id string | question string | answer string | documents list |
|---|---|---|---|
(29075)_1950_DA_16963020 | Reconstruct the content from the article about '(29075) 1950 DA'. | ''', provisional designation ', is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a value of 0.17 for a possi... | [
"(29075) 1950 DA\n\n''', provisional designation ', is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a v... |
(29075)_1950_DA_16963023 | Explain what '(29075) 1950 DA' covers in the 'Observations' section. | a rubble pile rotating faster than the breakup limit for its density, implying the asteroid is held together by van der Waals forces rather than gravity. made a distant approach to Earth on 5 February 2021. However, at that time it was half an AU away from Earth, preventing more useful astrometrics and timing that occ... | [
"(29075) 1950 DA\n\n''', provisional designation ', is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a v... |
(29075)_1950_DA_16963021 | Describe the 'Discovery and nomenclature' section of the article about '(29075) 1950 DA'. | was first discovered on 23 February 1950 by Carl A. Wirtanen at Lick Observatory. It was observed for seventeen days and then lost because this short observation arc resulted in large uncertainties in Wirtanen's orbital solution. On 31 December 2000, it was recovered at Lowell Observatory and was announced as on 4 Janu... | [
"(29075) 1950 DA\n\n''', provisional designation ', is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a v... |
(29075)_1950_DA_16963024 | Summarize the 'Possible Earth impact' part of '(29075) 1950 DA'. | an orbit moderately inclined (12 degrees) to the ecliptic plane (reducing in-plane perturbations); ; high-precision radar astrometry, which provides its distance and is complementary to the measurements of angular positions; ; a 68-year observation arc; ; an uncertainty region controlled by resonance. That has one of ... | [
"(29075) 1950 DA\n\n''', provisional designation ', is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a v... |
(29075)_1950_DA_16963022 | From the article on '(29075) 1950 DA', restate the 'Observations' content. | On 5 March 2001, made a close approach to Earth at a distance of 0.05207 AU. It was studied by radar at the Goldstone and Arecibo observatories from March 3 to 7, 2001. The studies showed that the asteroid has a mean diameter of 1.1 km, assuming that is a retrograde rotator. Optical lightcurve analysis by Lenka Sarou... | [
"(29075) 1950 DA\n\n''', provisional designation ', is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a v... |
(29075)_1950_DA_16963025 | From the article on '(29075) 1950 DA', restate the 'Possible Earth impact' content. | to slightly change as a result of the Yarkovsky effect. If ' continues on its present orbit, it may approach Earth on 16 March 2880, though the mean trajectory passes many millions of kilometres from Earth, so ' does not have a significant chance of impacting Earth. As of the 7 December 2015 solution, the probability o... | [
"(29075) 1950 DA\n\n''', provisional designation ', is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a v... |
(2R)-2-Methylpent-4-enoic_acid_25819238 | Based on the article about '(2R)-2-Methylpent-4-enoic acid', describe the 'Synthesis' section. | 1) acylation of the oxazolidinone using triethylamine as a base, and DMAP as an acyl carrier catalyst ; 2) addition of a pentene group via enolate addition using Sodium bis(trimethylsilyl)amide as a base and allyl iodide as the pentene donor ; 3) and cleavage of the oxazolidinone by LiOH solution in hydrogen peroxide. ... | [
"(2R)-2-Methylpent-4-enoic acid — Synthesis\n\n1) acylation of the oxazolidinone using triethylamine as a base, and DMAP as an acyl carrier catalyst ; 2) addition of a pentene group via enolate addition using Sodium bis(trimethylsilyl)amide as a base and allyl iodide as the pentene donor ; 3) and cleavage of the ox... |
(2R)-2-Methylpent-4-enoic_acid_25819239 | From the article on '(2R)-2-Methylpent-4-enoic acid', restate the 'Uses' content. | (R)-2-Methylpent-4-enoic acid can also be used in synthesis of other chiral compounds. For example, it has been used in the process of synthesizing the drug Sacubitril as a reagent for adding a chircal center to the molecule | [
"(2R)-2-Methylpent-4-enoic acid — Synthesis\n\n1) acylation of the oxazolidinone using triethylamine as a base, and DMAP as an acyl carrier catalyst ; 2) addition of a pentene group via enolate addition using Sodium bis(trimethylsilyl)amide as a base and allyl iodide as the pentene donor ; 3) and cleavage of the ox... |
(2R)-2-Methylpent-4-enoic_acid_25819237 | Describe the content of the article about '(2R)-2-Methylpent-4-enoic acid'. | (2R)-2-Methylpent-4-enoic acid is an organic acid with the chemical formula C6H10O2. Other names for this molecule include (R)-2-methyl-4-pentenoic acid, (R)-(−)-2-methyl-4-pentenoic acid, and methylallylacetic acid. | [
"(2R)-2-Methylpent-4-enoic acid — Synthesis\n\n1) acylation of the oxazolidinone using triethylamine as a base, and DMAP as an acyl carrier catalyst ; 2) addition of a pentene group via enolate addition using Sodium bis(trimethylsilyl)amide as a base and allyl iodide as the pentene donor ; 3) and cleavage of the ox... |
(3-Aminopropyl)triethoxysilane_29002122 | Explain what '(3-Aminopropyl)triethoxysilane' covers in the 'Toxicity' section. | APTES is a toxic compound with an MSDS health hazard score of 3. APTES fumes are destructive to the mucous membranes and the upper respiratory tract, and should be used in a fume hood with gloves. If a fume hood is not available, a face shield and full face respirator must be implemented. The target organs of APTES are... | [
"(3-Aminopropyl)triethoxysilane — Toxicity\n\nAPTES is a toxic compound with an MSDS health hazard score of 3. APTES fumes are destructive to the mucous membranes and the upper respiratory tract, and should be used in a fume hood with gloves. If a fume hood is not available, a face shield and full face respirator m... |
(3-Aminopropyl)triethoxysilane_29002121 | Describe the 'Use with cell cultures' section of the article about '(3-Aminopropyl)triethoxysilane'. | APTES-functionalized surfaces have been shown to be nontoxic to embryonic rat cardiomyocytes in vitro. Further experimentation is needed to evaluate toxicity to other cell types in extended culture. | [
"(3-Aminopropyl)triethoxysilane — Toxicity\n\nAPTES is a toxic compound with an MSDS health hazard score of 3. APTES fumes are destructive to the mucous membranes and the upper respiratory tract, and should be used in a fume hood with gloves. If a fume hood is not available, a face shield and full face respirator m... |
(3-Aminopropyl)triethoxysilane_29002119 | What information does the article about '(3-Aminopropyl)triethoxysilane' provide on 'Use with PDMS'? | APTES can be used to covalently bond thermoplastics to poly(dimethylsiloxane) (PDMS). Thermoplastics are treated with oxygen plasma to functionalize surface molecules, and subsequently coated with an aqueous 1% by volume APTES solution. PDMS is treated with oxygen plasma and placed in contact with the functionalized th... | [
"(3-Aminopropyl)triethoxysilane — Toxicity\n\nAPTES is a toxic compound with an MSDS health hazard score of 3. APTES fumes are destructive to the mucous membranes and the upper respiratory tract, and should be used in a fume hood with gloves. If a fume hood is not available, a face shield and full face respirator m... |
(3-Aminopropyl)triethoxysilane_29002118 | Summarize the following section from the article on '(3-Aminopropyl)triethoxysilane'. | (3-Aminopropyl)triethoxysilane (APTES) is an aminosilane frequently used in the process of silanization, the functionalization of surfaces with alkoxysilane molecules. It can also be used for covalent attaching of organic films to metal oxides such as silica and titania. | [
"(3-Aminopropyl)triethoxysilane — Toxicity\n\nAPTES is a toxic compound with an MSDS health hazard score of 3. APTES fumes are destructive to the mucous membranes and the upper respiratory tract, and should be used in a fume hood with gloves. If a fume hood is not available, a face shield and full face respirator m... |
(300163)_2006_VW139_32276626 | What does the article about '(300163) 2006 VW139' say regarding 'Orbit and classification'? | is a non-family asteroid of the main-belt's background population. It is both a binary asteroid and a main-belt comet, also known as "active asteroid". It orbits the Sun in the outer main-belt at a distance of 2.4–3.7 AU once every 5 years and 4 months (1,944 days; semi-major axis of 3.05 AU). Its orbit has an eccentri... | [
"(300163) 2006 VW139 — Orbit and classification\n\nis a non-family asteroid of the main-belt's background population. It is both a binary asteroid and a main-belt comet, also known as \"active asteroid\". It orbits the Sun in the outer main-belt at a distance of 2.4–3.7 AU once every 5 years and 4 months (1,944 day... |
(300163)_2006_VW139_32276628 | Based on the article about '(300163) 2006 VW139', describe the 'Diameter albedo and mass' section. | has a derived diameter of 1.8 kilometer. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.057 and calculates a diameter of 3.20 kilometers based on an absolute magnitude of 16.2. The binary system has an estimated mass between 1.3 kg and 1.1 kg. A single component has a derived mass of 6.15 kg. | [
"(300163) 2006 VW139 — Orbit and classification\n\nis a non-family asteroid of the main-belt's background population. It is both a binary asteroid and a main-belt comet, also known as \"active asteroid\". It orbits the Sun in the outer main-belt at a distance of 2.4–3.7 AU once every 5 years and 4 months (1,944 day... |
(300163)_2006_VW139_32276627 | What information does the article about '(300163) 2006 VW139' provide on 'First binary main-belt comet'? | was first observed by the Hubble Space Telescope (HST) in December 2011. It was imaged by HST in September 2016, just before it made its closest approach to the Sun and confirmed its binary nature with two asteroids orbiting each other, and revealed ongoing cometary activity. This makes the object the first known binar... | [
"(300163) 2006 VW139 — Orbit and classification\n\nis a non-family asteroid of the main-belt's background population. It is both a binary asteroid and a main-belt comet, also known as \"active asteroid\". It orbits the Sun in the outer main-belt at a distance of 2.4–3.7 AU once every 5 years and 4 months (1,944 day... |
(300163)_2006_VW139_32276625 | From the article on '(300163) 2006 VW139', restate the 'Discovery' content. | was discovered on 15 November 2006, by the Spacewatch survey at Kitt Peak National Observatory near Tucson, Arizona. The possible cometary activity was seen in November 2011 by Pan-STARRS. Both Spacewatch and Pan-STARRS are asteroid survey projects of NASA's Near Earth Object Observations Program. After the Pan-STARRS ... | [
"(300163) 2006 VW139 — Orbit and classification\n\nis a non-family asteroid of the main-belt's background population. It is both a binary asteroid and a main-belt comet, also known as \"active asteroid\". It orbits the Sun in the outer main-belt at a distance of 2.4–3.7 AU once every 5 years and 4 months (1,944 day... |
(300163)_2006_VW139_32276624 | Summarize the following section from the article on '(300163) 2006 VW139'. | , provisional designations and, as well as periodic cometary number , is a kilometer-sized asteroid from the outer regions of the asteroid belt and the first "binary main-belt comet" ever discovered. belongs to the exclusive class of main-belt comets, which display properties of both comets and asteroids. It is also a ... | [
"(300163) 2006 VW139 — Orbit and classification\n\nis a non-family asteroid of the main-belt's background population. It is both a binary asteroid and a main-belt comet, also known as \"active asteroid\". It orbits the Sun in the outer main-belt at a distance of 2.4–3.7 AU once every 5 years and 4 months (1,944 day... |
(307261)_2002_MS4_12705434 | Based on the article about '(307261) 2002 MS4', describe the 'Occultations' section. | passes through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021. Two stellar occultations by were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from participating observers. A negative chord graz... | [
"(307261) 2002 MS4 — Occultations\n\npasses through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021. Two stellar occultations by were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from parti... |
(307261)_2002_MS4_12705429 | What information does the article about '(307261) 2002 MS4' provide? | is a large classical Kuiper belt object and a possible dwarf planet in the Kuiper belt, a region of icy planetesimals beyond Neptune. It was discovered in 2002 by Chad Trujillo and Michael Brown, and has precovery images back to 8 April 1954. , is 46.4 AU from the Sun. It will reach perihelion, its closest point to the... | [
"(307261) 2002 MS4 — Occultations\n\npasses through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021. Two stellar occultations by were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from parti... |
(307261)_2002_MS4_12705431 | Describe the 'Orbit and classification' section of the article about '(307261) 2002 MS4'. | is similar in orbit and current position to Quaoar, although with higher eccentricity and inclination, orbiting every 272.5 years. belongs to the class of dynamically hot Kuiper belt objects. It is in an intermittent 18:11 orbital resonance with Neptune. | [
"(307261) 2002 MS4 — Occultations\n\npasses through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021. Two stellar occultations by were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from parti... |
(307261)_2002_MS4_12705430 | Describe the 'Discovery' section of the article about '(307261) 2002 MS4'. | was discovered on 18 June 2002 by Chad Trujillo and Michael Brown in their Caltech Wide Area Sky Survey conducted at Palomar Observatory. The discovery was announced by the Minor Planet Center on 21 November 2002. In 2007, an archive search revealed the existence of several precovery observations of, the earliest of wh... | [
"(307261) 2002 MS4 — Occultations\n\npasses through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021. Two stellar occultations by were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from parti... |
(307261)_2002_MS4_12705436 | Summarize the 'No known moons' part of '(307261) 2002 MS4'. | does not have any known moons orbiting it, thus an accurate mass estimate cannot be made. Based on its size alone, Brown lists it as nearly certain to be a dwarf planet. However, its low albedo may imply the opposite: dark, mid-sized bodies such as this, less than about 900–1000 km in diameter and with albedos le... | [
"(307261) 2002 MS4 — Occultations\n\npasses through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021. Two stellar occultations by were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from parti... |
(307261)_2002_MS4_12705432 | From the article on '(307261) 2002 MS4', restate the 'Observations' content. | , has an observation arc of 66 years. In 2008, the Spitzer Space Telescope estimated it to have a diameter of 726 km and the Herschel Space Telescope estimated it to be 934 km. Seven occultation events were observed from 2019 to 2021. The most successful was on 08 August 2020, involving 116 telescopes. The result was a... | [
"(307261) 2002 MS4 — Occultations\n\npasses through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021. Two stellar occultations by were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from parti... |
(307463)_2002_VU130_13444377 | Summarize the 'Orbit and classification' part of '(307463) 2002 VU130'. | is a plutino, a population of objects in the Kuiper belt that stay in a 2:3 resonance with Neptune. A large part of the inner Kuiper belt is formed by objects belonging to this population which is named after its largest member, Pluto. orbits the Sun at a distance of 30.9–47.1 AU once every 243 years and 9 months (89,... | [
"(307463) 2002 VU130 — Orbit and classification\n\nis a plutino, a population of objects in the Kuiper belt that stay in a 2:3 resonance with Neptune. A large part of the inner Kuiper belt is formed by objects belonging to this population which is named after its largest member, Pluto. orbits the Sun at a distance... |
(307463)_2002_VU130_13444379 | What does the article about '(307463) 2002 VU130' say regarding 'Diameter and albedo'? | Observations with Herschels PACS instrument were published in 2011. For , the measurements gave a mean-diameter of 252.9 km with an unusually high albedo of 0.179 and an absolute magnitude of 5.47. This result has been adopted in Johnstons Archive, giving a rounded diameter of 253 km, while Mike Brown estimates as simi... | [
"(307463) 2002 VU130 — Orbit and classification\n\nis a plutino, a population of objects in the Kuiper belt that stay in a 2:3 resonance with Neptune. A large part of the inner Kuiper belt is formed by objects belonging to this population which is named after its largest member, Pluto. orbits the Sun at a distance... |
(307463)_2002_VU130_13444376 | Reconstruct the content from the article about '(307463) 2002 VU130'. | , prov. designation:, is a trans-Neptunian object, located in the circumstellar disc of the Kuiper belt in the outermost region of the Solar System. The resonant trans-Neptunian object belongs to the population of plutinos and measures approximately 253 km in diameter. It was discovered on 7 November 2002, by American ... | [
"(307463) 2002 VU130 — Orbit and classification\n\nis a plutino, a population of objects in the Kuiper belt that stay in a 2:3 resonance with Neptune. A large part of the inner Kuiper belt is formed by objects belonging to this population which is named after its largest member, Pluto. orbits the Sun at a distance... |
(308635)_2005_YU55_868812 | Explain what '(308635) 2005 YU55' covers in the 'Study' section. | showed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200 meter-long, ~20 meter-high rise fo... | [
"(308635) 2005 YU55 — Study\n\nshowed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200... |
(308635)_2005_YU55_868811 | Reconstruct the content about 'Study' from the article on '(308635) 2005 YU55'. | During the 2011 passage was studied with radar using Goldstone, Arecibo, the Very Long Baseline Array, and the Green Bank Telescope. The Herschel Space Observatory has made far-infrared measurements of on 10 November, helping determine its temperature and composition. Radar analysis has also helped to pin down the aste... | [
"(308635) 2005 YU55 — Study\n\nshowed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200... |
(308635)_2005_YU55_868809 | Describe the '8 November 2011 flyby' section of the article about '(308635) 2005 YU55'. | In February 2010, was rated 1 on the Torino Scale for a potential pass near Earth on 10 November 2103, that posed no unusual level of danger. On 19 April 2010, radar ranging by the Arecibo radio telescope reduced uncertainties about the orbit by 50%. This improvement eliminated any possibility of an impact with Earth w... | [
"(308635) 2005 YU55 — Study\n\nshowed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200... |
(308635)_2005_YU55_868813 | What information does the article about '(308635) 2005 YU55' provide on 'Future trajectory'? | On 19 January 2029, will pass 0.0023 AU from Venus. The close approach distance to Venus in 2029 will determine how close the asteroid will pass to Earth in 2041. Before the November 2011 observations, the uncertainties in the post-2029 trajectory showed that the asteroid would pass somewhere between 0.002 AU and 0.3 A... | [
"(308635) 2005 YU55 — Study\n\nshowed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200... |
(308635)_2005_YU55_868808 | Reconstruct the content from the article about '(308635) 2005 YU55'. | , provisionally named 2005 YU55, is a potentially hazardous asteroid 360 meters in diameter, as measured after its Earth flyby. Previously it was estimated to be 310 meters or about 400 m (1,300 feet) in diameter. It was discovered on 28 December 2005 by Robert S. McMillan at Steward Observatory, Kitt Peak. On 8 Novemb... | [
"(308635) 2005 YU55 — Study\n\nshowed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200... |
(309239)_2007_RW10_1636097 | What information does the article about '(309239) 2007 RW10' provide on 'Discovery, orbit and physical properties'? | was discovered by the Palomar Distant Solar System Survey on September 9, 2007, with precovery images from 1988 (also taken at Palomar). At the time of discovery, this minor body was believed to be a Neptune trojan, but it is no longer listed as such. The Jet Propulsion Laboratory classifies as trans-Neptunian object b... | [
"(309239) 2007 RW10 — Discovery, orbit and physical properties\n\nwas discovered by the Palomar Distant Solar System Survey on September 9, 2007, with precovery images from 1988 (also taken at Palomar). At the time of discovery, this minor body was believed to be a Neptune trojan, but it is no longer listed as such... |
(309239)_2007_RW10_1636096 | Describe the content of the article about '(309239) 2007 RW10'. | , provisionally known as, is a temporary quasi-satellite of Neptune. Observed from Neptune, it would appear to go around it during one Neptunian year but it actually orbits the Sun, not Neptune. | [
"(309239) 2007 RW10 — Discovery, orbit and physical properties\n\nwas discovered by the Palomar Distant Solar System Survey on September 9, 2007, with precovery images from 1988 (also taken at Palomar). At the time of discovery, this minor body was believed to be a Neptune trojan, but it is no longer listed as such... |
(309239)_2007_RW10_1636098 | From the article on '(309239) 2007 RW10', restate the 'Quasi-satellite dynamical state and orbital evolution' content. | is currently following a quasi-satellite loop around Neptune. It has been a quasi-satellite of Neptune for about 12,500 years and it will remain in that dynamical state for another 12,500 years. Prior to the quasi-satellite dynamical state, was an trojan and it will go back to that state soon after leaving its current... | [
"(309239) 2007 RW10 — Discovery, orbit and physical properties\n\nwas discovered by the Palomar Distant Solar System Survey on September 9, 2007, with precovery images from 1988 (also taken at Palomar). At the time of discovery, this minor body was believed to be a Neptune trojan, but it is no longer listed as such... |
(309239)_2007_RW10_1636099 | From the article on '(309239) 2007 RW10', restate the 'Origin' content. | is a dynamically hot (both, high eccentricity and inclination) object that isunlikely to be a primordial Neptune co-orbital. It probably originated well beyond Neptune and was later temporarily captured in the 1:1 commensurability with Neptune. | [
"(309239) 2007 RW10 — Discovery, orbit and physical properties\n\nwas discovered by the Palomar Distant Solar System Survey on September 9, 2007, with precovery images from 1988 (also taken at Palomar). At the time of discovery, this minor body was believed to be a Neptune trojan, but it is no longer listed as such... |
(310071)_2010_KR59_30505956 | From the article on '(310071) 2010 KR59', restate the 'Discovery' content. | was discovered on May 18, 2010 at 7:45 UT by the WISE spacecraft. The WISE telescope scanned the entire sky in infrared light from January 2010 to February 2011. | [
"(310071) 2010 KR59 — Discovery\n\nwas discovered on May 18, 2010 at 7:45 UT by the WISE spacecraft. The WISE telescope scanned the entire sky in infrared light from January 2010 to February 2011.",
"(310071) 2010 KR59 — Co-orbital with Neptune\n\nfollows a complicated and short-lived horseshoe orbit around Neptu... |
(310071)_2010_KR59_30505959 | What does the article about '(310071) 2010 KR59' say regarding 'Co-orbital with Neptune'? | follows a complicated and short-lived horseshoe orbit around Neptune. Classical horseshoe orbits include the Lagrangian points L3, L4 and L5, this object horseshoe path goes from the L4 point towards Neptune reaching the L5 point and back. It will become a quasi-satellite of Neptune in about 5,000 years. | [
"(310071) 2010 KR59 — Discovery\n\nwas discovered on May 18, 2010 at 7:45 UT by the WISE spacecraft. The WISE telescope scanned the entire sky in infrared light from January 2010 to February 2011.",
"(310071) 2010 KR59 — Co-orbital with Neptune\n\nfollows a complicated and short-lived horseshoe orbit around Neptu... |
(310071)_2010_KR59_30505958 | From the article on '(310071) 2010 KR59', restate the 'Physical properties' content. | is a rather large minor body with an absolute magnitude of7.7 that translates into a diameter close to 100 kilometers. The discovering WISE/NEOWISE mission estimates a diameter of 110.06 kilometers with a large error margin of 30.820 km. | [
"(310071) 2010 KR59 — Discovery\n\nwas discovered on May 18, 2010 at 7:45 UT by the WISE spacecraft. The WISE telescope scanned the entire sky in infrared light from January 2010 to February 2011.",
"(310071) 2010 KR59 — Co-orbital with Neptune\n\nfollows a complicated and short-lived horseshoe orbit around Neptu... |
(310071)_2010_KR59_30505957 | From the article on '(310071) 2010 KR59', restate the 'Orbit' content. | follows a very eccentric orbit (eccentricity of 0.57) with a semi-major axis of 29.97 AU and an inclination of 19.76º. Its aphelion goes into the trans-neptunian belt but its perihelion is relatively close to Saturn's orbit. | [
"(310071) 2010 KR59 — Discovery\n\nwas discovered on May 18, 2010 at 7:45 UT by the WISE spacecraft. The WISE telescope scanned the entire sky in infrared light from January 2010 to February 2011.",
"(310071) 2010 KR59 — Co-orbital with Neptune\n\nfollows a complicated and short-lived horseshoe orbit around Neptu... |
(310071)_2010_KR59_30505955 | Summarize the following section from the article on '(310071) 2010 KR59'. | , provisional designation, is a trans-Neptunian object, approximately 110 kilometers in diameter. The object is trapped in a 1:1 mean motion resonance with Neptune, and rotates nearly every 9 hours around its axis. | [
"(310071) 2010 KR59 — Discovery\n\nwas discovered on May 18, 2010 at 7:45 UT by the WISE spacecraft. The WISE telescope scanned the entire sky in infrared light from January 2010 to February 2011.",
"(310071) 2010 KR59 — Co-orbital with Neptune\n\nfollows a complicated and short-lived horseshoe orbit around Neptu... |
(311999)_2007_NS2_26404215 | From the article on '(311999) 2007 NS2', restate the 'Origin' content. | Long-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka, calculations in both directions of time (4.5 Gyr into the past and 4.5 Gyr into the future) indicate that may be a primordial object, perhaps a survivor of the planetesimal populat... | [
"(311999) 2007 NS2 — Origin\n\nLong-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka, calculations in both directions of time (4.5 Gyr into the past and 4.5 Gyr into the future) indicate that may be a primordial object, perhaps a s... |
(311999)_2007_NS2_26404214 | Describe the 'Mars trojan and orbital evolution' section of the article about '(311999) 2007 NS2'. | Jean Meeus suspected that was a Mars Trojan, and this was confirmed by Reiner Stoss's analysis of two sets of observations dating from 1998 on the MPC database. It was confirmed to be a Mars Trojan numerically in 2012. Recent calculations confirm that it is a stable Mars Trojan asteroid with a libration period of 1310 ... | [
"(311999) 2007 NS2 — Origin\n\nLong-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka, calculations in both directions of time (4.5 Gyr into the past and 4.5 Gyr into the future) indicate that may be a primordial object, perhaps a s... |
(311999)_2007_NS2_26404213 | What does the article about '(311999) 2007 NS2' say regarding 'Discovery, orbit and physical properties'? | was discovered on 14 July 2007, by the Observatorio Astronómico de La Sagra. Its orbit is characterized by low eccentricity (0.054), moderate inclination (18.6°) and a semi-major axis of 1.52 AU. Upon discovery, it was classified as Mars-crosser by the Minor Planet Center. Its orbit is well determined as it is currentl... | [
"(311999) 2007 NS2 — Origin\n\nLong-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka, calculations in both directions of time (4.5 Gyr into the past and 4.5 Gyr into the future) indicate that may be a primordial object, perhaps a s... |
(31345)_1998_PG_4120478 | Describe the content of the article about '(31345) 1998 PG'. | is an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters. This asteroid was discovered on 3 August 1998, by the Lowell Observatory Near-Earth-Ob... | [
"(31345) 1998 PG\n\nis an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters. This asteroid was discovered on 3 August 1998, by the Lowell O... |
(31345)_1998_PG_4120481 | Describe the 'Spectral type' section of the article about '(31345) 1998 PG'. | In the SMASS taxonomy, is classified as a transitional Sq-type, which is an intermediary between the common stony S-type and the less frequent Q-type asteroids. | [
"(31345) 1998 PG\n\nis an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters. This asteroid was discovered on 3 August 1998, by the Lowell O... |
(31345)_1998_PG_4120482 | What does the article about '(31345) 1998 PG' say regarding 'Diameter and albedo'? | According to the 2006-published Photometric survey of binary near-Earth asteroids by Petr Pravec and derived data from the Collaborative Asteroid Lightcurve Link and the "Johnston's archive", measures between 880 and 940 meters in diameter and its surface has an albedo of 0.18 and 0.20, respectively. | [
"(31345) 1998 PG\n\nis an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters. This asteroid was discovered on 3 August 1998, by the Lowell O... |
(31345)_1998_PG_4120484 | Reconstruct the content about 'Moon' from the article on '(31345) 1998 PG'. | During the second photometric observation, it was discovered that is a probable/possible asynchronous binary system with a minor-planet moon orbiting it every 7.0035 hours, or twice this period solution. The moon's provisional designation is. The system has an estimated secondary-to-primary mean-diameter ratio of more ... | [
"(31345) 1998 PG\n\nis an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters. This asteroid was discovered on 3 August 1998, by the Lowell O... |
(31345)_1998_PG_4120485 | What information does the article about '(31345) 1998 PG' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 30 November 2001. As of 2018, it has not been named. | [
"(31345) 1998 PG\n\nis an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters. This asteroid was discovered on 3 August 1998, by the Lowell O... |
(31345)_1998_PG_4120480 | From the article on '(31345) 1998 PG', restate the 'Close approaches' content. | The asteroid has an Earth minimum orbital intersection distance of 0.2354 AU, which translates into approximately 92 lunar distances. It has made multiple close approaches to Earth, with the closest being 35,648,680 kilometers on 15 October 1978. With an aphelion of more than 2.8 AU, is also a Mars-crosser. | [
"(31345) 1998 PG\n\nis an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters. This asteroid was discovered on 3 August 1998, by the Lowell O... |
(315530)_2008_AP129_16721807 | Explain what '(315530) 2008 AP129' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 7 February 2012. As of 2018, it has not been named. | [
"(315530) 2008 AP129 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 7 February 2012. As of 2018, it has not been named.",
"(315530) 2008 AP129\n\nis a trans-Neptunian object and possibly a cubewano from the outermost regions of the Solar System, approximately 480 kilometers... |
(315530)_2008_AP129_16721805 | Describe the content of the article about '(315530) 2008 AP129'. | is a trans-Neptunian object and possibly a cubewano from the outermost regions of the Solar System, approximately 480 kilometers in diameter. It was discovered on 11 January 2008, by American Michael E. Brown and Megan Schwamb at Palomar Observatory in California. | [
"(315530) 2008 AP129 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 7 February 2012. As of 2018, it has not been named.",
"(315530) 2008 AP129\n\nis a trans-Neptunian object and possibly a cubewano from the outermost regions of the Solar System, approximately 480 kilometers... |
(315530)_2008_AP129_16721806 | What information does the article about '(315530) 2008 AP129' provide on 'Description'? | orbits the Sun at a distance of 36.1–47.6 AU once every 270 years and 5 months (98,778 days; semi-major axis of 41.8 AU). Its orbit has an eccentricity of 0.14 and an inclination of 27° with respect to the ecliptic. It has 3 precovery observations back to 1989. Lightcurve analysis gave an ambiguous rotation period of 9... | [
"(315530) 2008 AP129 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 7 February 2012. As of 2018, it has not been named.",
"(315530) 2008 AP129\n\nis a trans-Neptunian object and possibly a cubewano from the outermost regions of the Solar System, approximately 480 kilometers... |
(316179)_2010_EN65_30506018 | Explain what '(316179) 2010 EN65' covers in the 'Jumping trojan' section. | is another co-orbital of Neptune, the second brightest after the quasi-satellite. is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed "jumping trojan". | [
"(316179) 2010 EN65 — Jumping trojan\n\nis another co-orbital of Neptune, the second brightest after the quasi-satellite. is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed \"jumping trojan\".",
"(316179) 2010 EN65\n\nis a tran... |
(316179)_2010_EN65_30506014 | Reconstruct the content from the article about '(316179) 2010 EN65'. | is a trans-Neptunian object orbiting the Sun. However, with a semi-major axis of 30.8 AU, the object is actually a jumping Neptune trojan, co-orbital with Neptune, as the giant planet has a similar semi-major axis of 30.1 AU. The body is jumping from the Lagrangian point into via. , it is 54 AU from Neptune. By 2070, ... | [
"(316179) 2010 EN65 — Jumping trojan\n\nis another co-orbital of Neptune, the second brightest after the quasi-satellite. is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed \"jumping trojan\".",
"(316179) 2010 EN65\n\nis a tran... |
(316179)_2010_EN65_30506017 | Explain what '(316179) 2010 EN65' covers in the 'Physical properties' section. | is a quite large minor body with an absolute magnitude of 7.17 and an estimated diameter of 176 km based on an assumed albedo of 0.08. | [
"(316179) 2010 EN65 — Jumping trojan\n\nis another co-orbital of Neptune, the second brightest after the quasi-satellite. is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed \"jumping trojan\".",
"(316179) 2010 EN65\n\nis a tran... |
(316179)_2010_EN65_30506015 | From the article on '(316179) 2010 EN65', restate the 'Discovery' content. | was discovered on 7 March 2010, by David L. Rabinowitz and Suzanne W. Tourtellotte using the 1.3-meter Small and Medium Research Telescope System (SMARTS) at Cerro Tololo Observatory in Chile. | [
"(316179) 2010 EN65 — Jumping trojan\n\nis another co-orbital of Neptune, the second brightest after the quasi-satellite. is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed \"jumping trojan\".",
"(316179) 2010 EN65\n\nis a tran... |
(316179)_2010_EN65_30506019 | What does the article about '(316179) 2010 EN65' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 7 February 2012 (M.P.C. 78220). , it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures related to the Amazons, an all-female warrior tribe that ... | [
"(316179) 2010 EN65 — Jumping trojan\n\nis another co-orbital of Neptune, the second brightest after the quasi-satellite. is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed \"jumping trojan\".",
"(316179) 2010 EN65\n\nis a tran... |
(316179)_2010_EN65_30506016 | What does the article about '(316179) 2010 EN65' say regarding 'Orbit'? | follows a rather eccentric orbit (0.31) with a semi-major axis of 30.72 AU and an inclination of 19.3º. Its orbit is well determined with images dating back to 1989. | [
"(316179) 2010 EN65 — Jumping trojan\n\nis another co-orbital of Neptune, the second brightest after the quasi-satellite. is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed \"jumping trojan\".",
"(316179) 2010 EN65\n\nis a tran... |
(323137)_2003_BM80_8679969 | What information does the article about '(323137) 2003 BM80' provide? | , provisional designation: and cometary designation, is an asteroid and main-belt comet from the outer regions of the asteroid belt, approximately 9.4 km in diameter. It was discovered on 31 January 2003, by astronomers of the LONEOS program conducted at Anderson Mesa Station near Flagstaff, Arizona, in the United Stat... | [
"(323137) 2003 BM80\n\n, provisional designation: and cometary designation, is an asteroid and main-belt comet from the outer regions of the asteroid belt, approximately 9.4 km in diameter. It was discovered on 31 January 2003, by astronomers of the LONEOS program conducted at Anderson Mesa Station near Flagstaff, ... |
(323137)_2003_BM80_8679971 | Describe the 'Numbering and naming' section of the article about '(323137) 2003 BM80'. | This minor planet was numbered by the Minor Planet Center on 6 April 2012. , it has not been named. | [
"(323137) 2003 BM80\n\n, provisional designation: and cometary designation, is an asteroid and main-belt comet from the outer regions of the asteroid belt, approximately 9.4 km in diameter. It was discovered on 31 January 2003, by astronomers of the LONEOS program conducted at Anderson Mesa Station near Flagstaff, ... |
(323137)_2003_BM80_8679970 | Explain what '(323137) 2003 BM80' covers in the 'Orbit and classification' section. | is a main-belt comet with a Jupiter Tisserand's parameter of 2.99. It orbits the Sun in the outer asteroid belt at a distance of 3.4–5.1 AU once every 8 years and 9 months (3,199 days; semi-major axis of 4.25 AU). Its orbit has an eccentricity of 0.19 and an inclination of 6° with respect to the ecliptic. The body's ob... | [
"(323137) 2003 BM80\n\n, provisional designation: and cometary designation, is an asteroid and main-belt comet from the outer regions of the asteroid belt, approximately 9.4 km in diameter. It was discovered on 31 January 2003, by astronomers of the LONEOS program conducted at Anderson Mesa Station near Flagstaff, ... |
(32496)_2000_WX182_15688053 | Reconstruct the content about 'Diameter and albedo' from the article on '(32496) 2000 WX182'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 48.02 and 51.63 kilometers in diameter and its surface has an albedo of 0.070 and 0.080, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo... | [
"(32496) 2000 WX182 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 48.02 and 51.63 kilometers in diameter and its surface has an albedo of 0.070 and 0.080, respectively. The Collaborative A... |
(32496)_2000_WX182_15688049 | Explain what '(32496) 2000 WX182' covers in the 'Orbit and classification' section. | is a Jupiter trojan in a 1:1 orbital resonance with Jupiter. It is located in the trailering Trojan camp at the Gas Giant's Lagrangian point, 60° behind its orbit. It is also a non-family asteroid of the Jovian background population. It orbits the Sun at a distance of 4.9–5.7 AU once every 12 years and 1 month (4,419 d... | [
"(32496) 2000 WX182 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 48.02 and 51.63 kilometers in diameter and its surface has an albedo of 0.070 and 0.080, respectively. The Collaborative A... |
(32496)_2000_WX182_15688050 | What does the article about '(32496) 2000 WX182' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 30 November 2001 (M.P.C. 44050). , it has not been named. | [
"(32496) 2000 WX182 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 48.02 and 51.63 kilometers in diameter and its surface has an albedo of 0.070 and 0.080, respectively. The Collaborative A... |
(32496)_2000_WX182_15688048 | Describe the content of the article about '(32496) 2000 WX182'. | , provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 50 km in diameter. It was discovered on 18 November 2000, by astronomers with the LINEAR program at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The dark Jovian asteroid belongs the 100... | [
"(32496) 2000 WX182 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 48.02 and 51.63 kilometers in diameter and its surface has an albedo of 0.070 and 0.080, respectively. The Collaborative A... |
(32496)_2000_WX182_15688051 | Summarize the 'Physical characteristics' part of '(32496) 2000 WX182'. | is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical V–I color index of 0.95 and a BR color of 1.23 (also see table below). | [
"(32496) 2000 WX182 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 48.02 and 51.63 kilometers in diameter and its surface has an albedo of 0.070 and 0.080, respectively. The Collaborative A... |
(33342)_1998_WT24_32759068 | Based on the article about '(33342) 1998 WT24', describe the 'Future flyby candidate' section. | has an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list of possible Near-Earth Asteroid targets for future... | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759065 | What does the article about '(33342) 1998 WT24' say regarding 'Physical characteristics'? | During its close encounters in 2001 and 2015, astronomers were able to make radar images of its surface and determine physical properties that remain unknown for most asteroids. According to the ExploreNEOs Warm Spitzer Exploration Science program, is a bright E-type asteroid with an exceptionally high albedo of 0.75. | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759062 | Reconstruct the content about 'Record close encounter' from the article on '(33342) 1998 WT24'. | is a potentially hazardous asteroid. That means its orbit takes it very close to Earth and if it were to collide with our planet, it would cause devastation on at least a regional scale. On 16 December 2001, it became the first PHA to be observed passing within 5 Lunar Distances (the average distance between Earth and ... | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759069 | What information does the article about '(33342) 1998 WT24' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 28 January 2002. As of 2018, it has not been named. | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759067 | What information does the article about '(33342) 1998 WT24' provide on 'Rotation period'? | Several rotational lightcurves of have been obtained from radiometric and photometric observations. Lightcurve analysis gave a consolidated rotation period of 3.697 hours with a brightness amplitude between 0.19 and 0.65 magnitude (U=3). | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759066 | What does the article about '(33342) 1998 WT24' say regarding 'Diameter and albedo'? | measures between 350 and 415 meters in diameter and its surface has an albedo between 0.34 and 0.75. The Collaborative Asteroid Lightcurve Link an albedo of 0.34 and takes a diameter of 410 meters based on an absolute magnitude of 18.69. The asteroid is modestly elongated, approximately 420 × 330 meters. | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759060 | Based on the article about '(33342) 1998 WT24', describe the 'Low aphelion' section. | At the time of its discovery, astronomers were trying to find the first Apohele asteroid (one that is always closer to the Sun than Earth). All asteroids known at the time that got closer to the Sun than Earth also crossed Earth's orbit. Earlier that year, David J. Tholen claimed to have spotted the first Apohele aster... | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759064 | What information does the article about '(33342) 1998 WT24' provide on 'Frequent inner-planet encounters'? | is a Mercury-crosser asteroid, a Venus-crosser asteroid, and an Earth-crosser asteroid. Because of its relatively low inclination (7.34°), it is able to come close to each of these planets. Its orbit takes it within 0.021 AU of Mercury's orbit, 0.0368 AU of Venus's orbit, and 0.00989 AU of Earth's orbit. It makes frequ... | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759059 | From the article on '(33342) 1998 WT24', restate the 'Classification and orbit' content. | orbits the Sun at a distance of 0.42–1.02 AU once every 7 months (222 days; semi-major axis of 0.72 AU). Its orbit has an eccentricity of 0.42 and an inclination of 7° with respect to the ecliptic. | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759058 | What information does the article about '(33342) 1998 WT24' provide? | is a bright, sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid (PHA) of the Aten group, located in Venus's zone of influence that has frequent close encounters with Mercury, Venus, and Earth. It made a close approach to Earth on 11 December 2015, passing at a distance of about 4... | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759063 | Explain what '(33342) 1998 WT24' covers in the 'Record close encounter' section. | August 1969. However, was not discovered until September 1999 many years after its closest approach, so no one knew about in 1969. In September 2004, the well known PHA 4179 Toutatis came about 4 Lunar Distances from Earth. Due to its diameter being over ten times larger (5.7 km) and its closer approach, Toutatis at i... | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(33342)_1998_WT24_32759061 | What does the article about '(33342) 1998 WT24' say regarding 'Venus zone of influence'? | was the second asteroid discovered to be close enough to Venus as to be within the major planet's zone of influence. It is located at about the inner edge of the zone, while (99907) 1989 VA, the first asteroid discovered there, is at about the outer edge. It is possible for planets to capture asteroids located in their... | [
"(33342) 1998 WT24 — Future flyby candidate\n\nhas an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth. Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list... |
(336756)_2010_NV1_12790756 | Describe the 'Discovery' section of the article about '(336756) 2010 NV1'. | This trans-Neptunian object was discovered on 1 July 2010, by NASA's space-based Wide-field Infrared Survey Explorer (WISE). It was first observed by the Mount Lemmon Survey in 2009, extending the body's observation arc by 8 months prior to its official discovery observation by WISE. | [
"(336756) 2010 NV1 — Discovery\n\nThis trans-Neptunian object was discovered on 1 July 2010, by NASA's space-based Wide-field Infrared Survey Explorer (WISE). It was first observed by the Mount Lemmon Survey in 2009, extending the body's observation arc by 8 months prior to its official discovery observation by WIS... |
(336756)_2010_NV1_12790755 | Describe the content of the article about '(336756) 2010 NV1'. | , prov. designation:, is a highly eccentric planet crossing trans-Neptunian object, also classified as centaur and damocloid, approximately 52 km in diameter. It is on a retrograde cometary orbit. It has a barycentric semi-major axis (average distance from the Sun) of approximately 286 AU. | [
"(336756) 2010 NV1 — Discovery\n\nThis trans-Neptunian object was discovered on 1 July 2010, by NASA's space-based Wide-field Infrared Survey Explorer (WISE). It was first observed by the Mount Lemmon Survey in 2009, extending the body's observation arc by 8 months prior to its official discovery observation by WIS... |
(336756)_2010_NV1_12790758 | From the article on '(336756) 2010 NV1', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 31 August 2012 (M.P.C. 80287). , it has not been named. | [
"(336756) 2010 NV1 — Discovery\n\nThis trans-Neptunian object was discovered on 1 July 2010, by NASA's space-based Wide-field Infrared Survey Explorer (WISE). It was first observed by the Mount Lemmon Survey in 2009, extending the body's observation arc by 8 months prior to its official discovery observation by WIS... |
(336756)_2010_NV1_12790759 | From the article on '(336756) 2010 NV1', restate the 'Physical characteristics' content. | According to the surveys carried out by the NEOWISE mission, measures 44.2 kilometers in diameter and its surface has a low albedo of 0.057. More recent published data gives an diameter of 52.2 kilometers with an albedo of 0.042. | [
"(336756) 2010 NV1 — Discovery\n\nThis trans-Neptunian object was discovered on 1 July 2010, by NASA's space-based Wide-field Infrared Survey Explorer (WISE). It was first observed by the Mount Lemmon Survey in 2009, extending the body's observation arc by 8 months prior to its official discovery observation by WIS... |
(336756)_2010_NV1_12790757 | Summarize the 'Orbit and classification' part of '(336756) 2010 NV1'. | orbits the Sun at a distance of 9.4–547.2 AU once every 4643 years and 5 months (1,696,004 days; semi-major axis of 278.33 AU). Its orbit has an eccentricity of 0.97 and an inclination of 141° with respect to the ecliptic. It came to perihelion in December 2010 at a distance of 9.4 AU from the Sun. , it is 21.3 AU from... | [
"(336756) 2010 NV1 — Discovery\n\nThis trans-Neptunian object was discovered on 1 July 2010, by NASA's space-based Wide-field Infrared Survey Explorer (WISE). It was first observed by the Mount Lemmon Survey in 2009, extending the body's observation arc by 8 months prior to its official discovery observation by WIS... |
(341843)_2008_EV5_10643198 | Describe the 'Origin and orbital history' section of the article about '(341843) 2008 EV5'. | started its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption event that resulted in a highly fractured, shattered, or r... | [
"(341843) 2008 EV5 — Origin and orbital history\n\nstarted its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption eve... |
(341843)_2008_EV5_10643202 | Describe the 'Physical characteristics' section of the article about '(341843) 2008 EV5'. | is an oblate spheroid (also described as "muffin-shaped" ) 400 m in diameter. It rotates very slowly in a retrograde direction. There is a 150 m diameter concave feature, possibly an impact crater, or a relic feature from a previous episode of rapid rotation that caused the asteroid's shape to reconfigure. Visible and ... | [
"(341843) 2008 EV5 — Origin and orbital history\n\nstarted its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption eve... |
(341843)_2008_EV5_10643201 | Based on the article about '(341843) 2008 EV5', describe the '2008 close approach' section. | On 23 December 2008, made a close approach to Earth at a distance of 8.4 lunar distances (0.022 AU, 3.2 million km), its closest until 2169. Its brightness peaked on 26 December about 13.2 magnitude. | [
"(341843) 2008 EV5 — Origin and orbital history\n\nstarted its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption eve... |
(341843)_2008_EV5_10643197 | Reconstruct the content from the article about '(341843) 2008 EV5'. | , provisional designation, is a sub-kilometer asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Aten group, approximately 400 m in diameter. It was discovered on 4 March 2008, by astronomers of the Mount Lemmon Survey at Mount Lemmon Observatory near Tucson, Arizona, United States. | [
"(341843) 2008 EV5 — Origin and orbital history\n\nstarted its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption eve... |
(341843)_2008_EV5_10643203 | Summarize the 'Sample return mission' part of '(341843) 2008 EV5'. | was the preliminary baseline target of NASA's proposed sample-return Asteroid Redirect Mission. Besides, several other asteroids, including Itokawa and Bennu, were considered for this mission, before its cancellation in 2017. | [
"(341843) 2008 EV5 — Origin and orbital history\n\nstarted its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption eve... |
(341843)_2008_EV5_10643200 | Summarize the 'Origin and orbital history' part of '(341843) 2008 EV5'. | it can produce substantial orbital changes over timescales ranging from many millions to billions of years. The same physical phenomenon also creates a thermal torque that probably caused to take on a top-like appearance. Dynamical models indicate that migrated inward across the inner asteroid belt over long timescales... | [
"(341843) 2008 EV5 — Origin and orbital history\n\nstarted its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption eve... |
(341843)_2008_EV5_10643199 | Summarize the 'Origin and orbital history' part of '(341843) 2008 EV5'. | lower than 10%. If it does have a high albedo, a plausible source would be a population of high-albedo C-type asteroids in the inner asteroid belt. Second tier candidate families for the high-albedo case are Baptistina and Pallas. From here, the newly liberated began to change via the forces referred to as the Yarkovsk... | [
"(341843) 2008 EV5 — Origin and orbital history\n\nstarted its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers. 's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption eve... |
(342842)_2008_YB3_17602612 | Explain what '(342842) 2008 YB3' covers in the 'Diameter and albedo' section. | According to the survey of centaurs and scattered-disc objects carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 67.1 km in diameter and its surface has an albedo of 0.062, which makes it too small to be considered as a dwarf-planet candidate. | [
"(342842) 2008 YB3 — Diameter and albedo\n\nAccording to the survey of centaurs and scattered-disc objects carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 67.1 km in diameter and its surface has an albedo of 0.062, which makes it too small to be considered as a dwarf-plan... |
(342842)_2008_YB3_17602610 | Based on the article about '(342842) 2008 YB3', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 29 October 2012, receiving the number in the minor planet catalog (M.P.C. 80959). , it has not been named. According to the established naming conventions, it will be named after one of the many centaurs from Greek mythology, which are creatures with the upp... | [
"(342842) 2008 YB3 — Diameter and albedo\n\nAccording to the survey of centaurs and scattered-disc objects carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 67.1 km in diameter and its surface has an albedo of 0.062, which makes it too small to be considered as a dwarf-plan... |
(342842)_2008_YB3_17602613 | Based on the article about '(342842) 2008 YB3', describe the 'Rotation period' section. | , no rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. | [
"(342842) 2008 YB3 — Diameter and albedo\n\nAccording to the survey of centaurs and scattered-disc objects carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 67.1 km in diameter and its surface has an albedo of 0.062, which makes it too small to be considered as a dwarf-plan... |
(342842)_2008_YB3_17602608 | What information does the article about '(342842) 2008 YB3' provide on 'Orbit and classification'? | orbits the Sun at a distance of 6.5–16.7 AU once every 39 years and 5 months (14,399 days; semi-major axis of 11.58 AU). Its orbit has an eccentricity of 0.44 and an inclination of 105° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Siding Spring in December 2... | [
"(342842) 2008 YB3 — Diameter and albedo\n\nAccording to the survey of centaurs and scattered-disc objects carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 67.1 km in diameter and its surface has an albedo of 0.062, which makes it too small to be considered as a dwarf-plan... |
(342842)_2008_YB3_17602607 | Summarize the following section from the article on '(342842) 2008 YB3'. | , provisional designation:, is a sizable centaur and retrograde damocloid from the outer Solar System, approximately 67 km in diameter. It was discovered on 18 December 2008, by astronomers with the Siding Spring Survey at the Siding Spring Observatory in Australia. The minor planet was numbered in 2012 and has since n... | [
"(342842) 2008 YB3 — Diameter and albedo\n\nAccording to the survey of centaurs and scattered-disc objects carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 67.1 km in diameter and its surface has an albedo of 0.062, which makes it too small to be considered as a dwarf-plan... |
(35107)_1991_VH_23165656 | Explain what '(35107) 1991 VH' covers in the 'Close approaches' section. | The asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008. | [
"(35107) 1991 VH — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH — Mas... |
(35107)_1991_VH_23165658 | Reconstruct the content about 'Mass and density' from the article on '(35107) 1991 VH'. | The total mass of the system is 1.58 kg, based on the orbital motion of the satellite. The mass ratio of the satellite to the primary is 0.086, corresponding to a primary mass of 1.4 kg—approximately 12 times as massive as the satellite. Given the primary mass and diameter, its density is estimated to be about 1.7 g/cm... | [
"(35107) 1991 VH — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH — Mas... |
(35107)_1991_VH_23165660 | From the article on '(35107) 1991 VH', restate the 'Rotation' content. | Photometric observations in 1997 determined a primary rotation period of 2.624 hours, with a light curve amplitude of 0.08 magnitudes (U=3). Later photometric observations from 2003–2020 corroborated this result down to a precision of ±0.0001 seconds. | [
"(35107) 1991 VH — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH — Mas... |
(35107)_1991_VH_23165655 | Summarize the 'Orbit' part of '(35107) 1991 VH'. | orbits the Sun at a distance of 0.98–1.30 AU once every 1.21 years (443 days). Its orbit has an eccentricity of 0.14 and an inclination of 14° with respect to the ecliptic. | [
"(35107) 1991 VH — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH — Mas... |
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