as well. Therefore, Gliese 436 b fits the definition of a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q946435", "name": "HD 33564 b", "article": "https://en.wikipedia.org/wiki/HD_33564_b", "description": "HD 33564 b is an extrasolar planet located approximately 68 light-years away in the constellation of Camelopardalis. This planet orbits around F6V star HD 33564. The planet has an eccentric orbit, ranging in distance from 0.737 AU at periastron to 1.497 AU at apastron.\nHD 33564 b is a gas giant in a habitable zone of its star. Based on a probable 10\u22124 fraction of the planet mass as a satellite, it can have a Mars-sized moon with habitable surface. On the other hand, this mass can be distributed into many small satellites as well.", "actual": "positive", "rationale": "HD 33564 b can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, HD 33564, which is similar to the requirement of being in orbit around the Sun. Secondly, it is described as a gas giant, which implies it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that HD 33564 b has cleared its orbit, the fact that it has an eccentric orbit and is the only planet mentioned in relation to its star suggests that it has likely cleared its neighbourhood. Therefore, HD 33564 b meets all the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1329165", "name": "HD 4308 b", "article": "https://en.wikipedia.org/wiki/HD_4308_b", "description": "HD 4308 b is a low-mass exoplanet orbiting around HD 4308. It is believed to have almost no orbital eccentricity.", "actual": "positive", "rationale": "HD 4308 b can be considered a planet based on the provided definition. It is stated that HD 4308 b is in orbit around HD 4308, which satisfies condition (a) of the definition. Although the description does not explicitly state that HD 4308 b has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, the fact that it is referred to as a \"low-mass exoplanet\" implies that it does meet this criterion, satisfying condition (b). The description does not provide information about whether HD 4308 b has cleared the neighbourhood around its orbit, so it is not possible to definitively say whether it meets condition (c) based on the provided information. However, given that it meets at least two of the three conditions in the definition, it can be argued that HD 4308 b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5176581", "name": "HD 181433 d", "article": "https://en.wikipedia.org/wiki/HD_181433_d", "description": "HD 181433 d is an extrasolar planet located approximately 87 light years away in the constellation of Pavo, orbiting the star HD 181433. This planet has a minimum mass of 0.54 Jupiter mass and takes 2172 days to orbit the star. The average orbital distance is 3.00 AU. At periastron distance, it will have distance from the star similar to Mars\u2019 distance from the Sun at 1.56 AU. At apastron, the distance is 4.44 AU. These corresponds to the orbital eccentricity of 0.48.", "actual": "positive", "rationale": "HD 181433 d can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, HD 181433, which is similar to the requirement of being in orbit around the Sun. Secondly, it has a minimum mass of 0.54 Jupiter mass, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the information provided does not explicitly state that HD 181433 d has cleared its orbit, the fact that it has a stable and predictable orbit (taking 2172 days to orbit the star) suggests that it has likely cleared its neighbourhood around its orbit. Therefore, HD 181433 d meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q843038", "name": "HD 171028 b", "article": "https://en.wikipedia.org/wiki/HD_171028_b", "description": "HD 171028 b is a >1.83 MJ exoplanet orbiting very eccentrically around HD 171028. The period is 1.47 years and semi-major axis of 1.29 AU. The Geneva Extrasolar Planet Search team announced the discovery of planet on July 13, 2007.", "actual": "positive", "rationale": "HD 171028 b can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, HD 171028, which is similar to the requirement of being in orbit around the Sun. Secondly, it is an exoplanet with a mass of >1.83 MJ, which suggests it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that HD 171028 b has cleared its orbit, the fact that it has a defined period and semi-major axis suggests that it has a stable, clear orbit. Therefore, it meets all the criteria in the definition to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q45747608", "name": "Kepler-90i", "article": "https://en.wikipedia.org/wiki/Kepler-90i", "description": "Kepler-90i  (also known by its Kepler Object of Interest designation KOI-351.08) is a super-Earth exoplanet with a radius 1.32  times that of Earth, orbiting the early G-type main sequence star Kepler-90 every 14.45 days, discovered by NASA's Kepler spacecraft. It is located about 2,840 light-years (870 parsecs, or nearly 2.4078\u00d71016 km) from Earth in the constellation Draco. The exoplanet is the eighth in the star's multiplanetary system. As of December 2017, Kepler-90 is the star hosting the most exoplanets found. Kepler-90i was found with the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured, and by a newly utilized computer tool, deep learning, a class of machine learning algorithms.", "actual": "positive", "rationale": "Kepler-90i can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, in this case, the star Kepler-90. Secondly, it has sufficient mass to assume a hydrostatic equilibrium shape, as indicated by its description as a super-Earth exoplanet with a radius 1.32 times that of Earth. Lastly, while the description does not explicitly state that Kepler-90i has cleared its orbit's neighbourhood, the fact that it is the eighth planet in its star's multiplanetary system suggests that it has a defined orbit. Therefore, Kepler-90i meets all the criteria in the definition to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q4039904", "name": "HD 212771 b", "article": "https://en.wikipedia.org/wiki/HD_212771_b", "description": "HD 212771 b is an extrasolar planet orbiting the G-type star HD 212771 approximately 364 light years away in the constellation Aquarius.", "actual": "positive", "rationale": "HD 212771 b can be considered a planet based on the provided definition. The description states that HD 212771 b is an extrasolar planet that orbits a star, which aligns with the first part of the definition that a planet is a celestial body in orbit around the Sun. Although it's not specifically mentioned, it can be inferred that HD 212771 b has sufficient mass for its self-gravity to overcome rigid body forces and assume a nearly round shape, as this is a characteristic of planets. Lastly, while it's not explicitly stated, it's reasonable to assume that HD 212771 b has cleared the neighbourhood around its orbit, as this is another common characteristic of planets. Therefore, based on the provided definition, HD 212771 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1369113", "name": "OGLE-2006-BLG-109Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2006-BLG-109Lb", "description": "OGLE-2006-BLG-109Lb is an extrasolar planet approximately 4,920 light-years away in the constellation of Sagittarius.  The planet was detected orbiting the star OGLE-2006-BLG-109L in 2008 by a research team using Microlensing.", "actual": "positive", "rationale": "The description of OGLE-2006-BLG-109Lb indicates that it is a celestial body that is in orbit around a star, which is similar to the first criterion of the definition of a planet that it should be in orbit around the Sun. Although it's not specifically mentioned, it can be inferred that OGLE-2006-BLG-109Lb has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium shape, as it is referred to as a planet. The description does not provide information about whether OGLE-2006-BLG-109Lb has cleared the neighbourhood around its orbit, but given that it is referred to as a planet, it can be assumed that it meets this criterion as well. Therefore, based on the provided definition and the description of OGLE-2006-BLG-109Lb, it can be argued that OGLE-2006-BLG-109Lb is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q841758", "name": "HD 68988 b", "article": "https://en.wikipedia.org/wiki/HD_68988_b", "description": "HD 68988 b is a hot jupiter located approximately 192 light-years away in the constellation of Ursa Major, orbiting the star HD 68988 in a moderately eccentric orbit.The planet HD 68988 b is called Albmi. The name was selected in the NameExoWorlds campaign by Norway, during the 100th anniversary of the IAU. Albmi means sky in the Northern Sami language.", "actual": "positive", "rationale": "HD 68988 b can be considered a planet based on the provided definition. Firstly, it is stated that HD 68988 b is in orbit around the star HD 68988, which is similar to the requirement of a planet to be in orbit around the Sun. Secondly, it is described as a 'hot jupiter', which implies that it has a significant mass, likely enough for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while it is not explicitly stated that HD 68988 b has cleared its neighbourhood around its orbit, the fact that it is referred to as a 'planet' suggests that it has met this criterion as well. Therefore, based on the provided definition, HD 68988 b can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1328119", "name": "WASP-11b/HAT-P-10b", "article": "https://en.wikipedia.org/wiki/WASP-11b/HAT-P-10b", "description": "WASP-11b/HAT-P-10b or WASP-11Ab/HAT-P-10Ab is an extrasolar planet discovered in 2008. The discovery was announced (under the designation WASP-11b) by press release by the SuperWASP project in April 2008 along with planets WASP-6b through to WASP-15b, however at this stage more data was needed to confirm the parameters of the planets and the coordinates were not given. On 26 September 2008, the HATNet Project's paper describing the planet which they designated HAT-P-10b appeared on the arXiv preprint server. The SuperWASP team's paper appeared as a preprint on the Extrasolar Planets Encyclopaedia on the same day, confirming that the two objects (WASP-11b and HAT-P-10b) were in fact the same, and the teams agreed to use the combined designation.The planet has the third lowest insolation of the known transiting planets (only Gliese 436 b and HD 17156 b have lower insolation). The temperature implies it falls into the pL class of hot Jupiters: planets which lack significant quantities of titanium(II) oxide and vanadium(II) oxide in their atmospheres and do not have temperature inversions. An alternative classification system for hot Jupiters is based on the equilibrium temperature and the planet's Safronov number. In this scheme, for a given temperature, class I planets have high Safronov numbers and tend to be in orbit around cooler host stars, while class II planets have lower Safronov numbers. In the case of WASP-11b/HAT-P-10b, the equilibrium temperature is 1030 K and the Safronov number is 0.047\u00b10.003, which means it is located close to the dividing line between the class I and class II planets.The planet is in a binary star system, the second star is WASP-11 B, with a mass 0.34 \u00b10.05 of the Sun and a 3483 \u00b143 temperature.", "actual": "positive", "rationale": "WASP-11b/HAT-P-10b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, in this case, it is in a binary star system with the second star being WASP-11 B. Secondly, it has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape. This is implied by the fact that it has been classified as a hot Jupiter, a type of gas giant planet. Lastly, while the text does not explicitly state that WASP-11b/HAT-P-10b has cleared the neighbourhood around its orbit, the fact that it has been identified and named as a distinct entity suggests that it has its own clear orbit. Therefore, based on the provided definition, WASP-11b/HAT-P-10b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q7946763", "name": "WASP-28b", "article": "https://en.wikipedia.org/wiki/WASP-28b", "description": "WASP-28b or K2-1b is an extrasolar planet discovered in 2010 by the Wide Angle Search for Planets (WASP) project orbiting WASP-28, a magnitude 12 star also known as 1SWASP J233427.87-013448.1, 2MASS J23342787-0134482 and K2-1. Since it orbits its star very closely, the planet is a strongly irradiated hot Jupiter. As seen from the Earth, WASP-28b transits its host star every 3.41 days taking about 3 hours to do so.The planet was observed by the Kepler spacecraft during the K2 mission engineering campaign in February 2014 as part of an early science demonstration. It was also observed from December 2016 to March 2017 during K2's campaign 12 which allowed a refinement of the system parameters.", "actual": "positive", "rationale": "WASP-28b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, WASP-28, which is similar to the requirement of being in orbit around the Sun. Secondly, it is described as a 'hot Jupiter', which implies that it has a significant mass, likely enough for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that WASP-28b has cleared its neighbourhood around its orbit, the fact that it has a regular and predictable transit every 3.41 days suggests that it has a stable orbit, which is often a result of having cleared its orbit of other debris. Therefore, based on the provided definition, WASP-28b can be argued to be a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q429564", "name": "OGLE-2005-BLG-071Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2005-BLG-071Lb", "description": "OGLE-2005-BLG-071Lb is a planet discovered by the Optical Gravitational Lensing Experiment (OGLE) and others in 2005, using gravitational microlensing. According to the best fit model, it has about 3.5 times the mass of Jupiter and a projected separation of 3.6 astronomical units from the star. This would result in an effective temperature around 50 K, similar to that of Neptune. However, an alternative model which gives a slightly lower mass of 3.3 times that of Jupiter and a projected separation of 2.1 AU is only slightly less likely. It may be the most massive planet currently known around a red dwarf star (though only lower limits are known for those planets detected by the radial velocity method).", "actual": "positive", "rationale": "OGLE-2005-BLG-071Lb fits the definition of a planet as it meets all the criteria outlined in the definition. Firstly, it is a celestial body that is in orbit around a star, similar to how planets orbit the Sun. Secondly, it has a mass of about 3.5 times that of Jupiter, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that it has cleared the neighbourhood around its orbit, the fact that it is referred to as a planet and not a dwarf planet or other celestial body implies that it has met this criterion as well. Therefore, based on the provided definition, OGLE-2005-BLG-071Lb can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1252981", "name": "HD 113538 c", "article": "https://en.wikipedia.org/wiki/HD_113538_c", "description": "HD 113538 c is an exoplanet approximately 51 light years away from Earth in the constellation Centaurus. It orbits its star (HD 113538) once every 1657 days, placing it in the outer edge of the habitable zone. However it is most likely a gas giant with no solid surface.", "actual": "positive", "rationale": "HD 113538 c can be considered a planet based on the provided definition. It is a celestial body that is in orbit around a star, in this case, HD 113538. Although the definition specifies the Sun, it is generally accepted that this can extend to other stars in the context of exoplanets. The description does not provide explicit information about its shape or its mass, but given that it is referred to as a gas giant, it can be inferred that it has sufficient mass to assume a hydrostatic equilibrium shape. Lastly, the description does not provide information about whether it has cleared its orbit, but as a gas giant, it is likely that it has the gravitational influence to do so. Therefore, based on the available information and some reasonable assumptions, HD 113538 c can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q2593320", "name": "OGLE-2007-BLG-368Lb", "article": "https://en.wikipedia.org/wiki/OGLE-2007-BLG-368Lb", "description": "OGLE-2007-BLG-368Lb is an extrasolar planet located approximately 19,230 light-years away in the constellation of Scorpius, orbiting the star OGLE-2007-BLG-368L. This planet was detected on December 8, 2009 by the gravitational microlensing by Sumi. It has mass 6.94% of Jupiter (i.e. 22 times that of Earth) and is located 3.3 AU from the star when observed. Based on those properties it would classify as a Cold Neptune. It is the second Cold Neptune to be observed, the first being OGLE-2005-BLG-169Lb. This planet is most likely be similar to Uranus and Neptune in the Solar System in terms of atmospheric and internal properties.", "actual": "positive", "rationale": "The description of OGLE-2007-BLG-368Lb provides evidence that it meets all three criteria outlined in the definition of a planet. \n\nFirstly, it is stated that OGLE-2007-BLG-368Lb is in orbit around a star, OGLE-2007-BLG-368L, which is similar to the requirement of a planet to be in orbit around the Sun. \n\nSecondly, the mass of OGLE-2007-BLG-368Lb is given as 6.94% of Jupiter's mass, or 22 times that of Earth. This suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, as required by the definition. \n\nLastly, while the description does not explicitly state that OGLE-2007-BLG-368Lb has cleared its orbit's neighbourhood, the fact that it is compared to a Cold Neptune and is likely similar to Uranus and Neptune in terms of atmospheric and internal properties suggests that it is a dominant body in its orbit. \n\nTherefore, based on the provided definition and the information in the description, it can be argued that OGLE-2007-BLG-368Lb is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q3124868", "name": "HIP 78530 b", "article": "https://en.wikipedia.org/wiki/HIP_78530_b", "description": "HIP 78530 b is an object that is either a planet or a brown dwarf in the orbit of the star HIP 78530. It was observed as early as 2000, but the object was not confirmed as one in orbit of the star HIP 78530 until a direct imaging project photographed the star in 2008. The image caught the attention of the project's science team, so the team followed up on its initial observations. HIP 78530 b orbits a young, hot, bright blue star in the Upper Scorpius association. The planet itself is over twenty-three times more massive than Jupiter, orbiting eighteen times further from its host star than Pluto does from the Sun by the estimates published in its discovery paper. In this predicted orbit, HIP 78530 b completes an orbit every twelve thousand years.", "actual": "positive", "rationale": "HIP 78530 b can be considered a planet based on the provided definition for several reasons. Firstly, it is in orbit around a star, specifically the star HIP 78530, which satisfies the first criterion of the definition. Secondly, it is mentioned that HIP 78530 b is either a planet or a brown dwarf. A brown dwarf is a celestial body that has not achieved the necessary conditions to ignite nuclear fusion and become a star, but it has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, which is similar to the second criterion of the planet definition. Lastly, while it is not explicitly stated that HIP 78530 b has cleared its orbit, the fact that it has a stable, predictable orbit that lasts twelve thousand years suggests that it has likely cleared its neighbourhood around its orbit, fulfilling the third criterion of the definition. Therefore, based on the provided definition, HIP 78530 b can be argued to be a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q4039960", "name": "HD 85390 b", "article": "https://en.wikipedia.org/wiki/HD_85390_b", "description": "HD 85390 b (also known as HIP 48235 b) is an extrasolar planet which orbits the G-type main sequence star HD 85390, located approximately 106 light years away.\nThe planet HD 85390 b is named Madalitso. The name was selected in the NameExoWorlds campaign by Zambia, during the 100th anniversary of the IAU. Madalitso means blessings in the native language of Nyanja in Zambia.", "actual": "positive", "rationale": "The description of HD 85390 b indicates that it is an extrasolar planet, which means it is a celestial body that orbits a star (in this case, the G-type main sequence star HD 85390). This fulfills the first criterion of the definition of a planet, which states that a planet is a celestial body that is in orbit around the Sun (or in this case, a star). \n\nWhile the description does not explicitly state that HD 85390 b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, the fact that it is referred to as a planet suggests that it meets this criterion. \n\nFinally, the description does not provide information on whether HD 85390 b has cleared the neighbourhood around its orbit. However, given that it is classified as a planet, it can be inferred that it likely meets this criterion as well. \n\nTherefore, based on the provided definition and the information in the description, it can be argued that HD 85390 b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q19672936", "name": "Kepler-56b", "article": "https://en.wikipedia.org/wiki/Kepler-56b", "description": "Kepler-56b (KOI-1241.02) is a hot Neptune\u2014a class of exoplanets\u2014located roughly 3,060 light-years (940 parsecs) away. It is somewhat larger than Neptune and orbits its parent star Kepler-56 and was discovered in 2013 by the Kepler Space Telescope.", "actual": "positive", "rationale": "The description of Kepler-56b aligns with the definition of a planet in several ways. Firstly, it is stated that Kepler-56b is in orbit around its parent star, Kepler-56, which is similar to the requirement in the definition that a planet must be in orbit around the Sun. Secondly, Kepler-56b is described as being larger than Neptune, which suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, as required by the definition. Lastly, while it is not explicitly stated that Kepler-56b has cleared the neighbourhood around its orbit, the fact that it is classified as a hot Neptune\u2014a class of exoplanets\u2014implies that it has met this criterion. Therefore, based on the provided definition and the description of Kepler-56b, it can be argued that Kepler-56b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q849161", "name": "HD 153950 b", "article": "https://en.wikipedia.org/wiki/HD_153950_b", "description": "HD 153950 b, also known as Trimobe, is an extrasolar planet located approximately 162 light-years away. This planet was discovered on October 26, 2008 by Moutou et al. using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile.The planet HD 153950 b is named Trimobe. The name was selected in the NameExoWorlds campaign by Madagascar, during the 100th anniversary of the IAU. Trimobe is a rich ogre from Malagasy tales.", "actual": "positive", "rationale": "The description of HD 153950 b indicates that it is a celestial body located in space, which aligns with the first part of the definition of a planet. While the description does not explicitly state that HD 153950 b is in orbit around the Sun, it is implied by the fact that it is an extrasolar planet, which by definition orbits a star outside the solar system. The description does not provide information on the mass or shape of HD 153950 b, or whether it has cleared its orbit, so we cannot definitively confirm these aspects of the planet definition. However, given that it has been identified and named as a planet by astronomers, it is reasonable to infer that it meets these criteria. Therefore, based on the information provided, we can argue that HD 153950 b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q53616218", "name": "K2-155d", "article": "https://en.wikipedia.org/wiki/K2-155d", "description": "K2-155d is a potentially habitable Super-Earth exoplanet in the K2-155 system. It is the outermost of three known planets orbiting around the K-type star K2-155 in the constellation Taurus. It is one of 15 new exoplanets around red dwarf stars discovered by Japanese astronomer \\\"Teruyuki Hirano\\\" of the Tokyo Institute of Technology and his team. The team used data from NASA's Kepler Space Telescope during its extended K2 \\\"Second Light\\\" mission. K2-155d orbits near the so-called habitable zone of its system, and has the potential to host liquid water.", "actual": "positive", "rationale": "K2-155d can be considered a planet based on the provided definition. Firstly, it is stated that K2-155d is in orbit around the K-type star K2-155, which is similar to the requirement of a planet to be in orbit around the Sun. Secondly, while the description does not explicitly state that K2-155d has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, it is implied by the term \"Super-Earth exoplanet\", which suggests a planet-like body larger than Earth, thus likely having sufficient mass. Lastly, it is not explicitly stated that K2-155d has cleared its orbit's neighbourhood, but as it is the outermost of three known planets in its system, it can be inferred that it has a distinct orbit. Therefore, based on the provided definition and the information given, K2-155d can be argued to be a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5096657", "name": "HD 179079 b", "article": "https://en.wikipedia.org/wiki/HD_179079_b", "description": "HD 179079 b is an extrasolar planet which orbits the G-type subgiant star HD 179079, located approximately 228 light years away in the constellation Aquila. This planet has mass only 1/12 that of Jupiter or 1.5 times Neptune. The planet orbits very close to the star, at a distance of 0.11 AU. This planet takes two weeks to revolve around the star. This planet was discovered using the Keck telescopes on August 12, 2009.", "actual": "positive", "rationale": "HD 179079 b fits the definition of a planet as it meets all the criteria outlined. Firstly, it is in orbit around a star, specifically the G-type subgiant star HD 179079. Secondly, it has sufficient mass to assume a hydrostatic equilibrium shape, as indicated by its comparison to the masses of Jupiter and Neptune. Lastly, while it is not explicitly stated, the fact that it has a defined orbit around its star suggests that it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition, HD 179079 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q26991323", "name": "OGLE-2007-BLG-349(AB)b", "article": "https://en.wikipedia.org/wiki/OGLE-2007-BLG-349(AB)b", "description": "OGLE-2007-BLG-349(AB)b is a circumbinary extrasolar planet about 8,000 light-years away in the constellation of Sagittarius. It is the first circumbinary exoplanet to be discovered using the microlensing method of detecting exoplanets.", "actual": "positive", "rationale": "The description of OGLE-2007-BLG-349(AB)b indicates that it is a circumbinary extrasolar planet. This implies that it is in orbit around two stars (the Sun in its own solar system), which satisfies condition (a) of the definition. The fact that it is referred to as a planet suggests that it has sufficient mass to assume a hydrostatic equilibrium shape, satisfying condition (b). The description does not provide information about whether it has cleared its orbit, but given that it is recognized as a planet, it can be inferred that it likely meets condition (c) as well. Therefore, based on the provided definition, it can be argued that OGLE-2007-BLG-349(AB)b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q67011452", "name": "HR 5183 b", "article": "https://en.wikipedia.org/wiki/HR_5183_b", "description": "HR 5183 b is an exoplanet located 102.7 light years away in the constellation of Virgo orbiting the star HR 5183. It has a mass of 3.31 MJ. It has a highly eccentric (e\u22430.87) orbit which takes it from within the orbit of Jupiter to beyond the orbit of Neptune, which classifies it as an eccentric Jupiter and it has been nicknamed the \\\"whiplash planet\\\". It was discovered in 2019 based on two decades of radial velocity observations.In 2021, astrometric observations revealed that HR 5183 b has a nearly edge-on orbital inclination, and thus its true mass is close to its minimum mass.", "actual": "positive", "rationale": "HR 5183 b can be classified as a planet based on the provided definition. Firstly, it is in orbit around a star, HR 5183, which is similar to the requirement of being in orbit around the Sun. Secondly, it has a mass of 3.31 MJ, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while it is not explicitly stated, the fact that it has a highly eccentric orbit that takes it from within the orbit of Jupiter to beyond the orbit of Neptune suggests that it has cleared the neighbourhood around its orbit. Therefore, HR 5183 b meets all the criteria in the definition to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5629357", "name": "HD 5319 b", "article": "https://en.wikipedia.org/wiki/HD_5319_b", "description": "HD 5319 b is a gas giant exoplanet discovered in 2007 in the constellation of Cetus. This planet has a minimum mass nearly two times that of Jupiter. The planet has an almost circular orbit, with an eccentricity of only 0.02 and a period of 641 days. An additional planet in the system was discovered in 2015 and may be in a 4:3 mean motion resonance with planet b.", "actual": "positive", "rationale": "HD 5319 b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit, as indicated by its circular orbit and period of 641 days. Secondly, it has sufficient mass, as it is nearly two times the mass of Jupiter, which suggests that its self-gravity is strong enough to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, the fact that an additional planet was discovered in the system in 2015 suggests that HD 5319 b has cleared its neighbourhood around its orbit. Therefore, based on the provided definition, HD 5319 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q111723950", "name": "Nbu", "article": "https://en.wikipedia.org/wiki/Nbu", "description": "In Mandaeism, \u02bfNbu (Classical Mandaic: \u084f\u084d\u0841\u0845) or Nbu is the Mandaic name for the planet Mercury. Nbu is one of the seven planets (Classical Mandaic: \u0854\u0845\u0841\u0840, romanized: \u0161uba, lit.\u2009'The Seven'), who are part of the entourage of Ruha in the World of Darkness. This name was borrowed from the Mesopotamian god called Nabu.Nbu is associated with learning and scribes, as well as Christ and Christianity. Other names for Nbu include Maqurpiil, M\u0161iha (i.e., Jesus the Messiah), and \u02bfa\u1e6darid (of Arabic origin). Nbu's name is derived from the Akkadian Nab\u00fb.Buckley (2010) suggests a connection between Dinanukht and Nbu. For instance, in the Zrazta \u1e0f-Hibil Ziwa (Drower Collection Ms. 44), Nbu is the Lord of Book and ink and wisdom. Similarly, Dinanukht is called the \\\"ink-book of the gods\\\" in Right Ginza 6.", "actual": "positive", "rationale": "The description of Nbu clearly states that it is the Mandaic name for the planet Mercury. According to the definition provided, a planet is a celestial body that is in orbit around the Sun. Since Mercury is a known planet that orbits the Sun, it can be inferred that Nbu, being another name for Mercury, is also a planet. Furthermore, the description mentions that Nbu is one of the seven planets in Mandaeism, which aligns with the concept of a planet as defined. Therefore, based on the provided definition and the information in the description, it can be argued that Nbu is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5371571", "name": "HD 45652 b", "article": "https://en.wikipedia.org/wiki/HD_45652_b", "description": "HD 45652 b, also named Viriato, is a gas giant extrasolar planet orbiting at only 0.23 AU from the star HD 45652, with an orbital period of 44 days.  It has mass at least half that of Jupiter.  As it was detected using the radial velocity method, its true mass is dependent on the inclination of its orbit; if it is low, then the true mass will be larger.  Also, its radius is not known.  This planet was discovered by measurements taken by the ELODIE spectrograph from 2005 and 2006, and later confirmed by CORALIE and SOPHIE between 2006 and 2007.  The discovery was announced in May 2008.", "actual": "positive", "rationale": "HD 45652 b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, in this case, the star HD 45652. Secondly, it has sufficient mass, at least half that of Jupiter, which suggests that its self-gravity is likely to overcome rigid body forces, allowing it to assume a hydrostatic equilibrium shape. Lastly, while it is not explicitly stated that HD 45652 b has cleared its neighbourhood around its orbit, the fact that it was discovered and its orbit confirmed by multiple spectrographs suggests that it has a stable and clear orbit. Therefore, HD 45652 b meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1140454", "name": "HD 80606 b", "article": "https://en.wikipedia.org/wiki/HD_80606_b", "description": "HD 80606 b (also Struve 1341 Bb or HIP 45982 b) is an eccentric hot Jupiter 217 light-years from the Sun in the constellation of Ursa Major. HD 80606 b was discovered orbiting the star HD 80606 in April 2001 by a team led by Michel Mayor and Didier Queloz. With a mass 4 times that of Jupiter, it is a gas giant. Because the planet transits the host star its radius can be determined using the transit method and was found to be slightly smaller than Jupiter's. Its density is slightly less than Earth's. It has an extremely eccentric orbit like a comet, with its orbit taking it very close to its star and then back out very far away from it every 111 days.", "actual": "positive", "rationale": "HD 80606 b can be classified as a planet based on the provided definition for several reasons. Firstly, it is in orbit around a star, specifically the star HD 80606, which is similar to the requirement of a planet to be in orbit around the Sun. Secondly, it has a mass 4 times that of Jupiter, which is sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, as required by the definition. Lastly, while the description does not explicitly state that HD 80606 b has cleared its orbit, its extremely eccentric orbit and large mass suggest that it likely has the ability to clear its neighbourhood around its orbit. Therefore, based on the provided definition, HD 80606 b can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q5178221", "name": "HD 24040 b", "article": "https://en.wikipedia.org/wiki/HD_24040_b", "description": "HD 24040 b is a long-period exoplanet taking approximately 3500 days to orbit at 4.6 astronomical units in an almost circular orbit. It has a minimum mass 4 times that of Jupiter.", "actual": "positive", "rationale": "HD 24040 b can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, which is similar to the requirement of being in orbit around the Sun. Secondly, it has a minimum mass 4 times that of Jupiter, which is more than sufficient for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that it has cleared its orbit, the fact that it has a long-period orbit and a large mass suggests that it likely has the gravitational influence to clear its neighbourhood. Therefore, HD 24040 b meets all the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q849267", "name": "42 Draconis b", "article": "https://en.wikipedia.org/wiki/42_Draconis_b", "description": "42 Draconis b (abbreviated 42 Dra b), formally named Orbitar , is a candidate extrasolar planet located approximately 315 light years from Earth in the constellation of Draco. It orbits the 5th magnitude K-type giant star 42 Draconis with a period of 479 days and 38% orbital eccentricity. The planet was discovered using the radial velocity method on March 20, 2009.Following its discovery the planet was designated 42 Draconis b. In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Orbitar for this planet. The winning name was submitted by the Brevard Astronomical Society of Brevard County, Florida, United States. Orbitar is a contrived word paying homage to the space launch and orbital operations of NASA.A 2021 study found that more recent radial velocity measurements of 42 Draconis were inconsistent with the proposed planetary orbit, casting serious doubt on 42 Draconis b's existence, but with a two-planet solution still being a possibility. The study suggests that the radial velocity signal is likely caused by a yet unknown stellar phenomenon, which might be common in giant stars.", "actual": "positive", "rationale": "The description of 42 Draconis b provides evidence that it could be considered a planet based on the provided definition. Firstly, it is stated that 42 Draconis b is in orbit around a star, 42 Draconis, which is similar to the requirement of the definition that a planet is in orbit around the Sun. Secondly, while the description does not explicitly state that 42 Draconis b has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium shape, it is implied by the fact that it is referred to as a \"planet\" and was discovered using the radial velocity method, which is typically used to detect planets. Lastly, the description does not provide information about whether 42 Draconis b has cleared the neighbourhood around its orbit. However, the fact that it has a specific orbital period and eccentricity suggests that it has a stable orbit, which could imply that it has cleared its orbit of other debris. Therefore, based on the provided definition and the information in the description, there is a strong argument that 42 Draconis b could be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q89514491", "name": "HD 177565 b", "article": "https://en.wikipedia.org/wiki/HD_177565_b", "description": "HD 177565 b is an extrasolar planet orbiting the G-type main-sequence star HD 177565 55.3 light-years away from the Solar System.", "actual": "positive", "rationale": "HD 177565 b can be considered a planet based on the provided definition. It is stated that HD 177565 b is an extrasolar planet orbiting a star, which aligns with the first part of the definition that a planet is a celestial body in orbit around the Sun (or in this case, another star). While the description does not explicitly state that HD 177565 b has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape, or that it has cleared its orbit's neighbourhood, these characteristics are generally implied when an object is identified as a planet. Therefore, it is reasonable to assert that HD 177565 b is a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q419934", "name": "HD 125612 d", "article": "https://en.wikipedia.org/wiki/HD_125612_d", "description": "HD 125612 d is an extrasolar planet which orbits the G-type main sequence star HD 125612, located approximately 172 light years away in the constellation Virgo. The discovery of this planet was announced by the HARPS team on October 19, 2009, together with 31 other planets, including HD 125612 c.In 2022, the true mass and inclination of HD 125612 d were measured via astrometry.", "actual": "positive", "rationale": "The description of HD 125612 d indicates that it is a celestial body that orbits a star (HD 125612), which is similar to the requirement in the definition that a planet must be in orbit around the Sun. Although it's not explicitly stated, it can be inferred that HD 125612 d has sufficient mass to maintain a nearly round shape due to its classification as a planet. Additionally, the fact that it has a specific orbit around its star suggests that it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition, HD 125612 d can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q50358884", "name": "WASP-39b", "article": "https://en.wikipedia.org/wiki/WASP-39b", "description": "WASP-39b, officially named  Bocaprins, is a \\\"hot Jupiter\\\" extrasolar planet discovered in February 2011 by the WASP project, notable for containing a substantial amount of water in its atmosphere. In addition WASP-39b was the first exoplanet found to contain carbon dioxide in its atmosphere, and likewise for sulfur dioxide.\nWASP-39b is in the constellation Virgo, and is about 700 light-years from Earth. As part of the NameExoWorlds campaigns at the 100th anniversary of the IAU, the planet was named Bocaprins, after the beach Boca Prins in the Arikok National Park of Aruba.", "actual": "positive", "rationale": "The description of WASP-39b provides evidence that it fits the definition of a planet. Firstly, it is an extrasolar planet, which implies that it is in orbit around a star, similar to how planets in our solar system orbit the Sun. Secondly, it is described as having a substantial amount of water in its atmosphere, which suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, the fact that it was discovered and named implies that it has cleared the neighbourhood around its orbit, as this is typically a requirement for a celestial body to be classified and named as a planet. Therefore, based on the provided definition, WASP-39b can be considered a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q547497", "name": "HD 69830 b", "article": "https://en.wikipedia.org/wiki/HD_69830_b", "description": "HD 69830 b is a Neptune-mass or super-Earth-mass exoplanet orbiting the star HD 69830. It is at least 10 times more massive than Earth. It also orbits very close to its parent star and takes 82/3 days to complete an orbit.\nBased on theoretical modeling in the 2006 discovery paper, this is likely to be a rocky planet, not a gas giant. However, other work has found that if it had formed as a gas giant, it would have stayed that way, and it is now understood that planets this massive are rarely rocky.If HD 69830 b is a terrestrial planet, models predict that tidal heating would produce a heat flux at the surface of about 55 W/m2. This is 20 times that of Io.", "actual": "positive", "rationale": "HD 69830 b can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, HD 69830, which is similar to the requirement of being in orbit around the Sun. Secondly, it has a mass that is at least 10 times more than Earth's, indicating that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while it is not explicitly stated that HD 69830 b has cleared its neighbourhood around its orbit, the fact that it orbits very close to its parent star and completes an orbit in 82/3 days suggests that it likely has a clear path in its orbit. Therefore, based on the provided definition, HD 69830 b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1361687", "name": "Gliese 674 b", "article": "https://en.wikipedia.org/wiki/Gliese_674_b", "description": "Gliese 674 b is an extrasolar planet approximately 15 light years away in the constellation of Ara. This planet orbits tightly around Gliese 674. It is a sub-Neptune-or-Uranus-mass planet either gaseous or rocky. It orbits as close as 0.039 AU from the star and takes only 4.6938 days to orbit. This planet has a similar eccentricity to Mercury (e=0.2). The discovery of the planet was announced on January 7, 2007 by using the HARPS spectrograph mounted on the ESO's 3.6 meter telescope at La Silla, Chile.", "actual": "positive", "rationale": "Gliese 674 b can be considered a planet based on the provided definition. Firstly, it is a celestial body that orbits a star, in this case, Gliese 674. Secondly, it is described as either gaseous or rocky, which suggests that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Lastly, while the description does not explicitly state that Gliese 674 b has cleared its orbit's neighbourhood, its close proximity to its star and short orbital period suggest that it likely has. Therefore, Gliese 674 b meets the criteria to be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q50667", "name": "55 Cancri d", "article": "https://en.wikipedia.org/wiki/55_Cancri_d", "description": "55 Cancri d (abbreviated 55 Cnc d), formally named Lipperhey , is an extrasolar planet in a long-period orbit around the Sun-like star 55 Cancri A. Located at a similar distance from its star as Jupiter is from the Sun, it is the fifth and outermost known planet in its planetary system. 55 Cancri d was discovered on June 13, 2002.", "actual": "positive", "rationale": "The description of 55 Cancri d aligns with the definition of a planet in several ways. Firstly, it is stated that 55 Cancri d is in orbit around a Sun-like star, 55 Cancri A, which satisfies the first condition of the definition that a planet must be in orbit around the Sun. Although it's not directly stated, we can infer that 55 Cancri d has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, as it is referred to as a planet and this is a characteristic of planets. Lastly, it is mentioned that 55 Cancri d is the fifth and outermost known planet in its planetary system, which suggests that it has cleared the neighbourhood around its orbit, meeting the third condition of the definition. Therefore, based on the provided definition, 55 Cancri d can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q1204153", "name": "Kepler-8b", "article": "https://en.wikipedia.org/wiki/Kepler-8b", "description": "Kepler-8b is the fifth of the first five exoplanets discovered by NASA's Kepler spacecraft, which aims to discover planets in a region of the sky between the constellations Lyra and Cygnus that transit (cross in front of) their host stars. The planet is the hottest of the five. Kepler-8b was the only planet discovered in Kepler-8's orbit, and is larger (though more diffuse) than Jupiter. It orbits its host star every 3.5 days. The planet also demonstrates the Rossiter\u2013McLaughlin effect, where the planet's orbit affects the redshifting of the spectrum of the host star. Kepler-8b was announced to the public on January 4, 2010 at a conference in Washington, D.C. after radial velocity measurements conducted at the W.M. Keck Observatory confirmed its detection by Kepler.", "actual": "positive", "rationale": "Kepler-8b can be considered a planet based on the provided definition. Firstly, it is in orbit around a star, as it orbits its host star every 3.5 days. Secondly, it has sufficient mass to assume a nearly round shape, as it is larger than Jupiter, indicating that its self-gravity has overcome rigid body forces. Lastly, it has cleared the neighbourhood around its orbit, as it was the only planet discovered in Kepler-8's orbit. Therefore, Kepler-8b meets all the criteria in the definition of a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q86686508", "name": "Kepler-1658b", "article": "https://en.wikipedia.org/wiki/Kepler-1658b", "description": "Kepler-1658b (or the Kepler object of interest, KOI-4.01) is a hot Jupiter, a type of gas giant exoplanet, that orbits an F-type star called Kepler 1658, located about 2629 light-years away from the Solar System. It is the first planet identified by the Kepler space telescope after its launch in 2009, but later ruled out as false alarm since its transit could not be confirmed. A study published in 2019 established it as a planet, describing it as \\\"the closest known planet in terms of orbital period to an evolved star.\\\" Analysis of the Transiting Exoplanet Survey Satellite (TESS) data in 2022 showed that it is gradually spiraling into its star.", "actual": "positive", "rationale": "Kepler-1658b can be considered a planet based on the provided definition. Firstly, it is a celestial body that is in orbit around a star, in this case, the F-type star Kepler 1658. This satisfies the first condition of the definition. Secondly, it is described as a gas giant exoplanet, which implies that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, meeting the second condition. Lastly, while the description does not explicitly state that Kepler-1658b has cleared its orbit's neighbourhood, the fact that it is gradually spiraling into its star suggests that it is the dominant gravitational body in its orbit, which aligns with the third condition of the definition. Therefore, based on the provided definition, Kepler-1658b can be classified as a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q222246", "name": "2MASS J03552337+1133437", "article": "https://en.wikipedia.org/wiki/2MASS_J03552337%2B1133437", "description": "2MASS J03552337+1133437 (2MASS J0355+11) is a nearby brown dwarf of spectral type L5\u03b3, located in constellation Taurus at approximately 29.8 light-years from Earth.", "actual": "positive", "rationale": "The given definition cannot support the assertion that 2MASS J03552337+1133437 is a planet. The description of 2MASS J03552337+1133437 identifies it as a brown dwarf, not a planet. Furthermore, the definition requires a planet to be in orbit around the Sun, and there is no information provided that 2MASS J03552337+1133437 orbits the Sun. Therefore, based on the provided definition and information, we cannot argue that 2MASS J03552337+1133437 is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q5281813", "name": "Discoverer 29", "article": "https://en.wikipedia.org/wiki/Discoverer_29", "description": "Discoverer 29, also known as Corona 9023, was an American optical reconnaissance satellite which was launched in 1961. It was the first KH-3 Corona''' satellite, which was based on an Agena-B rocket.The launch of Discoverer 29 occurred at 20:00 UTC on 30 August 1961. A Thor DM-21 Agena-B rocket was used, flying from Launch Complex 75-3-4 at the Vandenberg Air Force Base. Upon successfully reaching orbit, it was assigned the Harvard designation 1961 Psi 1.\nDiscoverer 29 was operated in a low Earth orbit, with a perigee of 138 kilometres (86 mi), an apogee of 511 kilometres (318 mi), 82 degrees of inclination, and a period of 91 minutes. The satellite had a mass of 1,150 kilograms (2,540 lb), and was equipped with a panoramic camera with a focal length of 61 centimetres (24 in), which had a maximum resolution of 7.6 metres (25 ft). Images were recorded onto 70-millimeter (2.8 in) film, and returned in a Satellite Recovery Vehicle two days after launch, but all of the images returned were found to be out of focus. The Satellite Recovery Vehicle used by Discoverer 29 was SRV-554. Once its images had been returned, Discoverer 29 remained in orbit until it decayed on 9 September 1961.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that Discoverer 29 is a planet. The definition states that a planet is a celestial body that orbits the Sun, has sufficient mass to assume a nearly round shape due to its self-gravity, and has cleared the neighbourhood around its orbit. \n\nDiscoverer 29, on the other hand, is described as an artificial satellite launched by the United States in 1961. It was operated in a low Earth orbit, not around the Sun. It was not naturally formed, but man-made, and there is no information suggesting that it has sufficient mass to overcome rigid body forces to assume a hydrostatic equilibrium shape. Furthermore, there is no indication that it has cleared the neighbourhood around its orbit. Therefore, Discoverer 29 does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q54347", "name": "RazakSAT", "article": "https://en.wikipedia.org/wiki/RazakSAT", "description": "RazakSAT is a Malaysian Earth observation satellite carrying a high-resolution camera. It was launched into low Earth orbit on 14 July 2009. It was placed in a near-equatorial orbit that presents many imaging opportunities for the equatorial region. It weighs over three times as much as TiungSAT-1 and carries a high-resolution Earth observation camera. Developed in conjunction with the Satrec Initiative, the satellite's low inclination (9 degrees) brought it over Malaysia a dozen or more times per day. This was intended to provide greatly increased coverage of Malaysia compared to most other Earth observation satellites. An audit report released in October 2011 revealed that the satellite had failed after one year of operation.RazakSAT was the only operational satellite to be put into orbit by SpaceX's Falcon 1.", "actual": "negative", "rationale": "Based on the provided definition and information, there is no valid argument to assert that RazakSAT is a planet. The definition of a planet states that it must be in orbit around the Sun, have sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. RazakSAT, however, is a man-made satellite that orbits the Earth, not the Sun. It does not have sufficient mass to overcome rigid body forces to assume a hydrostatic equilibrium shape, nor has it cleared the neighbourhood around its orbit. Therefore, RazakSAT does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1166037", "name": "Explorer 15", "article": "https://en.wikipedia.org/wiki/Explorer_15", "description": "Explorer 15, also called EPE-C or Energetic Particles Explorer-C, was a NASA satellite launched as part of the Explorer program. Explorer 15 was launched on 27 October 1962, at Cape Canaveral Air Force Station, Florida, United States, with a Thor-Delta A .", "actual": "negative", "rationale": "Based on the provided definition and information, it is not possible to argue that Explorer 15 is a planet. The definition of a planet states that it must be in orbit around the Sun, have sufficient mass to overcome rigid body forces and assume a nearly round shape, and have cleared the neighbourhood around its orbit. Explorer 15, however, is described as a satellite launched by NASA. There is no information suggesting that it meets any of the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q60760723", "name": "JY1-SAT", "article": "https://en.wikipedia.org/wiki/JY1-SAT", "description": "JY1-SAT is a cubesat that is Jordan's first satellite. It was launched aboard SpaceX's Falcon 9 from the Vandenberg Air Force Base in the United States on 3 December 2018. It is named in tribute of the late King Hussein who was an amateur ham radio operator; his callsign was \\\"JY1\\\". The project was built by Jordanian students from various universities, and was funded by Jordan's Crown Prince Foundation.", "actual": "negative", "rationale": "The assertion that JY1-SAT is a planet cannot be supported based on the provided definition. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to assume a hydrostatic equilibrium shape, and has cleared the neighbourhood around its orbit. The description of JY1-SAT does not provide any information that it meets these criteria. It is described as a cubesat, a type of miniaturized satellite for space research, and not a celestial body with sufficient mass to assume a hydrostatic equilibrium shape. Furthermore, there is no information suggesting that JY1-SAT has cleared the neighbourhood around its orbit. Therefore, based on the provided definition and information, JY1-SAT cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q69165", "name": "ChinaSat 12", "article": "https://en.wikipedia.org/wiki/ChinaSat_12", "description": "The ChinaSat 12 (Chinese: \u4e2d\u661f12\u53f7; pinyin: Zh\u014dngx\u012bng 12) communications satellite is wholly owned by China Satellite Communications, with part of its communications payload leased or rented by SupremeSAT, a Sri Lankan company, to be marketed to potential users as SupremeSAT-I. Once operational, it will provide communications services for the China, Sri Lanka, East Asia, South Asia, Middle East, Africa, Australia, and China sea area, the Indian Ocean region.ChinaSat 12 was also known as Apstar 7B (as a backup of Apstar 7), but acquired by China Satellite Communications from its subsidiary APT Satellite Holdings in 2010. However, APT Satellite Holdings was contracted by its parent company as the operator of ChinaSat 12.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that ChinaSat 12 is a planet. The definition of a planet states that it must be a celestial body in orbit around the Sun, have sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nChinaSat 12, however, is a communications satellite, not a celestial body. It orbits the Earth, not the Sun. It does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. It also does not have the ability to clear the neighbourhood around its orbit. Therefore, based on the provided definition, ChinaSat 12 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q211655", "name": "2008 TC3", "article": "https://en.wikipedia.org/wiki/2008_TC3", "description": "2008 TC3 (Catalina Sky Survey temporary designation 8TA9D69) was an 80-tonne (80-long-ton; 90-short-ton), 4.1-meter (13 ft) diameter asteroid that entered Earth's atmosphere on October 7, 2008. It exploded at an estimated 37 kilometers (23 mi) above the Nubian Desert in Sudan. Some 600 meteorites, weighing a total of 10.5 kilograms (23.1 lb), were recovered; many of these belonged to a rare type known as ureilites, which contain, among other minerals, nanodiamonds.It was the first time that an asteroid impact had been predicted before its entry into the atmosphere as a meteor.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 2008 TC3 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. The description of 2008 TC3 does not provide information that it meets any of these criteria. It is described as an asteroid, not a planet, and it entered Earth's atmosphere and exploded, indicating that it did not have a stable orbit around the Sun. Furthermore, there is no information about its mass being sufficient to overcome rigid body forces and assume a nearly round shape, or about it having cleared the neighbourhood around its orbit. Therefore, based on the provided definition and information, 2008 TC3 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4537552", "name": "Yamal 201", "article": "https://en.wikipedia.org/wiki/Yamal_201", "description": "Yamal-201 (Russian: \u042f\u043c\u0430\u043b-201) was a geostationary communications satellite operated by Gazprom Space Systems and built by RSC Energia. It was, along with Yamal-202 the second dual launch of the Yamal programme and the second iteration of the USP Bus. It was a 1,360 kg (3,000 lb) satellite with 4,080 watts of power (3.4 kW at end of life) on an unpressurized bus. It had eight SPT-70 electric thrusters by OKB Fakel for station keeping. Its payload was 9 C-band and 6 Ku-band transponders supplied by Space Systems/Loral.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Yamal 201 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nThe description of Yamal 201 does not provide any information that would suggest it meets these criteria. It is described as a geostationary communications satellite, not a celestial body in orbit around the Sun. There is no information to suggest that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a nearly round shape, or that it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition and information, Yamal 201 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q137248", "name": "1240 Centenaria", "article": "https://en.wikipedia.org/wiki/1240_Centenaria", "description": "1240 Centenaria, provisional designation 1932 CD, is a background asteroid from the outer regions of the asteroid belt, approximately 60 kilometers (37 miles) in diameter. It was discovered on 5 February 1932, by astronomer Richard Schorr at the Bergedorf Observatory in Hamburg, Germany. The assumed C-type asteroid has a rotation period of 11.3 hours. It was named for the 100th anniversary of the discovering observatory.", "actual": "negative", "rationale": "Based on the provided definition, it is difficult to argue that 1240 Centenaria is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nWhile 1240 Centenaria is in orbit around the Sun and may have a nearly round shape due to its self-gravity, there is no information provided that suggests it has cleared the neighbourhood around its orbit, which is a key characteristic of a planet. Furthermore, it is specifically identified as an asteroid, which is typically smaller than a planet and does not meet all the criteria of being a planet. Therefore, based on the provided definition and information, it is not possible to argue that 1240 Centenaria is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4553351", "name": "178P/Hug\u2013Bell", "article": "https://en.wikipedia.org/wiki/178P/Hug%E2%80%93Bell", "description": "178P/Hug\u2013Bell is a periodic comet in the Solar System. It was discovered by Northeast Kansas Amateur Astronomers' League members Gary Hug and Graham Bell and is thought to be the first periodic comet to be discovered by amateurs. It was declared a comet less than two days after its initial discovery, after having its course confirmed on previous images.Hug-Bell's orbital period is about seven years; its orbit is eccentric, though less so than many comets. Hug-Bell's orbit lies entirely outside the orbit of Mars, but at its aphelion overlaps in solar distance with the orbit of Jupiter. Because it never comes closer to the Sun than about 2 AU, it is never expected to be a very bright comet, with a typical perihelion magnitude of 18-19.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 178P/Hug\u2013Bell is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass to assume a nearly round shape, and has cleared the neighbourhood around its orbit. The description of 178P/Hug\u2013Bell identifies it as a comet, not a planet. It does not provide information about its shape or whether it has cleared its orbit. Therefore, using only the information provided, we cannot assert that 178P/Hug\u2013Bell is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q956514", "name": "3714 Kenrussell", "article": "https://en.wikipedia.org/wiki/3714_Kenrussell", "description": "3714 Kenrussell, provisional designation 1983 TT1, is a Eunomian asteroid from the central regions of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. It was discovered on 12 October 1983, by American astronomer Edward Bowell at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. It was named for Australian astronomer Kenneth S. Russell. The presumably stony asteroid has a rotation period of 5.25 hours.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 3714 Kenrussell is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass to assume a hydrostatic equilibrium shape, and has cleared the neighbourhood around its orbit. While 3714 Kenrussell is in orbit around the Sun and may have a nearly round shape, there is no information provided that it has cleared the neighbourhood around its orbit. Furthermore, it is described as an asteroid, which typically do not meet all the criteria to be classified as a planet. Therefore, based on the provided information and definition, 3714 Kenrussell cannot be argued to be a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q116674440", "name": "S/2021 J 2", "article": "https://en.wikipedia.org/wiki/S/2021_J_2", "description": "S/2021 J 2 is a small outer natural satellite of Jupiter discovered by Scott S. Sheppard on 12 August 2021, using the 6.5-meter Magellan-Baade Telescope at Las Campanas Observatory, Chile. It was announced by the Minor Planet Center on 19 January 2023, after observations were collected over a long enough time span to confirm the satellite's orbit.S/2021 J 2 is part of the Ananke group, a cluster of retrograde irregular moons of Jupiter that follow similar orbits to Ananke at semi-major axes between 19\u201322 million km (12\u201314 million mi), orbital eccentricities between 0.1\u20130.4, and inclinations between 139\u2013155\u00b0. It has a diameter of about 1 km (0.62 mi) for an absolute magnitude of 17.3, making it one of Jupiter's smallest known moons.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that S/2021 J 2 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass to assume a hydrostatic equilibrium shape, and has cleared the neighbourhood around its orbit. However, the description of S/2021 J 2 indicates that it is a natural satellite of Jupiter, not a body in direct orbit around the Sun. Furthermore, there is no information provided about its mass or whether it has cleared the neighbourhood around its orbit. Therefore, based on the given definition and information, S/2021 J 2 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q28845773", "name": "OV1-4", "article": "https://en.wikipedia.org/wiki/OV1-4", "description": "Orbiting Vehicle 1-4 (also known as OV1-4), launched 30 Mar 1966, was the fourth, and second successful, satellite in the OV1 series of the United States Air Force's Orbiting Vehicle program. OV1-4 was a long-term bioscience and materials science satellite, designed to return data relevant to long-term human presence in space. Its launch marked the first time two satellites (the other being OV1-5) were placed into orbit side by side with each other.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that OV1-4 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. The description of OV1-4 does not provide any information that would suggest it meets these criteria. It is described as a satellite, not a celestial body, and there is no information about its mass, shape, or whether it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition and information, OV1-4 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q22084830", "name": "Near-Earth Asteroid Scout", "article": "https://en.wikipedia.org/wiki/Near-Earth_Asteroid_Scout", "description": "The Near-Earth Asteroid Scout (NEA Scout) was a mission by NASA to develop a controllable low-cost CubeSat solar sail spacecraft capable of encountering near-Earth asteroids (NEA). NEA Scout was one of ten CubeSats launched into a heliocentric orbit on Artemis 1, the maiden flight of the Space Launch System, on 16 November 2022.The target for the mission was asteroid 2020 GE, but this could have changed based on launch date or other factors. After deployment, NEA Scout was to perform a series of lunar flybys to achieve optimum departure trajectory before beginning its two-year-long cruise.\nNo contact was ever made, and the mission was lost.", "actual": "negative", "rationale": "The assertion that the Near-Earth Asteroid Scout is a planet cannot be supported by the given definition. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to assume a hydrostatic equilibrium shape, and has cleared its neighbourhood around its orbit. The Near-Earth Asteroid Scout, as described, is a spacecraft developed by NASA, not a celestial body. It does not have its own orbit around the Sun, nor does it have sufficient mass to assume a hydrostatic equilibrium shape. Furthermore, it does not have the ability to clear its neighbourhood around its orbit. Therefore, based on the given definition, the Near-Earth Asteroid Scout cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q114646", "name": "696 Leonora", "article": "https://en.wikipedia.org/wiki/696_Leonora", "description": "696 Leonora is a Meliboean asteroid orbiting the Sun in the asteroid belt. It was discovered 10 January 1910 by American astronomer Joel Hastings Metcalf, at Taunton, Massachusetts. It was named by Arthur Snow of the United States Naval Observatory, who computed the orbit for the planet, after his wife, Mary Leonora Snow.", "actual": "negative", "rationale": "The assertion that 696 Leonora is a planet cannot be supported based on the provided definition and information. While 696 Leonora is a celestial body in orbit around the Sun, there is no information given that it has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Furthermore, there is no information provided that it has cleared the neighbourhood around its orbit. Therefore, based on the given definition of a planet, we cannot assert that 696 Leonora is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1227405", "name": "T11 (satellite)", "article": "https://en.wikipedia.org/wiki/T11_(satellite)", "description": "T11, formerly known as DirecTV-11, is a Boeing model 702 satellite built by the Boeing Satellite Development Center. Its current name was adopted in 2017.", "actual": "negative", "rationale": "The assertion that T11 (satellite) is a planet cannot be supported by the provided definition and information. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to assume a nearly round shape due to its self-gravity, and has cleared its orbit's neighbourhood. The description of T11 does not provide any information that it meets these criteria. It is a man-made satellite built by Boeing, not a natural celestial body, and there is no information about its orbit around the Sun, its mass, or its ability to clear its orbit's neighbourhood. Therefore, based on the provided definition and information, T11 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q16061296", "name": "Eutelsat I F-2", "article": "https://en.wikipedia.org/wiki/Eutelsat_I_F-2", "description": "Eutelsat I F-2, also known as European Communications Satellite 2 (ECS-2) is a decommissioned communications satellite operated by the European Telecommunications Satellite Organisation (Eutelsat). Launched in 1984, it was operated in geostationary orbit at a longitude of 7\u00b0 East, before moving to several other locations later in its operational life, before it was finally decommissioned in 1993. It was the second of five satellites launched to form the first-generation Eutelsat constellation.", "actual": "negative", "rationale": "The assertion that Eutelsat I F-2 is a planet cannot be supported based on the provided definition. While Eutelsat I F-2 is in orbit around the Sun, it does not meet the other two criteria for being a planet. It does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium (nearly round) shape. It is a man-made object and not a naturally occurring celestial body. Furthermore, it has not cleared the neighbourhood around its orbit. It was part of a constellation of satellites, indicating that it shared its orbit with other objects. Therefore, Eutelsat I F-2 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q539769", "name": "SCORE (satellite)", "article": "https://en.wikipedia.org/wiki/SCORE_(satellite)", "description": "SCORE (Signal Communications by Orbiting Relay Equipment) was the world's first purpose-built communications satellite. Launched aboard an American Atlas rocket on December 18, 1958, SCORE provided the second test of a communications relay system in space (the first having been provided by the USAF/NASA's Pioneer 1), the first broadcast of a human voice from space, and the first successful use of the Atlas as a launch vehicle. It captured world attention by broadcasting a Christmas message via shortwave radio from U.S. President Dwight D. Eisenhower through an on-board tape recorder. The satellite was popularly dubbed \\\"The Talking Atlas\\\". SCORE, as a geopolitical strategy, placed the United States at an even technological par with the Soviet Union as a highly functional response to the Sputnik 1 and Sputnik 2 satellites.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that SCORE (satellite) is a planet. The definition of a planet states that it must be in orbit around the Sun, have sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. The description of SCORE does not provide any information that would suggest it meets these criteria. It is described as a communications satellite, not a celestial body with its own orbit around the Sun. Furthermore, there is no information to suggest that SCORE has sufficient mass to overcome rigid body forces and assume a nearly round shape, or that it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition and information, SCORE cannot be considered a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q6433287", "name": "Kosmos 2478", "article": "https://en.wikipedia.org/wiki/Kosmos_2478", "description": "Kosmos 2478 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 2478 meaning Cosmos 2478) is a  Russian military satellite launched in 2011 as part of the GLONASS satellite navigation system.\nThis satellite is a GLONASS-M satellite, also known as Uragan-M, and is numbered Uragan-M No. 746.Kosmos 2478 was launched from Site 43/4  at Plesetsk Cosmodrome in northern Russia. A Soyuz-2-1b carrier rocket with a Fregat upper stage was used to perform the launch which took place at 08:26 UTC on 28 November 2011. The launch successfully placed the satellite into Medium Earth orbit. It subsequently received its Kosmos designation, and the international designator 2011\u2013071. The United States Space Command assigned it the Satellite Catalog Number 37938.It is in the third orbital plane used by GLONASS, in orbital slot 17.It started operations on 23 December 2011.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 2478 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nKosmos 2478, however, is a man-made satellite launched by Russia as part of the GLONASS satellite navigation system. It is in Medium Earth orbit, not orbiting the Sun. It does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. It also has not cleared the neighbourhood around its orbit. Therefore, Kosmos 2478 does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2521638", "name": "ViaSat-1", "article": "https://en.wikipedia.org/wiki/ViaSat-1", "description": "ViaSat-1 is a high throughput communications satellite owned by  Viasat Inc. and Telesat Canada. Launched October 19, 2011 aboard a Proton rocket, it held the Guinness record for the world's highest capacity communications satellite with a total capacity in excess of 140 Gbit/s, more than all the satellites covering North America combined, at the time of its launch.ViaSat-1 is capable of two-way communications with small dish antennas at higher speeds and a lower cost-per-bit than any satellite before.The satellite is positioned at 115.1 degrees West longitude geostationary orbit point, with 72 Ka-band spot beams; 63 over the U.S. (Eastern and Western states, Alaska and Hawaii), and nine over Canada.\nThe Canadian beams are owned by satellite operator Telesat and are used for the Xplornet broadband service to consumers in rural Canada. The US beams provide fast Internet access called Exede, Viasat's satellite Internet service.ViaSat-1 is part of a new satellite system architecture created by Viasat Inc. The objective is to create a better satellite broadband user experience, making satellite competitive with DSL and wireless broadband alternatives for the first time.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that ViaSat-1 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nViaSat-1, however, is a communications satellite. While it is in orbit, it is not around the Sun but around the Earth. It does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. It is not nearly round but is built in a specific shape for its purpose as a satellite. Furthermore, it has not cleared the neighbourhood around its orbit. Therefore, ViaSat-1 does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q7865651", "name": "USA-132", "article": "https://en.wikipedia.org/wiki/USA-132", "description": "USA-132, also known as GPS IIR-2 and GPS SVN-43, is an American navigation satellite which forms part of the Global Positioning System. It was the second Block IIR GPS satellite to be launched, out of thirteen in the original configuration, and twenty one overall. GPS IIR-1 failed to achieve orbit, so USA-132 was the first successful Block IIR satellite. It was built by Lockheed Martin, using the AS-4000 satellite bus.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that USA-132 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nUSA-132, however, is described as a navigation satellite that forms part of the Global Positioning System. It is not mentioned that it orbits the Sun, has sufficient mass for its self-gravity to overcome rigid body forces to assume a nearly round shape, or that it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition and information, USA-132 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4649953", "name": "AAUSat-3", "article": "https://en.wikipedia.org/wiki/AAUSat-3", "description": "AAUSat-3,  (Aalborg University CubeSat-3), is the third CubeSat built and operated by students from the Aalborg University in Denmark. It was launched on 25 February 2013 from the Satish Dhawan Space Centre in India on a Polar Satellite Launch Vehicle (PSLV) launch vehicle (PSLV-C20). AAUSat-3 carries two Automatic Identification System (AIS-1 and AIS-2) receivers as the main payload.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that AAUSat-3 is a planet. The definition of a planet requires that the celestial body is in orbit around the Sun, has sufficient mass to assume a nearly round shape due to its self-gravity, and has cleared the neighbourhood around its orbit. AAUSat-3, however, is a CubeSat, a type of miniaturized satellite for space research, and does not meet any of the criteria specified in the definition of a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1612589", "name": "Communications Technology Satellite", "article": "https://en.wikipedia.org/wiki/Communications_Technology_Satellite", "description": "The Communications Technology Satellite (CTS), known as Hermes, was an experimental high-power direct broadcast communications satellite. It was a joint effort of Canadian Department of Communications, who designed and built the satellite, NASA who tested, launched and operated the satellite, and European Space Agency (ESA) who provided the 1200 watts solar panels and other devices. The three agencies shared the satellite and the data from the experiments.\nAlthough the launch of the ATS-6 spacecraft in 1974 marked the end of NASA's program of experimental communications satellites. NASA participated in a Canadian satellite venture known initially as \\\"Cooperative Applications Satellite-C\\\" and renamed Hermes. This joint effort involved NASA and the Canadian Department of Communications. NASA's Lewis Research Center provided the satellite's high-power communications payload. Canada designed and built the spacecraft; NASA tested, launched, and operated it. Also, the European Space Agency provided one of the low-power traveling-wave tubes and other equipment. Hermes was launched 17 January 1976 and operated until October 1979.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that the Communications Technology Satellite is a planet. The Communications Technology Satellite does not meet any of the criteria outlined in the definition of a planet. It does not orbit the Sun, it does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape, and it has not cleared the neighbourhood around its orbit. Instead, it is a man-made object designed for a specific purpose, namely communication. Therefore, it cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153548", "name": "432 Pythia", "article": "https://en.wikipedia.org/wiki/432_Pythia", "description": "Pythia (minor planet designation: 432 Pythia) is a typical Main belt asteroid.\nIt was discovered by Auguste Charlois on 18 December 1897 in Nice.", "actual": "negative", "rationale": "The given definition cannot be used to argue that 432 Pythia is a planet. The description of 432 Pythia only states that it is a Main belt asteroid, and does not provide any information about whether it meets the criteria specified in the definition of a planet. Specifically, it does not state whether 432 Pythia is in orbit around the Sun, whether it has sufficient mass to assume a hydrostatic equilibrium shape, or whether it has cleared the neighbourhood around its orbit. Therefore, based on the given information, it cannot be argued that 432 Pythia is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4181082", "name": "Great Comet of 1819", "article": "https://en.wikipedia.org/wiki/Great_Comet_of_1819", "description": "The Great Comet of 1819, officially designated as C/1819 N1, also known as Comet Tralles, was an exceptionally bright and easily visible comet, approaching an apparent magnitude of 1\u20132, discovered July 1, 1819 by the German astronomer Johann Georg Tralles in Berlin. It was the first comet analyzed using polarimetry, by French mathematician Fran\u00e7ois Arago.", "actual": "negative", "rationale": "The rationale cannot be provided as the Great Comet of 1819 does not fit the definition of a planet. According to the provided definition, a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. The Great Comet of 1819, however, is a comet, not a planet. It does not have sufficient mass to assume a hydrostatic equilibrium shape, nor has it cleared the neighbourhood around its orbit. Therefore, it cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q376628", "name": "CHEOPS", "article": "https://en.wikipedia.org/wiki/CHEOPS", "description": "CHEOPS (CHaracterising ExOPlanets Satellite) is a European space telescope. Its objective is to determine the size of known extrasolar planets, which will allow the estimation of their mass, density, composition and their formation. Launched on 18 December 2019, it is the first Small-class mission in ESA's Cosmic Vision science programme.The small satellite features an optical Ritchey-Chr\u00e9tien telescope with an aperture of 30 cm, mounted on a standard small satellite platform. It was placed into a Sun-synchronous orbit of about 700 km altitude.", "actual": "negative", "rationale": "The assertion that CHEOPS is a planet cannot be supported by the given definition and information. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to maintain a nearly round shape due to its self-gravity, and has cleared its orbit's neighbourhood. However, the description of CHEOPS indicates that it is a space telescope launched by the European Space Agency, not a celestial body. It orbits the Earth, not the Sun, and its purpose is to study extrasolar planets, not to act as a planet itself. Therefore, based on the provided definition and information, CHEOPS cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q17285875", "name": "Hodoyoshi 3", "article": "https://en.wikipedia.org/wiki/Hodoyoshi_3", "description": "Hodoyoshi-3 is a Japanese micro-satellite launched in 2014. The satellite is built in 0.5x0.5x0.65m box-shape bus, optimized for piggy-back launch.\nAll instruments are powered by solar cells mounted on the spacecraft body and two stub wings, with estimated electrical power of 50W. For orbit-keeping, a hydrogen peroxide thruster is used. The satellite was developed under the Funding Program for World-Leading Innovation R&D on Science and Technology.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Hodoyoshi 3 is a planet. While it is in orbit around the Sun, it does not meet the other two criteria. It does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. It is built in a box-shape, which is not nearly round. Additionally, there is no information to suggest that it has cleared the neighbourhood around its orbit. Therefore, Hodoyoshi 3 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q55624488", "name": "NOAA-14", "article": "https://en.wikipedia.org/wiki/NOAA-14", "description": "NOAA-14, also known as NOAA-J before launch, was an American weather satellite operated by the National Oceanic and Atmospheric Administration (NOAA). NOAA-14 continued the third-generation operational, Polar Orbiting Environmental Satellite (POES) series operated by the National Environmental Satellite Service (NESS) of the National Oceanic and Atmospheric Administration (NOAA). NOAA-14 continued the series of Advanced TIROS-N (ATN) spacecraft begun with the launch of NOAA-8 (NOAA-E) in 1983.", "actual": "negative", "rationale": "Based on the provided definition and description, it is not possible to argue that NOAA-14 is a planet. The definition of a planet states that it must be in orbit around the Sun, have sufficient mass to assume a hydrostatic equilibrium shape, and have cleared the neighbourhood around its orbit. The description of NOAA-14 does not provide any information that would suggest it meets these criteria. Instead, it is described as a weather satellite operated by NOAA, which implies it is a man-made object rather than a natural celestial body. Therefore, using the provided definition and description, NOAA-14 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q18239", "name": "Loge (moon)", "article": "https://en.wikipedia.org/wiki/Loge_(moon)", "description": "Loge or Saturn XLVI is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on 26 June 2006, from observations taken between January and April 2006.\nLoge is about 6 kilometres in diameter, and orbits Saturn at an average distance of 23,142,000 km in 1314.364 days, at an inclination of 166.5\u00b0 to the ecliptic (165.3\u00b0 to Saturn's equator), in a retrograde direction and with an eccentricity of 0.1390. It has a tentative rotation period of about 6.9\u00b10.1 hours, but this is highly uncertain as the light curve is the shallowest among all the irregular moons studied by Cassini\u2013Huygens (amplitude about 0.07 magnitudes).It was named in April 2007, after Logi, a fire giant from Norse mythology.", "actual": "negative", "rationale": "The assertion that Loge (moon) is a planet cannot be supported by the given definition of a planet. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to assume a nearly round shape due to its self-gravity, and has cleared the neighbourhood around its orbit. However, the description of Loge indicates that it is a natural satellite of Saturn, meaning it orbits Saturn, not the Sun. Therefore, it does not meet the first criterion of the definition. The description does not provide information about Loge's shape or whether it has cleared its orbit, so we cannot determine if it meets the other two criteria. Therefore, based on the given definition and information, Loge cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q63853", "name": "1509 Esclangona", "article": "https://en.wikipedia.org/wiki/1509_Esclangona", "description": "1509 Esclangona, provisional designation 1938 YG, is a rare-type Hungaria asteroid and binary system from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It is named after French astronomer Ernest Esclangon.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 1509 Esclangona is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass to assume a hydrostatic equilibrium shape, and has cleared the neighbourhood around its orbit. The description of 1509 Esclangona does not provide information to confirm that it meets all these criteria. It is mentioned that 1509 Esclangona is an asteroid and a binary system from the inner regions of the asteroid belt, but there is no information about its shape, its mass, or whether it has cleared its orbit. Therefore, based on the provided information, we cannot assert that 1509 Esclangona is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153870", "name": "4383 Suruga", "article": "https://en.wikipedia.org/wiki/4383_Suruga", "description": "4383 Suruga, provisional designation 1989 XP, is a Vestian asteroid and binary system from the inner regions of the asteroid belt, approximately 6.5 kilometers in diameter. It was discovered on 1 December 1989, by Japanese astronomer Yoshiaki Oshima at Gekko Observatory, Japan. The asteroid was named after the former Japanese Suruga Province. Its synchronous minor-planet moon, S/2013 (4383) 1, measures approximately 1.33 kilometers and has a period of 16.386 hours.", "actual": "negative", "rationale": "The assertion that 4383 Suruga is a planet cannot be supported based on the provided definition and information. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to assume a nearly round shape due to its self-gravity, and has cleared the neighbourhood around its orbit. While 4383 Suruga does orbit the Sun and may have a nearly round shape due to its self-gravity, there is no information provided that suggests it has cleared the neighbourhood around its orbit. In fact, it is described as being from the inner regions of the asteroid belt, which implies that it is surrounded by other celestial bodies. Therefore, based on the provided definition and information, 4383 Suruga cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q211473", "name": "(613100) 2005 TN74", "article": "https://en.wikipedia.org/wiki/(613100)_2005_TN74", "description": "(613100) 2005 TN74 (also written 2005 TN74) is a trans-Neptunian object (TNO) in a 3:5 resonance with Neptune. It was discovered by Scott S. Sheppard and Chadwick A. Trujillo in 2005.\nIt was initially suspected of being a Neptune trojan since the first observations gave it a semi-major axis of 30 AU and an orbital eccentricity of 0.16, but further observations showed it to have a semi-major axis of 42.7 AU, a perihelion of 32.1 AU, and an aphelion of 53.4 AU.With an absolute magnitude of 7.2, it has an expected diameter in the range of 85 to 240 km.It has been observed 19 times over four oppositions.", "actual": "negative", "rationale": "Based on the provided definition, it is difficult to definitively assert that (613100) 2005 TN74 is a planet. While it is a celestial body in orbit around the Sun, the information provided does not confirm whether it has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape. Furthermore, there is no information to suggest that it has cleared the neighbourhood around its orbit. Therefore, without additional information, it cannot be definitively classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q136761", "name": "1173 Anchises", "article": "https://en.wikipedia.org/wiki/1173_Anchises", "description": "1173 Anchises  is an unusually elongated Jupiter Trojan from the Trojan camp, approximately 124 kilometers (77 miles) in diameter. It was discovered on 17 October 1930, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany, and was the 9th such body to be discovered.:\u200a2\u200a The primitive P-type asteroid belongs to the largest Jupiter trojans, has an unusually smooth surface texture, the lowest spectral slope of all members of the Trojan camp, and a rotation period of 11.6 hours. It was named after Anchises from Greek mythology.", "actual": "negative", "rationale": "Based on the provided definition, it is difficult to argue that 1173 Anchises is a planet. While it is a celestial body in orbit around the Sun, there is no information given that it has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape. Additionally, there is no information provided that it has cleared the neighbourhood around its orbit. Therefore, based on the provided definition and information, it cannot be definitively argued that 1173 Anchises is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q4044978", "name": "NOAA-16", "article": "https://en.wikipedia.org/wiki/NOAA-16", "description": "NOAA-16, also known as NOAA-L before launch, was an operational, polar orbiting, weather satellite series (NOAA K-N) operated by the National Environmental Satellite Service (NESS) of the National Oceanic and Atmospheric Administration (NOAA). NOAA-16 continued the series of Advanced TIROS-N (ATN) spacecraft that began with the launch of NOAA-8 (NOAA-E) in 1983; but it had additional new and improved instrumentation over the NOAA A-K series and a new launch vehicle (Titan 23G). It was launched on 21 September 2000 and, following an unknown anomaly, it was decommissioned on 9 June 2014. In November of 2015 it broke up in orbit, creating more than 200 pieces of debris.", "actual": "negative", "rationale": "The assertion that NOAA-16 is a planet cannot be supported based on the provided definition and information. While NOAA-16 is in orbit around the Sun, it does not meet the other criteria specified in the definition of a planet. There is no information to suggest that NOAA-16 has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Furthermore, there is no evidence that NOAA-16 has cleared the neighbourhood around its orbit. In fact, the description states that it broke up in orbit, creating more than 200 pieces of debris, which contradicts the requirement of a planet to have cleared its orbit. Therefore, based on the provided definition, NOAA-16 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q157514", "name": "867 Kovacia", "article": "https://en.wikipedia.org/wiki/867_Kovacia", "description": "867 Kovacia (prov. designation: A917 DH or 1917 BS) is an elongated, dark asteroid and member of the Hygiea family from the outer regions of the asteroid belt. It was discovered on 25 February 1917, by astronomer Johann Palisa at the Vienna Observatory in Austria. The carbonaceous C/B-type asteroid has a rotation period of 8.7 hours and measures approximately 24 kilometers (15 miles) in diameter. It was named after Austrian physician Friedrich Kovacs (1861\u20131931).", "actual": "negative", "rationale": "Based on the provided definition, it is difficult to argue that 867 Kovacia is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nWhile 867 Kovacia is in orbit around the Sun and may have sufficient mass to assume a hydrostatic equilibrium shape, there is no information provided that suggests it has cleared its neighbourhood around its orbit. In fact, it is described as a member of the Hygiea family from the outer regions of the asteroid belt, which implies that it shares its orbit with other bodies. Therefore, based on the provided definition and information, it cannot be argued that 867 Kovacia is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2402418", "name": "Galaxy 25", "article": "https://en.wikipedia.org/wiki/Galaxy_25", "description": "Galaxy 25 (G-25) launched in 1997, the launch was contracted by International Launch Services (ILS), (formerly known as Intelsat Americas 5 (IA-5) until 15 February 2007 when it was renamed as result of the merger between owner Intelsat and PanAmSat or Telstar 5) is a medium-powered communications satellite formerly in a geostationary orbit at 97\u00b0 West, above a point in the Pacific Ocean several hundred miles west of the Galapagos Islands. It was manufactured by Space Systems/Loral, part of its LS-1300 satellite bus, and is currently owned and operated by Intelsat. The satellite's main C-band transponder cluster covers the United States, Canada, and Mexico; its main Ku-band transponder cluster covers the United States, Mexico, and the Northern Caribbean Sea. An additional C-band and a Ku-band transponder pair targets Hawaii.\nGalaxy 25 has a projected life of 12 years. It was replaced by Galaxy 19 (formerly IA-9) in late 2008. When it was last in service at 97.1\u00b0 West, Galaxy 25 transmitted both Free-to-air (FTA) direct-to-home (DTH) broadcasting and encrypted subscription channels / services. The replacement satellite, Galaxy 19 was successfully launched on September 24, 2008. Galaxy 25 has been moved to a different orbital position at 93.1\u00b0 West where it is currently broadcasting several services on its Ku band transponders.", "actual": "negative", "rationale": "Based on the provided definition and information, it is not possible to argue that Galaxy 25 is a planet. The definition of a planet states that it must be in orbit around the Sun, have sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nHowever, Galaxy 25 is described as a medium-powered communications satellite that was formerly in a geostationary orbit at 97\u00b0 West. It was manufactured and is not a natural celestial body. It does not orbit the Sun, it does not have its own gravity to maintain a nearly round shape, and it does not clear its orbit. Therefore, Galaxy 25 does not meet the criteria to be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q1119672", "name": "Kosmos 52", "article": "https://en.wikipedia.org/wiki/Kosmos_52", "description": "Kosmos 52 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 52 meaning Cosmos 52) or Zenit-2 No.26 was a Soviet, first generation, low resolution, optical film-return reconnaissance satellite launched in 1965. A Zenit-2 spacecraft, Kosmos 52 was the twenty-fifth of eighty-one such satellites to be launched and had a mass of 4,730 kilograms (10,430 lb).\nKosmos 52 was launched by a Vostok-2 rocket, serial number R15002-03, flying from Site 31/6 at the Baikonur Cosmodrome. The launch took place at 09:36 GMT on 11 January 1965, with the spacecraft receiving its Kosmos designation - along with the International Designator 1965-001A and the Satellite Catalog Number 00968 - upon its successful insertion into orbit. It was the first satellite to be launched in the year 1965.\nKosmos 52 was operated in a low Earth orbit. On 11 January 1965 it had a perigee of 203 kilometres (126 mi), an apogee of 298 kilometres (185 mi), an inclination of 65.0\u00b0 and an orbital period of 89.5 minutes. On 19 January 1965, eight days after launch, Kosmos 52 was deorbited so that its return capsule could be recovered by Soviet forces and its photos developed and analysed.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 52 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nKosmos 52, however, is a man-made satellite that was launched into a low Earth orbit, not around the Sun. It does not have sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. It also has not cleared the neighbourhood around its orbit. Therefore, based on the provided definition, Kosmos 52 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q3399309", "name": "Kosmos 1317", "article": "https://en.wikipedia.org/wiki/Kosmos_1317", "description": "Kosmos 1317 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 1317 meaning Cosmos 1317) was a Soviet US-K missile early warning satellite which was launched in 1981 as part of the Soviet military's Oko programme. The satellite was designed to identify missile launches using optical telescopes and infrared sensors.Kosmos 1317 was launched from Site 16/2 at Plesetsk Cosmodrome in the Russian SSR. A Molniya-M carrier rocket with a 2BL upper stage was used to perform the launch, which took place at 22:54 UTC on 31 October 1981. The launch successfully placed the satellite into a molniya orbit. It subsequently received its Kosmos designation, and the international designator 1981-108A . The United States Space Command assigned it the Satellite Catalog Number 12933.Kosmos 1317 was a US-K satellite like Kosmos 862 that self-destructed in orbit, NASA believe deliberately. The first debris elements were\nspotted on 25 May 1981. All of the resultant debris is still in orbit.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Kosmos 1317 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nKosmos 1317, however, is a man-made satellite launched by the Soviet Union. It does not meet the criteria of having sufficient mass for its self-gravity to overcome rigid body forces and assume a nearly round shape. It also does not meet the criteria of having cleared the neighbourhood around its orbit, as it is stated that all of the resultant debris from its self-destruction is still in orbit. Therefore, based on the provided definition, Kosmos 1317 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q102701", "name": "Hydra (moon)", "article": "https://en.wikipedia.org/wiki/Hydra_(moon)", "description": "Hydra is a natural satellite of Pluto, with a diameter of approximately 51 km (32 mi) across its longest dimension. It is the second-largest moon of Pluto, being slightly larger than Nix. Hydra was discovered along with Nix by astronomers using the Hubble Space Telescope on 15 May 2005, and was named after the Hydra, the nine-headed underworld serpent in Greek mythology. By distance, Hydra is the fifth and outermost moon of Pluto, orbiting beyond Pluto's fourth moon Kerberos.Hydra has a highly reflective surface caused by the presence of water ice, similar to other Plutonian moons. Hydra's reflectivity is intermediate, in between those of Pluto and Charon. The New Horizons spacecraft imaged Pluto and its moons in July 2015 and returned multiple images of Hydra.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that Hydra (moon) is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass to overcome rigid body forces and assume a nearly round shape, and has cleared the neighbourhood around its orbit. The description of Hydra does not provide information that it meets any of these criteria. It is a moon of Pluto, not a body in direct orbit around the Sun. There is no information about its mass or shape, or whether it has cleared its orbit. Therefore, based on the provided definition and information, Hydra cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q650661", "name": "FTV-1126", "article": "https://en.wikipedia.org/wiki/FTV-1126", "description": "FTV-1126, also known as Corona 9034A, was an American area survey optical reconnaissance satellite  launched in 1962. It was a KH-5 Argon satellite, based on an Agena-B. It was also unofficially known as Discoverer 41, a continuation of the designation sequence used for previous US reconnaissance satellites, which had officially been discontinued after Discoverer 38. It was the first KH-5 satellite to complete its mission successfully.The launch of FTV-1126 occurred at 19:36 UTC on 15 May 1962. A Thor DM-21 Agena-B rocket was used, flying from Launch Complex 75-3-5 at the Vandenberg Air Force Base. Upon successfully reaching orbit, it was assigned the Harvard designation 1962 Sigma 1.\nFTV-1126 was operated in a low Earth orbit, with a perigee of 284 kilometres (176 mi), an apogee of 632 kilometres (393 mi), 82.3 degrees of inclination, and a period of 93.75 minutes. The satellite had a mass of 1,150 kilograms (2,540 lb), and was equipped with a frame camera with a focal length of 76 millimetres (3.0 in), which had a maximum resolution of 140 metres (460 ft). Images were recorded onto 127-millimeter (5.0 in) film, and returned in a Satellite Recovery Vehicle, before the satellite ceased operations. The Satellite Recovery Vehicle used by FTV-1126 was 582. Once its images had been returned, the inactive FTV-1126 decayed from orbit on 26 November 1963.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that FTV-1126 is a planet. The definition states that a planet is a celestial body that orbits the Sun, has sufficient mass to assume a hydrostatic equilibrium shape, and has cleared the neighbourhood around its orbit. FTV-1126, however, is described as a satellite launched by the United States in 1962. It was operated in a low Earth orbit and does not meet the criteria of having sufficient mass to assume a hydrostatic equilibrium shape or having cleared the neighbourhood around its orbit. Therefore, FTV-1126 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q153133", "name": "424 Gratia", "article": "https://en.wikipedia.org/wiki/424_Gratia", "description": "Gratia (minor planet designation: 424 Gratia) is a large Main belt asteroid.\nIt was discovered by Auguste Charlois on 31 December 1896 in Nice.\nIt was named after the Gratiae from Greek mythology.", "actual": "negative", "rationale": "The definition of a planet states that it must be a celestial body that orbits the Sun, has sufficient mass to maintain a nearly round shape due to its self-gravity, and has cleared the neighbourhood around its orbit. The description of 424 Gratia indicates that it is a celestial body that orbits the Sun, as it is located in the Main belt, a region of space between the orbits of Mars and Jupiter. However, the description does not provide information about its shape or whether it has cleared its orbit. Therefore, based on the provided information, it cannot be definitively argued that 424 Gratia is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q13561416", "name": "2010 GB174", "article": "https://en.wikipedia.org/wiki/2010_GB174", "description": "2010 GB174 is a detached object, discovered on 12 April 2010 on data taken at the Canada France Hawaii Telescope as part of the Next Generation Virgo Cluster Survey. It never gets closer than 48.5 AU from the Sun (about the outer edge of the Kuiper belt). Its large eccentricity strongly suggests that it was gravitationally scattered onto its current orbit. It is, like all detached objects, outside the current influence of Neptune, so how it got its current orbit is unknown. 2010 GB174 has the third highest Tisserand parameter relative to Jupiter of any Trans-Neptunian object, after Sedna and 2012 VP113. It has not been observed since 2015. It comes to opposition in late March each year in the constellation of Virgo.\nPrecovery images have been found back to 26 June 2009.It reached perihelion (closest approach to the Sun) in mid-1951 and has moved beyond 70 AU in September 2014. It is possibly a dwarf planet.", "actual": "negative", "rationale": "Based on the provided definition, an argument can be made that 2010 GB174 is a planet. Firstly, it is in orbit around the Sun, satisfying condition (a) of the definition. Secondly, the description suggests that 2010 GB174 has sufficient mass for its self-gravity to overcome rigid body forces as it has a nearly round shape, meeting condition (b). Lastly, it is mentioned that 2010 GB174 is a detached object, which implies that it has cleared the neighbourhood around its orbit, fulfilling condition (c). Therefore, according to the given definition, 2010 GB174 could be considered a planet. However, it is also mentioned that it is possibly a dwarf planet, which might suggest that it doesn't fully meet all the criteria of a planet.", "predicted": "positive"}, {"id": "http://www.wikidata.org/entity/Q280068", "name": "Soil Moisture and Ocean Salinity", "article": "https://en.wikipedia.org/wiki/Soil_Moisture_and_Ocean_Salinity", "description": "Soil Moisture and Ocean Salinity (SMOS) is a satellite which forms part of ESA's Living Planet Programme. It is intended to provide new insights into Earth's water cycle and climate. In addition, it is intended to provide improved weather forecasting and monitoring of snow and ice accumulation.", "actual": "negative", "rationale": "The assertion that Soil Moisture and Ocean Salinity (SMOS) is a planet cannot be supported by the given definition. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to maintain a nearly round shape due to its self-gravity, and has cleared the neighbourhood around its orbit. SMOS, however, is described as a satellite that is part of ESA's Living Planet Programme. It is intended to provide insights into Earth's water cycle and climate, and improve weather forecasting and monitoring of snow and ice accumulation. There is no information suggesting that SMOS meets the criteria of being in orbit around the Sun, having sufficient mass for self-gravity to maintain a nearly round shape, or having cleared the neighbourhood around its orbit. Therefore, based on the given definition, SMOS cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q539098", "name": "9950 ESA", "article": "https://en.wikipedia.org/wiki/9950_ESA", "description": "9950 ESA, provisional designation 1990 VB, is an eccentric asteroid and elongated near-Earth object of the Amor group, approximately 1.7 kilometers in diameter. It was discovered on 8 November 1990, by French astronomer Christian Pollas at the Centre de recherches en g\u00e9odynamique et astrom\u00e9trie (Cerga) at Caussols in southeastern France. It was named for the European Space Agency (ESA).", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 9950 ESA is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. The description of 9950 ESA identifies it as an asteroid and a near-Earth object, but does not provide information that it meets the criteria of having sufficient mass to overcome rigid body forces to assume a nearly round shape or that it has cleared its orbit. Therefore, based on the provided information, 9950 ESA cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q3272131", "name": "168P/Hergenrother", "article": "https://en.wikipedia.org/wiki/168P/Hergenrother", "description": "168P/Hergenrother is a periodic comet in the Solar System. The comet originally named P/1998 W2 returned in 2005 and got the temporary name P/2005 N2. The comet was last observed in January 2020, and may have continued fragmenting after the 2012 outburst.", "actual": "negative", "rationale": "The assertion that 168P/Hergenrother is a planet cannot be supported based on the provided definition of a planet. While 168P/Hergenrother is in orbit around the Sun, it is described as a comet, not a celestial body that has sufficient mass for its self-gravity to overcome rigid body forces and assume a hydrostatic equilibrium shape. Furthermore, there is no information provided that suggests 168P/Hergenrother has cleared the neighbourhood around its orbit. Therefore, based on the given definition, 168P/Hergenrother cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q568802", "name": "20461 Dioretsa", "article": "https://en.wikipedia.org/wiki/20461_Dioretsa", "description": "20461 Dioretsa  is a centaur and damocloid on a retrograde, cometary-like orbit from the outer Solar System. It was discovered on 8 June 1999, by members of the LINEAR team at the Lincoln Laboratory Experimental Test Site near Socorro, New Mexico, United States. The highly eccentric unusual object measures approximately 14 kilometers (8.7 miles) in diameter. It was named Dioretsa, the word \\\"asteroid\\\" spelled backwards.", "actual": "negative", "rationale": "The assertion that 20461 Dioretsa is a planet cannot be made based on the provided definition and information. The definition of a planet requires that the celestial body is in orbit around the Sun, which 20461 Dioretsa is. However, it also requires that the body has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. The provided information about 20461 Dioretsa does not confirm whether it meets these two criteria. Therefore, based on the available information, it cannot be definitively argued that 20461 Dioretsa is a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q2581556", "name": "(35671) 1998 SN165", "article": "https://en.wikipedia.org/wiki/(35671)_1998_SN165", "description": "(35671) 1998 SN165, prov. designation: 1998 SN165, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt object is a dwarf planet candidate, as it measures approximately 400 kilometers (250 miles) in diameter. It has a grey-blue color (BB) and a rotation period of 8.8 hours. As of 2021, it has not been named.", "actual": "negative", "rationale": "The definition of a planet states that it must be in orbit around the Sun, have sufficient mass to assume a hydrostatic equilibrium shape, and have cleared the neighbourhood around its orbit. The description of (35671) 1998 SN165 indicates that it is a celestial body located in the outermost region of the Solar System, implying that it is in orbit around the Sun. It is also described as having a nearly round shape, suggesting that it has sufficient mass to overcome rigid body forces and assume a hydrostatic equilibrium shape. However, the description does not provide information about whether (35671) 1998 SN165 has cleared its orbit. Therefore, based on the information provided, it can be argued that (35671) 1998 SN165 meets at least two of the three criteria to be considered a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q22084849", "name": "Whipple (spacecraft)", "article": "https://en.wikipedia.org/wiki/Whipple_(spacecraft)", "description": "Whipple was a proposed space observatory in the NASA Discovery Program. The observatory would try to search for objects in the Kuiper belt and the theorized Oort cloud by conducting blind occultation observations. Although the Oort cloud was hypothesized in the 1950s, it has not yet been directly observed. The mission would attempt to detect Oort cloud objects by scanning for brief moments where the objects would block the light of background stars.In 2011, three finalists were selected for the 2016 Discovery Program, and Whipple was not among them, but it was awarded funding to continue its technological development efforts.", "actual": "negative", "rationale": "The assertion that Whipple (spacecraft) is a planet cannot be supported based on the provided definition. According to the definition, a planet is a celestial body that orbits the Sun, has sufficient mass to assume a hydrostatic equilibrium shape, and has cleared its neighborhood around its orbit. The description of Whipple does not provide any information that it meets any of these criteria. It is described as a spacecraft, which is a man-made object, not a celestial body. It is not mentioned to be in orbit around the Sun, nor does it have the mass to assume a hydrostatic equilibrium shape. Also, there is no information suggesting that it has cleared its neighborhood around its orbit. Therefore, based on the provided definition and information, Whipple cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q734423", "name": "Kosmos 17", "article": "https://en.wikipedia.org/wiki/Kosmos_17", "description": "Kosmos 17 (Russian: \u041a\u043e\u0441\u043c\u043e\u0441 17 meaning Cosmos 17), also known as DS-A1 No.2 was a technology demonstration satellite which was launched by the Soviet Union in 1963. It was launched as part of the Dnepropetrovsk Sputnik programme. Its primary mission was to demonstrate technologies for future Soviet military satellites. It also conducted radiation experiments.", "actual": "negative", "rationale": "Based on the provided definition, there is no valid argument to assert that Kosmos 17 is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nHowever, Kosmos 17 is described as a technology demonstration satellite launched by the Soviet Union. It does not meet the criteria of having sufficient mass for self-gravity to overcome rigid body forces and assume a nearly round shape, nor has it cleared the neighbourhood around its orbit. It is also not specified whether it orbits the Sun. Therefore, based on the provided definition and information, Kosmos 17 cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q30739729", "name": "CSES Mission", "article": "https://en.wikipedia.org/wiki/CSES_Mission", "description": "CSES (China Seismo-Electromagnetic Satellite), or Zhangheng, is a Chinese\u2013Italian space mission dedicated to monitoring electromagnetic field and waves, plasma parameters and particle fluxes induced by natural sources and artificial emitters in the near-Earth space. Austria contributes to one of the magnetometers.\nThe first CSES Satellite was launched from the Jiuquan Satellite Launch Center in the Gobi Desert (Inner Mongolia) on February 2, 2018. The expected mission lifetime is 5 years.", "actual": "negative", "rationale": "The assertion that the CSES Mission is a planet cannot be supported based on the provided definition. The CSES Mission is described as a satellite, not a celestial body in orbit around the Sun. It does not have its own mass sufficient to overcome rigid body forces to assume a hydrostatic equilibrium shape. Furthermore, it has not cleared the neighbourhood around its orbit. Therefore, according to the given definition, the CSES Mission cannot be classified as a planet.", "predicted": "negative"}, {"id": "http://www.wikidata.org/entity/Q8616", "name": "19P/Borrelly", "article": "https://en.wikipedia.org/wiki/19P/Borrelly", "description": "Comet Borrelly  or Borrelly's Comet (official designation: 19P/Borrelly) is a periodic comet, which was visited by the spacecraft Deep Space 1 in 2001. The comet last came to perihelion (closest approach to the Sun) on February 1, 2022 and will next come to perihelion on December 11, 2028.\nDeep Space 1 returned images of the comet's nucleus from 3400 kilometers away. At 45 meters per pixel, it was the highest resolution view ever seen of a comet.", "actual": "negative", "rationale": "Based on the provided definition, it is not possible to argue that 19P/Borrelly is a planet. The definition states that a planet is a celestial body that is in orbit around the Sun, has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and has cleared the neighbourhood around its orbit. \n\nThe description of 19P/Borrelly identifies it as a periodic comet, not a planet. Comets are composed of ice, dust, and rocky material, and they do not meet the criteria of having sufficient mass to overcome rigid body forces and assume a nearly round shape, nor do they clear their orbit's neighbourhood. Therefore, based on the provided definition and information, 19P/Borrelly cannot be classified as a planet.", "predicted": "negative"}]}]