id string | question string | answer string | documents list |
|---|---|---|---|
(154276)_2002_SY50_26180814 | Reconstruct the content about 'Close approaches' from the article on '(154276) 2002 SY50'. | The asteroid has an Earth minimum orbital intersection distance of 0.0027 AU, which corresponds to 1.05 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. In November 1933, it approached Earth at a nominal distance of 0.098 AU, and in November 2002 at 0.084 AU. Its closest... | [
"(154276) 2002 SY50 β Physical characteristics\n\nPhotometry by the Sloan Digital Sky Survey has characterized as an uncommon K-type asteroid, which is typically seen among members of the Eos family in the asteroid belt.",
"(154276) 2002 SY50\n\n, provisional designation, is a stony asteroid on a highly eccentric... |
(154276)_2002_SY50_26180818 | Based on the article about '(154276) 2002 SY50', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 2 April 2007 (M.P.C. 59337). As of 2018, it has not been named. | [
"(154276) 2002 SY50 β Physical characteristics\n\nPhotometry by the Sloan Digital Sky Survey has characterized as an uncommon K-type asteroid, which is typically seen among members of the Eos family in the asteroid belt.",
"(154276) 2002 SY50\n\n, provisional designation, is a stony asteroid on a highly eccentric... |
(15502)_1999_NV27_11686092 | Summarize the following section from the article on '(15502) 1999 NV27'. | , provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 53 km in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian asteroid has a rotation period o... | [
"(15502) 1999 NV27\n\n, provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 53 km in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian astero... |
(15502)_1999_NV27_11686094 | From the article on '(15502) 1999 NV27', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 21 June 2000 (M.P.C. 40827). , it has not been named. | [
"(15502) 1999 NV27\n\n, provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 53 km in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian astero... |
(15502)_1999_NV27_11686096 | Reconstruct the content about 'Rotation period' from the article on '(15502) 1999 NV27'. | In September 2009, a first rotational lightcurve of was obtained from photometric observations by Linda French at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a rotation period of 15.03 hours with a brightness variation of 0.10 magnitude (U=2). Since then, follow-up observations by Da... | [
"(15502) 1999 NV27\n\n, provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 53 km in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian astero... |
(15502)_1999_NV27_11686093 | What information does the article about '(15502) 1999 NV27' provide on 'Orbit and classification'? | is a dark Jovian asteroid in a 1:1 orbital resonance with Jupiter. It is located in the trailering Trojan camp at the Gas Giant's Lagrangian point, 60Β° behind its orbit. It is also a non-family asteroid of the Jovian background population. It orbits the Sun at a distance of 5.0β5.2 AU once every 11 years and 7 months (... | [
"(15502) 1999 NV27\n\n, provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 53 km in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian astero... |
(15502)_1999_NV27_11686097 | From the article on '(15502) 1999 NV27', restate the 'Diameter and albedo' content. | According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 50.86 and 53.10 kilometers in diameter and its surface has an albedo of 0.067 and 0.069, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albed... | [
"(15502) 1999 NV27\n\n, provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 53 km in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian astero... |
(15692)_1984_RA_3700177 | Based on the article about '(15692) 1984 RA', describe the 'Rotation period' section. | In July 2013, a rotational lightcurve of this asteroid was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station in California. Lightcurve analysis gave a long rotation period of 37.44 hours with a brightness amplitude of 0.66 magnitude, indicative of an elongated shape... | [
"(15692) 1984 RA β Rotation period\n\nIn July 2013, a rotational lightcurve of this asteroid was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station in California. Lightcurve analysis gave a long rotation period of 37.44 hours with a brightness amplitude of 0.66 m... |
(15692)_1984_RA_3700179 | What does the article about '(15692) 1984 RA' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40991). As of 2018, it has not been named. | [
"(15692) 1984 RA β Rotation period\n\nIn July 2013, a rotational lightcurve of this asteroid was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station in California. Lightcurve analysis gave a long rotation period of 37.44 hours with a brightness amplitude of 0.66 m... |
(15692)_1984_RA_3700178 | Describe the 'Diameter and albedo' section of the article about '(15692) 1984 RA'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures 1.728 kilometers in diameter and its surface has an exceptionally high albedo of 0.78. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.30 β a compromise value between the E-... | [
"(15692) 1984 RA β Rotation period\n\nIn July 2013, a rotational lightcurve of this asteroid was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station in California. Lightcurve analysis gave a long rotation period of 37.44 hours with a brightness amplitude of 0.66 m... |
(15692)_1984_RA_3700174 | Summarize the following section from the article on '(15692) 1984 RA'. | , provisional designation, is a Hungaria asteroid from the innermost regions of the asteroid belt, approximately 2 km in diameter. It was discovered on 1 September 1984, by Italian astronomer Maria Barucci at the Palomar Observatory in California, United States. The presumed E-type asteroid has a longer-than average ro... | [
"(15692) 1984 RA β Rotation period\n\nIn July 2013, a rotational lightcurve of this asteroid was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station in California. Lightcurve analysis gave a long rotation period of 37.44 hours with a brightness amplitude of 0.66 m... |
(15700)_1987_QD_16023030 | Reconstruct the content about 'Orbit and classification' from the article on '(15700) 1987 QD'. | is a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5β2.9 AU once every 3 years and 3 months (1,199 days; semi-maj... | [
"(15700) 1987 QD β Orbit and classification\n\nis a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5β2.9 AU on... |
(15700)_1987_QD_16023032 | Reconstruct the content about 'Physical characteristics' from the article on '(15700) 1987 QD'. | In the SDSS-based taxonomy and according to the survey conducted by Pan-STARRS, is an X-type asteroid. It has also been classified as a common, stony S-type asteroid. | [
"(15700) 1987 QD β Orbit and classification\n\nis a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5β2.9 AU on... |
(15700)_1987_QD_16023034 | What does the article about '(15700) 1987 QD' say regarding 'Strong binary candidate'? | The photometric observations during September and October 2010 revealed that is a candidate for a synchronous binary asteroid with a minor-planet moon orbiting it every 50.3 hours at an estimated average distance of 14 km. The findings were announced on 6 November 2009. The lightcurve indicated mutual occultation even... | [
"(15700) 1987 QD β Orbit and classification\n\nis a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5β2.9 AU on... |
(15700)_1987_QD_16023029 | Reconstruct the content from the article about '(15700) 1987 QD'. | ''', provisional designation ', is a Mars-crossing asteroid and a binary candidate from inside the innermost region of the asteroid belt, approximately 3 km in diameter. It was discovered on 24 August 1987, by American astronomer Stephen Singer-Brewster at the Palomar Observatory in California. The likely spherical X-t... | [
"(15700) 1987 QD β Orbit and classification\n\nis a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5β2.9 AU on... |
(15700)_1987_QD_16023035 | What does the article about '(15700) 1987 QD' say regarding 'Diameter and albedo'? | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 2.95 kilometers in diameter and its surface has an albedo of 0.268, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and derives a diameter of 3.04 k... | [
"(15700) 1987 QD β Orbit and classification\n\nis a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5β2.9 AU on... |
(15700)_1987_QD_16023031 | Explain what '(15700) 1987 QD' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40991). As of 2018, it has not been named. | [
"(15700) 1987 QD β Orbit and classification\n\nis a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5β2.9 AU on... |
(15874)_1996_TL66_13857091 | Summarize the following section from the article on '(15874) 1996 TL66'. | , provisional designation, is a trans-Neptunian object of the scattered disc orbiting in the outermost region of the Solar System. The Spitzer Space Telescope has estimated this object to be about 575 km in diameter, but 2012 estimates from the Herschel Space Observatory estimate the diameter as closer to 339 km. It is... | [
"(15874) 1996 TL66\n\n, provisional designation, is a trans-Neptunian object of the scattered disc orbiting in the outermost region of the Solar System. The Spitzer Space Telescope has estimated this object to be about 575 km in diameter, but 2012 estimates from the Herschel Space Observatory estimate the diameter ... |
(15874)_1996_TL66_13857093 | Reconstruct the content about 'Orbit and size' from the article on '(15874) 1996 TL66'. | orbits the Sun with a semi-major axis of 83.9 AU but is currently only 35 AU from the Sun with an apparent magnitude of 21. In 2007, the Spitzer Space Telescope estimated it to have a low albedo with a diameter of about 575 km. More-recent measurements in 2012 by the 'TNOs are Cool' research project and reanalysis of o... | [
"(15874) 1996 TL66\n\n, provisional designation, is a trans-Neptunian object of the scattered disc orbiting in the outermost region of the Solar System. The Spitzer Space Telescope has estimated this object to be about 575 km in diameter, but 2012 estimates from the Herschel Space Observatory estimate the diameter ... |
(15874)_1996_TL66_13857092 | Reconstruct the content about 'Discovery' from the article on '(15874) 1996 TL66'. | Discovered in 1996 by David C. Jewitt et al., it was the first object to be categorized as a scattered-disk object (SDO), although, discovered a year earlier, was later recognised as a scattered-disk object. It was considered one the largest known trans-Neptunian objects at the time of the discovery, being placed secon... | [
"(15874) 1996 TL66\n\n, provisional designation, is a trans-Neptunian object of the scattered disc orbiting in the outermost region of the Solar System. The Spitzer Space Telescope has estimated this object to be about 575 km in diameter, but 2012 estimates from the Herschel Space Observatory estimate the diameter ... |
(15875)_1996_TP66_2105749 | Reconstruct the content about 'Physical properties' from the article on '(15875) 1996 TP66'. | has a RR taxonomic class, with "very red" surface in the visible (rather than a "neutral" or "grey-blue" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660) and VβI (1.310). The resulting BβR magnitude is 1.71... | [
"(15875) 1996 TP66 β Physical properties\n\nhas a RR taxonomic class, with \"very red\" surface in the visible (rather than a \"neutral\" or \"grey-blue\" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660... |
(15875)_1996_TP66_2105746 | What information does the article about '(15875) 1996 TP66' provide on 'Orbit and classification'? | belongs to the dynamical population of plutinos, named after its largest member, Pluto. Plutinos are resonant trans-Neptunian objects in a 2:3 orbital resonance with Neptune, which means that they orbit the Sun exactly twice while Neptune orbits the Sun three times. It orbits the Sun at a distance of 26.3β52.0 AU once ... | [
"(15875) 1996 TP66 β Physical properties\n\nhas a RR taxonomic class, with \"very red\" surface in the visible (rather than a \"neutral\" or \"grey-blue\" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660... |
(15875)_1996_TP66_2105748 | Summarize the 'Numbering and naming' part of '(15875) 1996 TP66'. | This minor planet was numbered by the Minor Planet Center on 26 July 2000 and received the number in the minor planet catalog (M.P.C. 40993). As of 2018, it has not been named. | [
"(15875) 1996 TP66 β Physical properties\n\nhas a RR taxonomic class, with \"very red\" surface in the visible (rather than a \"neutral\" or \"grey-blue\" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660... |
(15875)_1996_TP66_2105747 | What information does the article about '(15875) 1996 TP66' provide on 'Inside Neptune's orbit'? | In 2000, this object came closest to the Sun (perihelion) at 26.3 AU, and has since moved away to a distance of 29.2 AU by the end of 2018. This means that this small plutino is still well inside the orbit of Neptune which has a semi-major axis of 30.1 AU. Like Pluto, this plutino spends part of its orbit closer to the... | [
"(15875) 1996 TP66 β Physical properties\n\nhas a RR taxonomic class, with \"very red\" surface in the visible (rather than a \"neutral\" or \"grey-blue\" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660... |
(15875)_1996_TP66_2105751 | Describe the 'Rotation period' section of the article about '(15875) 1996 TP66'. | was part of a rotational lightcurve study which was published in the journal Nature in 1999. The photometric observations gave a brightness variation of no more than 0.12 magnitude, which is indicative of a rather spherical shape. As of 2018, the body's rotation period and pole remain unknown. | [
"(15875) 1996 TP66 β Physical properties\n\nhas a RR taxonomic class, with \"very red\" surface in the visible (rather than a \"neutral\" or \"grey-blue\" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660... |
(15875)_1996_TP66_2105745 | Reconstruct the content from the article about '(15875) 1996 TP66'. | , provisional designation, is a resonant trans-Neptunian object of the plutino population, located in the outermost region of the Solar System, approximately 154 km in diameter. It was discovered on 11 October 1996, by astronomers Jane Luu, David C. Jewitt and Chad Trujillo at the Mauna Kea Observatories, Hawaii, in th... | [
"(15875) 1996 TP66 β Physical properties\n\nhas a RR taxonomic class, with \"very red\" surface in the visible (rather than a \"neutral\" or \"grey-blue\" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660... |
(15875)_1996_TP66_2105750 | Explain what '(15875) 1996 TP66' covers in the 'Diameter and albedo' section. | According to the survey carried out by the Herschel Space Telescope using its PACS instrument, measures 154 kilometers in diameter and its surface has an albedo of 0.074. The results supersedes a previous study that gave a much larger diameter of 350 kilometers with a lower albedo of 0.03. According to Michael Brown, i... | [
"(15875) 1996 TP66 β Physical properties\n\nhas a RR taxonomic class, with \"very red\" surface in the visible (rather than a \"neutral\" or \"grey-blue\" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: BβV (1.050), VβR (0.660... |
(15977)_1998_MA11_15688070 | Describe the 'Numbering and naming' section of the article about '(15977) 1998 MA11'. | This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). , it has not been named. | [
"(15977) 1998 MA11 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). , it has not been named.",
"(15977) 1998 MA11 β Rotation period\n\nIn August 2013, Robert Stephens at the Center for Solar System Studies observed over three nights. However no m... |
(15977)_1998_MA11_15688072 | From the article on '(15977) 1998 MA11', restate the 'Rotation period' content. | In August 2013, Robert Stephens at the Center for Solar System Studies observed over three nights. However no meaningful rotational lightcurve could be determined, as the lightcurve's amplitude never varied more than 0.02 magnitude. A period of 11.17 hours was only derived for demonstration purpose (U=2-). In December... | [
"(15977) 1998 MA11 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). , it has not been named.",
"(15977) 1998 MA11 β Rotation period\n\nIn August 2013, Robert Stephens at the Center for Solar System Studies observed over three nights. However no m... |
(15977)_1998_MA11_15688073 | Reconstruct the content about 'Diameter and albedo' from the article on '(15977) 1998 MA11'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 43.53 and 51.53 kilometers in diameter and its surface has an albedo of 0.071 and 0.046, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo... | [
"(15977) 1998 MA11 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). , it has not been named.",
"(15977) 1998 MA11 β Rotation period\n\nIn August 2013, Robert Stephens at the Center for Solar System Studies observed over three nights. However no m... |
(15977)_1998_MA11_15688068 | Summarize the following section from the article on '(15977) 1998 MA11'. | , provisional designation:, is a Jupiter trojan from the Trojan camp, approximately 45 km in diameter. It was discovered on 19 June 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The suspected tumbler is also a slow rotator wit... | [
"(15977) 1998 MA11 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). , it has not been named.",
"(15977) 1998 MA11 β Rotation period\n\nIn August 2013, Robert Stephens at the Center for Solar System Studies observed over three nights. However no m... |
(15977)_1998_MA11_15688069 | Based on the article about '(15977) 1998 MA11', describe 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, 60Β° behind its orbit. It orbits the Sun at a distance of 4.9β5.4 AU once every 11 years and 10 months (4,309 days; semi-major axis of 5.18 AU). Its orbit has an eccentricity of 0... | [
"(15977) 1998 MA11 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). , it has not been named.",
"(15977) 1998 MA11 β Rotation period\n\nIn August 2013, Robert Stephens at the Center for Solar System Studies observed over three nights. However no m... |
(159857)_2004_LJ1_1179214 | Describe the 'Diameter and albedo' section of the article about '(159857) 2004 LJ1'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 2.47 kilomet... | [
"(159857) 2004 LJ1 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids o... |
(159857)_2004_LJ1_1179213 | What information does the article about '(159857) 2004 LJ1' provide on 'Rotation period'? | Three rotational lightcurves of have been obtained from photometric observations by Johanna Torppa, AdriΓ‘n GalΓ‘d and Brian Warner since 2004. Lightcurve analysis gave a consolidated rotation period of 2.7247 hours with a brightness amplitude between 0.15 and 0.59 magnitude (U=3). | [
"(159857) 2004 LJ1 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids o... |
(159857)_2004_LJ1_1179209 | Summarize the following section from the article on '(159857) 2004 LJ1'. | , provisional designation, is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 kilometers in diameter. The asteroid was discovered on 10 June 2004, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Sit... | [
"(159857) 2004 LJ1 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids o... |
(159857)_2004_LJ1_1179211 | What information does the article about '(159857) 2004 LJ1' provide on 'Close approaches'? | With an absolute magnitude of at least 15.4, is one of the brightest and presumably largest known potentially hazardous asteroid (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0168 AU, which translates into 6.5 lunar distances (LD). On 16 November 2038, this asteroid will make its closest ne... | [
"(159857) 2004 LJ1 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids o... |
(159857)_2004_LJ1_1179210 | From the article on '(159857) 2004 LJ1', restate the 'Orbit and classification' content. | is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects. The body orbits the Sun at a distance of 0.9β3.6 AU once every 3 years and 5 months (1,244 days; semi-major axis of 2.26 AU). Its orbit has an eccentricity of 0.59 and an incli... | [
"(159857) 2004 LJ1 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids o... |
(159857)_2004_LJ1_1179215 | Explain what '(159857) 2004 LJ1' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 30 June 2007. As of 2018, it has not been named. | [
"(159857) 2004 LJ1 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids o... |
(162058)_1997_AE12_20676097 | What information does the article about '(162058) 1997 AE12' provide? | is a stony, sub-kilometer asteroid and likely the slowest rotator known to exist. It is classified as near-Earth object of the Amor group and measures approximately 800 meters in diameter. The asteroid was discovered on 10 January 1997 by the Spacewatch survey at Kitt Peak National Observatory near Tucson, Arizona | [
"(162058) 1997 AE12\n\nis a stony, sub-kilometer asteroid and likely the slowest rotator known to exist. It is classified as near-Earth object of the Amor group and measures approximately 800 meters in diameter. The asteroid was discovered on 10 January 1997 by the Spacewatch survey at Kitt Peak National Observator... |
(162058)_1997_AE12_20676100 | Summarize the 'Spectral type' part of '(162058) 1997 AE12'. | is a rare Q-type asteroid with a very dark surface, reflecting only about 7% of the light it receives. It has also been described a common stony S-type asteroid. | [
"(162058) 1997 AE12\n\nis a stony, sub-kilometer asteroid and likely the slowest rotator known to exist. It is classified as near-Earth object of the Amor group and measures approximately 800 meters in diameter. The asteroid was discovered on 10 January 1997 by the Spacewatch survey at Kitt Peak National Observator... |
(162058)_1997_AE12_20676098 | Reconstruct the content about 'Orbit and classification' from the article on '(162058) 1997 AE12'. | is an Amor asteroid, a group of near-Earth object that approach the orbit of Earth from beyond, but do not cross it. It orbits the Sun at a distance of 1.1β3.7 AU once every 3 years and 8 months (1,330 days). Its orbit has an eccentricity of 0.55 and an inclination of 5Β° with respect to the ecliptic. Published by the D... | [
"(162058) 1997 AE12\n\nis a stony, sub-kilometer asteroid and likely the slowest rotator known to exist. It is classified as near-Earth object of the Amor group and measures approximately 800 meters in diameter. The asteroid was discovered on 10 January 1997 by the Spacewatch survey at Kitt Peak National Observator... |
(162058)_1997_AE12_20676102 | What does the article about '(162058) 1997 AE12' say regarding 'Diameter and albedo'? | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 0.847 kilometers in diameter and its surface has an albedo of 0.186. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 0.782 kilo... | [
"(162058) 1997 AE12\n\nis a stony, sub-kilometer asteroid and likely the slowest rotator known to exist. It is classified as near-Earth object of the Amor group and measures approximately 800 meters in diameter. The asteroid was discovered on 10 January 1997 by the Spacewatch survey at Kitt Peak National Observator... |
(162058)_1997_AE12_20676099 | From the article on '(162058) 1997 AE12', restate the 'Close approaches' content. | occasionally makes close approaches to Earth and Mars. It has an Earth minimum orbital intersection distance of 0.0881 AU, which is about 34.3 lunar distances. Its closest recorded approach to Earth took place on 30 August 2003, when the asteroid came within 0.1238 AU from Earth. It will come closer still on 8 October ... | [
"(162058) 1997 AE12\n\nis a stony, sub-kilometer asteroid and likely the slowest rotator known to exist. It is classified as near-Earth object of the Amor group and measures approximately 800 meters in diameter. The asteroid was discovered on 10 January 1997 by the Spacewatch survey at Kitt Peak National Observator... |
(162421)_2000_ET70_6013590 | Reconstruct the content about 'Diameter and albedo' from the article on '(162421) 2000 ET70'. | According to shape modeling of radar observations, the asteroid's overall dimensions are 2.6Γ2.2Γ2.1 kilometers. Based on an absolute magnitude of 18.2, this results in a notably low albedo of 0.018. More recent modeling combining radar, photometric, and infrared data gave and even more elongated shape of 2.9Γ2.2Γ1.5 k... | [
"(162421) 2000 ET70 β Diameter and albedo\n\nAccording to shape modeling of radar observations, the asteroid's overall dimensions are 2.6Γ2.2Γ2.1 kilometers. Based on an absolute magnitude of 18.2, this results in a notably low albedo of 0.018. More recent modeling combining radar, photometric, and infrared data ga... |
(162421)_2000_ET70_6013585 | What information does the article about '(162421) 2000 ET70' provide? | is a dark, elongated and oblate asteroid, classified as near-Earth object and potentially hazardous asteroid of the Aten group, approximately 2.2 kilometers in diameter. It was discovered on 8 March 2000, by astronomers of the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near ... | [
"(162421) 2000 ET70 β Diameter and albedo\n\nAccording to shape modeling of radar observations, the asteroid's overall dimensions are 2.6Γ2.2Γ2.1 kilometers. Based on an absolute magnitude of 18.2, this results in a notably low albedo of 0.018. More recent modeling combining radar, photometric, and infrared data ga... |
(162421)_2000_ET70_6013586 | Explain what '(162421) 2000 ET70' covers in the 'Orbit and classification' section. | orbits the Sun at a distance of 0.8β1.1 AU once every 11 months (336 days; semi-major axis of 0.95 AU). Its orbit has an eccentricity of 0.12 and an inclination of 22Β° with respect to the ecliptic. A first precovery was found in the Digitized Sky Survey from images taken at ESO's La Silla Observatory in February 1977. ... | [
"(162421) 2000 ET70 β Diameter and albedo\n\nAccording to shape modeling of radar observations, the asteroid's overall dimensions are 2.6Γ2.2Γ2.1 kilometers. Based on an absolute magnitude of 18.2, this results in a notably low albedo of 0.018. More recent modeling combining radar, photometric, and infrared data ga... |
(162421)_2000_ET70_6013589 | What does the article about '(162421) 2000 ET70' say regarding 'Rotation period, pole, and shape'? | During its close approach in February 2012, a rotational lightcurve of was obtained from photometric observations by a collaboration of astronomers from Uruguay, Australia, and the United States. Analysis of the lightcurve gave a period of 8.947 hours with a brightness amplitude of 0.60 magnitude (U=3-). Radar observat... | [
"(162421) 2000 ET70 β Diameter and albedo\n\nAccording to shape modeling of radar observations, the asteroid's overall dimensions are 2.6Γ2.2Γ2.1 kilometers. Based on an absolute magnitude of 18.2, this results in a notably low albedo of 0.018. More recent modeling combining radar, photometric, and infrared data ga... |
(162421)_2000_ET70_6013591 | What information does the article about '(162421) 2000 ET70' provide on 'Numbering and naming'? | This minor planet was numbered on 26 September 2007, after its orbital parameters had been sufficiently determined (M.P.C. 60670). As of 2018, it has not been named. | [
"(162421) 2000 ET70 β Diameter and albedo\n\nAccording to shape modeling of radar observations, the asteroid's overall dimensions are 2.6Γ2.2Γ2.1 kilometers. Based on an absolute magnitude of 18.2, this results in a notably low albedo of 0.018. More recent modeling combining radar, photometric, and infrared data ga... |
(163243)_2002_FB3_26066679 | Reconstruct the content about 'Close approaches' from the article on '(163243) 2002 FB3'. | The asteroid has an Earth minimum orbital intersection distance of 0.0034 AU, which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. | [
"(163243) 2002 FB3 β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0034 AU, which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size.",
"(163243) 2002 FB3 β Rotation period\n\nIn March 2016, a rotational li... |
(163243)_2002_FB3_26066681 | Based on the article about '(163243) 2002 FB3', describe the 'Rotation period' section. | In March 2016, a rotational lightcurve of this asteroid was obtained from photometric observations. Lightcurve analysis gave a rotation period of 6.231 hours with a brightness amplitude of 0.19 magnitude (U=2). | [
"(163243) 2002 FB3 β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0034 AU, which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size.",
"(163243) 2002 FB3 β Rotation period\n\nIn March 2016, a rotational li... |
(163243)_2002_FB3_26066677 | Summarize the following section from the article on '(163243) 2002 FB3'. | , provisional designation, is a stony asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Athen group, approximately 1.6 km in diameter. It was discovered on 18 March 2002, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Expe... | [
"(163243) 2002 FB3 β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0034 AU, which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size.",
"(163243) 2002 FB3 β Rotation period\n\nIn March 2016, a rotational li... |
(163243)_2002_FB3_26066683 | Explain what '(163243) 2002 FB3' covers in the 'Naming' section. | This minor planet was numbered by the MPC on 26 September 2007 (M.P.C. 60678). As of 2018, it has not been named. | [
"(163243) 2002 FB3 β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0034 AU, which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size.",
"(163243) 2002 FB3 β Rotation period\n\nIn March 2016, a rotational li... |
(163243)_2002_FB3_26066678 | Reconstruct the content about 'Orbit and classification' from the article on '(163243) 2002 FB3'. | is a member of the Athen group of asteroids. It orbits the Sun at a distance of 0.3β1.2 AU once every 8 months (243 days; semi-major axis of 0.76 AU). Its orbit has an eccentricity of 0.60 and an inclination of 20Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation a... | [
"(163243) 2002 FB3 β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0034 AU, which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size.",
"(163243) 2002 FB3 β Rotation period\n\nIn March 2016, a rotational li... |
(163348)_2002_NN4_3665338 | From the article on '(163348) 2002 NN4', restate the 'Diameter and albedo' content. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures (735) meters in diameter, and its surface has a dark albedo of (0.03). (The NEOWISE publication uses the designation G3348 for this asteroid. ) In 2016, astronomers using the European New Technology Teles... | [
"(163348) 2002 NN4 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures (735) meters in diameter, and its surface has a dark albedo of (0.03). (The NEOWISE publication uses the designation G3348 for this asteroid. ) In 2016, ast... |
(163348)_2002_NN4_3665337 | What does the article about '(163348) 2002 NN4' say regarding 'Physical characteristics'? | A spectroscopic survey of the small near-Earth asteroid population conducted by European astronomers determined that is an X-type asteroid. Because of the objects low albedo (see below), it would be considered a primitive P-type asteroid in the Tholen classification. | [
"(163348) 2002 NN4 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures (735) meters in diameter, and its surface has a dark albedo of (0.03). (The NEOWISE publication uses the designation G3348 for this asteroid. ) In 2016, ast... |
(163348)_2002_NN4_3665339 | From the article on '(163348) 2002 NN4', restate the 'Rotation period' content. | In August 2016, the first rotational lightcurve of was obtained from photometric observations over five nights by Brian Warner at the Center for Solar System Studies in California. Lightcurve analysis gave a rotation period of 14.5 hours with a high brightness variation of 0.74 magnitude, indicative of a highly elonga... | [
"(163348) 2002 NN4 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures (735) meters in diameter, and its surface has a dark albedo of (0.03). (The NEOWISE publication uses the designation G3348 for this asteroid. ) In 2016, ast... |
(163348)_2002_NN4_3665335 | Describe the content of the article about '(163348) 2002 NN4'. | (prov. designation: ) is a dark, sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group that flew by Earth on 6 June 2020. The highly elongated X-type asteroid has a rotation period of 14.5 hours and measures approximately 0.7 km in diameter. It was discovered by LINEAR at the Lincoln Labo... | [
"(163348) 2002 NN4 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures (735) meters in diameter, and its surface has a dark albedo of (0.03). (The NEOWISE publication uses the designation G3348 for this asteroid. ) In 2016, ast... |
(163348)_2002_NN4_3665336 | What does the article about '(163348) 2002 NN4' say regarding 'Orbit'? | flew by Earth on 6 June 2020, passing 0.034 AU from Earth. The asteroid had been recovered two days earlier on 4 June 2020. By 11 June 2020, the asteroid had brightened to apparent magnitude 14.4, which is roughly the brightness of Pluto. Being a member of the Aten asteroids, orbits the Sun at a distance of 0.50β1.26 ... | [
"(163348) 2002 NN4 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures (735) meters in diameter, and its surface has a dark albedo of (0.03). (The NEOWISE publication uses the designation G3348 for this asteroid. ) In 2016, ast... |
(163899)_2003_SD220_19805670 | What information does the article about '(163899) 2003 SD220' provide on '2021'? | will pass at a distance of 14.1 lunar distances (0.03628 AU) on December 17, 2021. It was observed by the Goldstone Solar System Radar from November to December 2021. | [
"(163899) 2003 SD220 β 2021\n\nwill pass at a distance of 14.1 lunar distances (0.03628 AU) on December 17, 2021. It was observed by the Goldstone Solar System Radar from November to December 2021.",
"(163899) 2003 SD220 β 2015\n\nIt was observed in December 2015 at a distance of 28.3 lunar distances (0.07296 AU)... |
(163899)_2003_SD220_19805668 | What does the article about '(163899) 2003 SD220' say regarding '2015'? | It was observed in December 2015 at a distance of 28.3 lunar distances (0.07296 AU) on December 24, and its brightest was 15.22 magnitude on December 16. It showed an elongated shape, up to 2 km wide, described as being shaped like a sweet potato. | [
"(163899) 2003 SD220 β 2021\n\nwill pass at a distance of 14.1 lunar distances (0.03628 AU) on December 17, 2021. It was observed by the Goldstone Solar System Radar from November to December 2021.",
"(163899) 2003 SD220 β 2015\n\nIt was observed in December 2015 at a distance of 28.3 lunar distances (0.07296 AU)... |
(163899)_2003_SD220_19805667 | Based on the article about '(163899) 2003 SD220', describe the 'Earth flybys 2015β2027' section. | It passed about 28 lunar distances (LD) from the Earth on 25 December 2015. It came within about 7 LD (0.0189 AU) on 22 December 2018. Its peak brightness was about 13.13 magnitude on 16 December 2018. Observations are planned for favorable flybys in 2021, 2024, and 2027. It will pass with 14 LD (0.0363 AU) on 17 Decem... | [
"(163899) 2003 SD220 β 2021\n\nwill pass at a distance of 14.1 lunar distances (0.03628 AU) on December 17, 2021. It was observed by the Goldstone Solar System Radar from November to December 2021.",
"(163899) 2003 SD220 β 2015\n\nIt was observed in December 2015 at a distance of 28.3 lunar distances (0.07296 AU)... |
(163899)_2003_SD220_19805669 | Reconstruct the content about 'Closest flyby 2018' from the article on '(163899) 2003 SD220'. | passed its closest distance of 7.34 LD (0.01899 AU) on 22 December 2018. It was on the list of Goldstone targets for December 2018 to gain more information for the Near-Earth Object Human Space Flight Accessible Targets Study (NHATS). Its peak brightness was about 13.1 magnitude on 16 December 2018, moving south from U... | [
"(163899) 2003 SD220 β 2021\n\nwill pass at a distance of 14.1 lunar distances (0.03628 AU) on December 17, 2021. It was observed by the Goldstone Solar System Radar from November to December 2021.",
"(163899) 2003 SD220 β 2015\n\nIt was observed in December 2015 at a distance of 28.3 lunar distances (0.07296 AU)... |
(163899)_2003_SD220_19805666 | Reconstruct the content from the article about '(163899) 2003 SD220'. | is a sub-kilometer asteroid and tumbling slow rotator, classified as near-Earth object and potentially hazardous asteroid of the Aten group, which orbit the Sun between Venus and Earth. Its orbital period of 0.75 years means that it orbits the sun about 4 times for every 3 of the Earth. It was discovered on 29 Septembe... | [
"(163899) 2003 SD220 β 2021\n\nwill pass at a distance of 14.1 lunar distances (0.03628 AU) on December 17, 2021. It was observed by the Goldstone Solar System Radar from November to December 2021.",
"(163899) 2003 SD220 β 2015\n\nIt was observed in December 2015 at a distance of 28.3 lunar distances (0.07296 AU)... |
(164121)_2003_YT1_26180567 | Summarize the 'Rotation period' part of '(164121) 2003 YT1'. | Several rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude. | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(164121)_2003_YT1_26180565 | Summarize the 'Meteor stream' part of '(164121) 2003 YT1'. | On 28 April 2017, a 2.7 cm fragment of is suspected of having impacted Earth creating a fireball over Kyoto, Japan. The fragment would have broken off the parent body within the last ten thousand years. | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(164121)_2003_YT1_26180568 | What information does the article about '(164121) 2003 YT1' provide on 'Diameter and albedo'? | According to radar observations with the Arecibo Observatory and the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures between 1.0 and 1.717 kilometers in diameter and its surface has an albedo between 0.198 and 0.4861. The Collaborative Asteroid Lightcurve ... | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(164121)_2003_YT1_26180570 | Explain what '(164121) 2003 YT1' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 26 September 2007 (M.P.C. 60686). As of 2018, it has not been named. | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(164121)_2003_YT1_26180563 | Based on the article about '(164121) 2003 YT1', describe the 'Orbit and classification' section. | is a member of the Earth-crossing group of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It orbits the Sun at a distance of 0.8β1.4 AU once every 1 years and 2 months (427 days; semi-major axis of 1.11 AU). Its orbit has an eccentricity of 0.29 and an inclinatio... | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(164121)_2003_YT1_26180569 | From the article on '(164121) 2003 YT1', restate the 'Satellite' content. | The Arecibo radar observations in May 2004 revealed that is a synchronous binary asteroid. Follow-up observations confirmed a 210-meter sized minor-planet moon orbiting its primary every 30 hours at a distance of 2.7 km. | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(164121)_2003_YT1_26180564 | Summarize the 'Close approaches and Torino rating' part of '(164121) 2003 YT1'. | The asteroid has an Earth minimum orbital intersection distance of 0.0027 AU, which corresponds to 1.05 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. On the Torino Scale, this object was rated level 1 on 27 December 2003 with an observation arc of 8.7 days. It was rem... | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(164121)_2003_YT1_26180562 | Summarize the following section from the article on '(164121) 2003 YT1'. | , provisional designation, is a bright asteroid and synchronous binary system on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 2 km in diameter. It was discovered on 18 December 2003, by astronomers with the Catalina Sky Survey at the Cat... | [
"(164121) 2003 YT1 β Rotation period\n\nSeveral rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.",
"(164121) 2003 YT... |
(16882)_1998_BO13_27707095 | Summarize the 'Orbit and classification' part of '(16882) 1998 BO13'. | is a non-family asteroid from the main belt's background population, and a member of the small group of Zhongguo asteroids, located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits of the Zhongguos are stable over half a billion year... | [
"(16882) 1998 BO13 β Orbit and classification\n\nis a non-family asteroid from the main belt's background population, and a member of the small group of Zhongguo asteroids, located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits... |
(16882)_1998_BO13_27707094 | Describe the content of the article about '(16882) 1998 BO13'. | , provisional designation, is a dark Zhongguo asteroid from the background population in the outermost region of the asteroid belt, approximately 10 km in diameter. It was discovered on 24 January 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near ... | [
"(16882) 1998 BO13 β Orbit and classification\n\nis a non-family asteroid from the main belt's background population, and a member of the small group of Zhongguo asteroids, located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits... |
(16882)_1998_BO13_27707096 | From the article on '(16882) 1998 BO13', restate the 'Physical characteristics' content. | has an absolute magnitude of 13.5. As of 2018, no rotational lightcurve for this asteroid has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. | [
"(16882) 1998 BO13 β Orbit and classification\n\nis a non-family asteroid from the main belt's background population, and a member of the small group of Zhongguo asteroids, located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits... |
(16882)_1998_BO13_27707097 | Explain what '(16882) 1998 BO13' covers in the 'Diameter and albedo' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 9.827 kilometers in diameter and its surface has an albedo of 0.061, which is rather typical for the abundant carbonaceous C-type asteroids in the outer main-belt. | [
"(16882) 1998 BO13 β Orbit and classification\n\nis a non-family asteroid from the main belt's background population, and a member of the small group of Zhongguo asteroids, located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits... |
(16882)_1998_BO13_27707098 | Summarize the 'Numbering and naming' part of '(16882) 1998 BO13'. | This minor planet was numbered by the Minor Planet Center on 13 September 2000, after its orbit had sufficiently been secured (M.P.C. 41165). As of 2018, it has not been named. | [
"(16882) 1998 BO13 β Orbit and classification\n\nis a non-family asteroid from the main belt's background population, and a member of the small group of Zhongguo asteroids, located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits... |
(16960)_1998_QS52_1009777 | Describe the 'Rotation period' section of the article about '(16960) 1998 QS52'. | In 2008, two rotational lightcurves of were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotation period of 5.789 and 5.8 hours with a brig... | [
"(16960) 1998 QS52 β Rotation period\n\nIn 2008, two rotational lightcurves of were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotati... |
(16960)_1998_QS52_1009775 | Describe the 'Close approaches' section of the article about '(16960) 1998 QS52'. | With an absolute magnitude of 14.3, is one of the brightest and largest known potentially hazardous asteroid (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0144 AU, which corresponds to 5.6 lunar distances. Its eccentric orbit leads to close approaches with Mercury and Venus and carries it b... | [
"(16960) 1998 QS52 β Rotation period\n\nIn 2008, two rotational lightcurves of were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotati... |
(16960)_1998_QS52_1009776 | From the article on '(16960) 1998 QS52', restate the 'Physical characteristics' content. | In the SMASS classification, is a Sq-subtype, that transitions between the stony S- and Q-type asteroids. Observers at the NASA Infrared Telescope Facility have also characterized this body as an Sr-type, which transitions to the rare R-type asteroids. | [
"(16960) 1998 QS52 β Rotation period\n\nIn 2008, two rotational lightcurves of were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotati... |
(16960)_1998_QS52_1009773 | Summarize the following section from the article on '(16960) 1998 QS52'. | (prov. designation: ) is a stony asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 4.1 km in diameter. It was discovered on 25 August 1998, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near S... | [
"(16960) 1998 QS52 β Rotation period\n\nIn 2008, two rotational lightcurves of were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotati... |
(16960)_1998_QS52_1009778 | What information does the article about '(16960) 1998 QS52' provide on 'Diameter and albedo'? | has not been observed by any of the space-based surveys such as IRAS, Akari or the Wide-field Infrared Survey Explorer. The Collaborative Asteroid Lightcurve Link assumes a stony standard albedo of 0.20 for its surface, and calculates a diameter of 4.10 kilometers based on an absolute magnitude of 14.3. | [
"(16960) 1998 QS52 β Rotation period\n\nIn 2008, two rotational lightcurves of were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotati... |
(16960)_1998_QS52_1009774 | Summarize the 'Orbit and classification' part of '(16960) 1998 QS52'. | is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects. It orbits the Sun at a distance of 0.31β4.1 AU once every 3 years and 3 months (1,194 days; semi-major axis of 2.20 AU). Its orbit has an exceptionally high eccentricity of 0.8... | [
"(16960) 1998 QS52 β Rotation period\n\nIn 2008, two rotational lightcurves of were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotati... |
(172034)_2001_WR1_12492026 | Summarize the 'Hayabusa2 mission' part of '(172034) 2001 WR1'. | is currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample capsule in December 2020, it is expected to retain 30 kg of xenon propellant, which can be used to extend its service and flyby new targets to explore. | [
"(172034) 2001 WR1 β Physical characteristics\n\nhas been characterized as a common, stony S-type asteroid.",
"(172034) 2001 WR1 β Hayabusa2 mission\n\nis currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample ... |
(172034)_2001_WR1_12492027 | From the article on '(172034) 2001 WR1', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 24 December 2007 (M.P.C. 61443). , it has not been named. | [
"(172034) 2001 WR1 β Physical characteristics\n\nhas been characterized as a common, stony S-type asteroid.",
"(172034) 2001 WR1 β Hayabusa2 mission\n\nis currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample ... |
(172034)_2001_WR1_12492029 | What does the article about '(172034) 2001 WR1' say regarding 'Rotation period'? | In March 2018, a rotational lightcurve of was obtained from photometric observations by Brian Warner at the Palmer Divide Station in California. Lightcurve analysis gave a rotation period of 8.048 hours with a brightness amplitude of 0.95 magnitude (U=3), indicative of a non-spherical shape. | [
"(172034) 2001 WR1 β Physical characteristics\n\nhas been characterized as a common, stony S-type asteroid.",
"(172034) 2001 WR1 β Hayabusa2 mission\n\nis currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample ... |
(172034)_2001_WR1_12492024 | Summarize the 'Orbit and classification' part of '(172034) 2001 WR1'. | is an Amor asteroid β a subgroup of near-Earth asteroids that approach the orbit of Earth from beyond, but do not cross it. The object orbits the Sun at a distance of 1.02β1.54 AU once every 17 months (527 days; semi-major axis of 1.28 AU). Its orbit has an eccentricity of 0.20 and an inclination of 25Β° with respect to... | [
"(172034) 2001 WR1 β Physical characteristics\n\nhas been characterized as a common, stony S-type asteroid.",
"(172034) 2001 WR1 β Hayabusa2 mission\n\nis currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample ... |
(172034)_2001_WR1_12492023 | Reconstruct the content from the article about '(172034) 2001 WR1'. | , provisional designation:, is a sub-kilometer near-Earth object of the Amor group, approximately 650 m in diameter. The S-type asteroid has been identified as a potential flyby target of the Hayabusa2 mission. It was discovered on 17 November 2001, by astronomers with the Lincoln Near-Earth Asteroid Research at the Li... | [
"(172034) 2001 WR1 β Physical characteristics\n\nhas been characterized as a common, stony S-type asteroid.",
"(172034) 2001 WR1 β Hayabusa2 mission\n\nis currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample ... |
(172034)_2001_WR1_12492025 | Based on the article about '(172034) 2001 WR1', describe the 'Close encounters' section. | has an Earth minimum orbital intersection distance of 0.0747 AU which corresponds to 29.1 lunar distances. In September 1926, it approached Earth to 0.1496 AU, its closest approach of all close encounters since 1900. Only in September 2199, it will approach Earth at a similar distance of 0.1514 AU. | [
"(172034) 2001 WR1 β Physical characteristics\n\nhas been characterized as a common, stony S-type asteroid.",
"(172034) 2001 WR1 β Hayabusa2 mission\n\nis currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample ... |
(172034)_2001_WR1_12492030 | Based on the article about '(172034) 2001 WR1', describe the 'Diameter and albedo' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, has an albedo of 0.34 and measures 0.63 and 0.66 kilometers in diameter, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of... | [
"(172034) 2001 WR1 β Physical characteristics\n\nhas been characterized as a common, stony S-type asteroid.",
"(172034) 2001 WR1 β Hayabusa2 mission\n\nis currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample ... |
(175706)_1996_FG3_24229002 | From the article on '(175706) 1996 FG3', restate the 'Lightcurves' content. | Several rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Pravec, Petr Scheirich and Stefano Mottola, as well as by the Very Large Telescope VISR instrument. Lightcurve analysis gave a well-defined rotation period of 3.594 to 3.595 hours with a brightness vari... | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(175706)_1996_FG3_24228999 | Based on the article about '(175706) 1996 FG3', describe the 'Target of planned Chinese mission' section. | China plans to land a probe on after 2020 as part of its asteroid exploration mission. The mission includes plans for fly-by of three asteroids (one of them is 99942 Apophis), and land on to conduct in situ sampling analysis on the surface, according to Ji Jianghui, a researcher at the Purple Mountain Observatory of th... | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(175706)_1996_FG3_24229004 | Describe the 'Satellite' section of the article about '(175706) 1996 FG3'. | During the photometric observations in December 1998, the binary nature of this asteroid was revealed. It was the first binary near-Earth asteroid for which eclipse events were detected in the visible spectrum. The binary system has a diameter ratio of 0.28, a density of 1.4 g/cm3, and an ecliptic latitude of -84Β° for ... | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(175706)_1996_FG3_24228997 | Describe the 'Orbit and classification' section of the article about '(175706) 1996 FG3'. | orbits the Sun at a distance of 0.7β1.4 AU once every 1 years and 1 month (395 days; semi-major axis of 1.05 AU). Its orbit has an eccentricity of 0.35 and an inclination of 2Β° with respect to the ecliptic. It has an Earth minimum orbital intersection distance of 0.0283 AU, which corresponds to 11.0 lunar distances. In... | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(175706)_1996_FG3_24228998 | What information does the article about '(175706) 1996 FG3' provide on 'Target of rejected Marco Polo mission'? | Due to its binary nature and its low delta-v heliocentric orbit (also see Hohmann transfer orbit), this asteroid was selected for MarcoPolo-R, which was the Marco Polo spacecraft first proposed mission. MarcoPolo-R was originally selected for the assessment study phase in the M3 slot of ESA's Cosmic Vision program, but... | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(175706)_1996_FG3_24229003 | Explain what '(175706) 1996 FG3' covers in the 'Diameter and albedo' section. | According to numerous observations, including the EXPLORENEOs survey, NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission and the Spitzer Space Telescope, the asteroid measures between 1.55 and 1.90 kilometers in diameter and its surface has a low albedo of 0.03 to 0.05. The Collaborative Ast... | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(175706)_1996_FG3_24229000 | Describe the 'Numbering and naming' section of the article about '(175706) 1996 FG3'. | This minor planet was numbered by the Minor Planet Center on 21 February 2008. As of 2018, it has not been named. | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(175706)_1996_FG3_24228996 | Summarize the following section from the article on '(175706) 1996 FG3'. | is a carbonaceous asteroid and binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.7 km in diameter. The primary has a spheroidal shape. Its minor-planet moon measures approximately 490 m in diameter. It was discovered on 24 March 1996, by Australian as... | [
"(175706) 1996 FG3 β Physical characteristics\n\nThe carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.",
"(175706) 1996 FG3 β Lightcurves\n\nSeveral rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Prav... |
(181902)_1999_RD215_3721049 | What information does the article about '(181902) 1999 RD215' provide on 'Orbit and classification'? | orbits from the center of the Kuiper belt to well beyond into the scattered disc. It orbits the Sun at a distance of 37.5β204.4 AU once every 1330 years and 7 months (485,993 days; semi-major axis of 121 AU). Its orbit has an eccentricity of 0.69 and an inclination of 26Β° with respect to the ecliptic. The body's observ... | [
"(181902) 1999 RD215 β Orbit and classification\n\norbits from the center of the Kuiper belt to well beyond into the scattered disc. It orbits the Sun at a distance of 37.5β204.4 AU once every 1330 years and 7 months (485,993 days; semi-major axis of 121 AU). Its orbit has an eccentricity of 0.69 and an inclination... |
(181902)_1999_RD215_3721050 | Describe the 'Diameter and albedo' section of the article about '(181902) 1999 RD215'. | According to the Johnston's Archive and Michael Brown, measures 147 and 148 kilometers in diameter, and its surface has an estimated albedo of 0.09 and 0.08, respectively. | [
"(181902) 1999 RD215 β Orbit and classification\n\norbits from the center of the Kuiper belt to well beyond into the scattered disc. It orbits the Sun at a distance of 37.5β204.4 AU once every 1330 years and 7 months (485,993 days; semi-major axis of 121 AU). Its orbit has an eccentricity of 0.69 and an inclination... |
(181902)_1999_RD215_3721048 | Describe the content of the article about '(181902) 1999 RD215'. | is a trans-Neptunian object of the scattered disc, approximately 148 kilometers in diameter. It was discovered on 6 September 1999, by American astronomers Chad Trujillo, Jane Luu, and David Jewitt at the Mauna Kea Observatories, Hawaii. | [
"(181902) 1999 RD215 β Orbit and classification\n\norbits from the center of the Kuiper belt to well beyond into the scattered disc. It orbits the Sun at a distance of 37.5β204.4 AU once every 1330 years and 7 months (485,993 days; semi-major axis of 121 AU). Its orbit has an eccentricity of 0.69 and an inclination... |
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