id string | question string | answer string | documents list |
|---|---|---|---|
(55637)_2002_UX25_23681084 | What information does the article about '(55637) 2002 UX25' provide on 'Composition'? | With a density of 0.82 g/cm3, assuming that the primary and satellite have the same density, is one of the largest known solid objects in the Solar System that is less dense than water. Why this should be is not well understood, because objects of its size in the Kuiper belt often contain a fair amount of rock and are ... | [
"(55637) 2002 UX25\n\nis a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3. has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it t... |
(55637)_2002_UX25_23681081 | Explain what '(55637) 2002 UX25' covers in the 'Numbering and naming' section. | This minor planet was numbered (55637) by the Minor Planet Center on 16 February 2003 (M.P.C. 47763). , it has not been named. | [
"(55637) 2002 UX25\n\nis a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3. has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it t... |
(55637)_2002_UX25_23681083 | From the article on '(55637) 2002 UX25', restate the 'Physical characteristics' content. | A variability of the visual brightness was detected which could be fit to a period of 14.38 or 16.78 h (depending on a single-peaked or double peaked curve). The light-curve amplitude is ΔM = 0.21. The analysis of combined thermal radiometry of from measurements by the Spitzer Space Telescope and Herschel Space Telesco... | [
"(55637) 2002 UX25\n\nis a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3. has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it t... |
(55637)_2002_UX25_23681082 | From the article on '(55637) 2002 UX25', restate the 'Classification' content. | has a perihelion of 36.7 AU, which it will next reach in 2065. As of 2020, is 40 AU from the Sun. The Minor Planet Center classifies as a cubewano while the Deep Ecliptic Survey (DES) classifies it as scattered-extended. The DES using a 10 My integration (last observation: 2009-10-22) shows it with a minimum perihelion... | [
"(55637) 2002 UX25\n\nis a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3. has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it t... |
(55638)_2002_VE95_24320429 | Describe the 'Color and composition' section of the article about '(55638) 2002 VE95'. | In the visible light, has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively. The near-infrared spectrum of is flat with two distinct absorption bands of water ice at 1.5 and 2.0 μm. There is the third feature near ... | [
"(55638) 2002 VE95 — Color and composition\n\nIn the visible light, has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively. The near-infrared spectrum of is flat with two distinct absorption bands of water ice a... |
(55638)_2002_VE95_24320427 | From the article on '(55638) 2002 VE95', restate the 'Rotation period' content. | The rotation period of is poorly defined and has ambiguous results with multiple alternative period solutions in between 4.90 and 10 hours. In December 2002, a rotational lightcurve of this object was obtained from photometric observations by astromomers from the Sierra Nevada Observatory in Spain. Lightcurve analysis... | [
"(55638) 2002 VE95 — Color and composition\n\nIn the visible light, has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively. The near-infrared spectrum of is flat with two distinct absorption bands of water ice a... |
(55638)_2002_VE95_24320426 | What does the article about '(55638) 2002 VE95' say regarding 'Numbering and naming'? | was numbered (55638) by the Minor Planet Center on 16 February 2003 (M.P.C. 47763). , it has not been named. According to the established naming conventions for plutinos, it will be named after a mythological figure from the underworld. | [
"(55638) 2002 VE95 — Color and composition\n\nIn the visible light, has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively. The near-infrared spectrum of is flat with two distinct absorption bands of water ice a... |
(55638)_2002_VE95_24320428 | Reconstruct the content about 'Diameter and albedo' from the article on '(55638) 2002 VE95'. | In 2010, observations with the Herschel Space Telescope, using its PACS instrument to measure the object's thermal radiation, gave a mean-diameter of 249.8 km with a relatively high albedo of 0.149 for an absolute magnitude of 5.7. In addition, an asteroid occultations on 3 December 2015, gave a best-fit ellipse dimens... | [
"(55638) 2002 VE95 — Color and composition\n\nIn the visible light, has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively. The near-infrared spectrum of is flat with two distinct absorption bands of water ice a... |
(55638)_2002_VE95_24320424 | Describe the content of the article about '(55638) 2002 VE95'. | , prov. designation:, is a trans-Neptunian object from the outermost region of the Solar System. It was discovered on 14 November 2002, by astronomers with the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This resonant trans-Neptunian object is a member of the plutino po... | [
"(55638) 2002 VE95 — Color and composition\n\nIn the visible light, has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively. The near-infrared spectrum of is flat with two distinct absorption bands of water ice a... |
(55638)_2002_VE95_24320425 | Based on the article about '(55638) 2002 VE95', describe the 'Orbit and classification' section. | belongs to the plutino population, named after its largest member, Pluto. Plutinos are resonant trans-Neptunian objects, that are locked in a stable 2:3 mean-motion resonance with Neptune, orbiting the Sun twice for every three orbits Neptune does. They form a significantly large part of the inner Kuiper belt, as hundr... | [
"(55638) 2002 VE95 — Color and composition\n\nIn the visible light, has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively. The near-infrared spectrum of is flat with two distinct absorption bands of water ice a... |
(5645)_1990_SP_23818733 | What information does the article about '(5645) 1990 SP' provide on 'Orbit and classification'? | The asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic. | [
"(5645) 1990 SP — Orbit and classification\n\nThe asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.",
"(5645) 1990 SP — Rotation\n\nIn April 2002, Czech astronomer Petr Prave... |
(5645)_1990_SP_23818737 | What information does the article about '(5645) 1990 SP' provide on 'Rotation'? | In April 2002, Czech astronomer Petr Pravec obtained a rotational lightcurve from a photometric observations, which gave a relatively long period of 30.39 hours with a brightness variation of 0.7 in magnitude (U=2). The observations have also shown that the body is most likely in a tumbling motion. | [
"(5645) 1990 SP — Orbit and classification\n\nThe asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.",
"(5645) 1990 SP — Rotation\n\nIn April 2002, Czech astronomer Petr Prave... |
(5645)_1990_SP_23818735 | Explain what '(5645) 1990 SP' covers in the 'Precovery' section. | Published by the Digitized Sky Survey (DSS), a first precovery was taken at the discovering observatory in 1974, extending the asteroid's observation arc by 16 years prior to its discovery. | [
"(5645) 1990 SP — Orbit and classification\n\nThe asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.",
"(5645) 1990 SP — Rotation\n\nIn April 2002, Czech astronomer Petr Prave... |
(5645)_1990_SP_23818734 | Based on the article about '(5645) 1990 SP', describe the 'Close approaches' section. | This near-Earth asteroid has an Earth minimum orbit intersection distance of 0.055 AU, only slightly above the threshold minimum distance of 19.5 lunar distances (0.05 AU) to make it a potentially hazardous object. It also makes close approaches to Mars. On 14 April 1969, it passed the Red Planet at only 0.013 AU. | [
"(5645) 1990 SP — Orbit and classification\n\nThe asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.",
"(5645) 1990 SP — Rotation\n\nIn April 2002, Czech astronomer Petr Prave... |
(5645)_1990_SP_23818738 | Explain what '(5645) 1990 SP' covers in the 'Diameter and albedo' section. | Estimates for the body's diameter range from 1.6 to 2.2 kilometers with an albedo for its surface between 0.06 and 0.12, according to observations made by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and by the Spitzer Space Telescope. The Collaborative Asteroid Lightcurve Link takes the revised WI... | [
"(5645) 1990 SP — Orbit and classification\n\nThe asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.",
"(5645) 1990 SP — Rotation\n\nIn April 2002, Czech astronomer Petr Prave... |
(5645)_1990_SP_23818732 | Describe the content of the article about '(5645) 1990 SP'. | (5645) 1990 SP is an eccentric and tumbling asteroid, classified as near-Earth object of the Apollo group, approximately 1.7 kilometers in diameter. It was discovered on 20 September 1990, by Scottish–Australian astronomer Robert McNaught at the Siding Spring Observatory in Canberra, Australia. | [
"(5645) 1990 SP — Orbit and classification\n\nThe asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.",
"(5645) 1990 SP — Rotation\n\nIn April 2002, Czech astronomer Petr Prave... |
(5645)_1990_SP_23818736 | Reconstruct the content about 'Physical characteristics' from the article on '(5645) 1990 SP'. | The stony S-type asteroid is also characterized as a P-type, based on post-cryogenic observations by the Spitzer Space Telescope, while observations at the NASA Infrared Telescope Facility using its SpeX instrument during a follow-up campaign of the Spitzer-observed objects between 2009 and 2012, gave it a C/X/T spectr... | [
"(5645) 1990 SP — Orbit and classification\n\nThe asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.",
"(5645) 1990 SP — Rotation\n\nIn April 2002, Czech astronomer Petr Prave... |
(5646)_1990_TR_23818917 | What does the article about '(5646) 1990 TR' say regarding 'Orbit'? | The asteroid orbits the Sun at a distance of 1.2–3.1 AU once every 3 years and 2 months (1,147 days). Its orbit has an eccentricity of 0.44 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory, five months prior to its offic... | [
"(5646) 1990 TR — Orbit\n\nThe asteroid orbits the Sun at a distance of 1.2–3.1 AU once every 3 years and 2 months (1,147 days). Its orbit has an eccentricity of 0.44 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory,... |
(5646)_1990_TR_23818918 | Based on the article about '(5646) 1990 TR', describe the 'Lightcurve' section. | In December 2012, the so far best rated rotational lightcurve was obtained by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 3.1999 hours with a brightness variation of 0.12 magnitude (U=3). Photometric observations also gave a period of 19.4... | [
"(5646) 1990 TR — Orbit\n\nThe asteroid orbits the Sun at a distance of 1.2–3.1 AU once every 3 years and 2 months (1,147 days). Its orbit has an eccentricity of 0.44 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory,... |
(5646)_1990_TR_23818919 | Explain what '(5646) 1990 TR' covers in the 'Diameter and albedo' section. | According to the surveys carried out by the Spitzer Space Telescope and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures 2.03 and 2.723 kilometers in diameter and its surface has an albedo of 0.19 and 0.66. The Collaborative Asteroid Lightcurve Link assumes an albedo... | [
"(5646) 1990 TR — Orbit\n\nThe asteroid orbits the Sun at a distance of 1.2–3.1 AU once every 3 years and 2 months (1,147 days). Its orbit has an eccentricity of 0.44 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory,... |
(5646)_1990_TR_23818916 | Describe the content of the article about '(5646) 1990 TR'. | is a probable rare-type binary asteroid classified as near-Earth object of the Amor group, approximately 2.3 kilometers in diameter. It was discovered on 11 October 1990, by Japanese astronomers Seiji Ueda and Hiroshi Kaneda at Kushiro Observatory near Kushiro, in eastern Hokkaido, Japan. | [
"(5646) 1990 TR — Orbit\n\nThe asteroid orbits the Sun at a distance of 1.2–3.1 AU once every 3 years and 2 months (1,147 days). Its orbit has an eccentricity of 0.44 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory,... |
(574372)_2010_JO179_2712587 | Summarize the 'Diameter and albedo' part of '(574372) 2010 JO179'. | The object's mean diameter has been estimated to measure 574 and 735 kilometers, with an assumed albedo of 0.09, by Michael Brown and the Johnston's Archive respectively, while the discoverers estimate a diameter of 600–900 kilometers with an estimated albedo of 0.21 to 0.07. | [
"(574372) 2010 JO179 — Diameter and albedo\n\nThe object's mean diameter has been estimated to measure 574 and 735 kilometers, with an assumed albedo of 0.09, by Michael Brown and the Johnston's Archive respectively, while the discoverers estimate a diameter of 600–900 kilometers with an estimated albedo of 0.21 to... |
(574372)_2010_JO179_2712586 | From the article on '(574372) 2010 JO179', restate the 'Photometry' content. | Photometric observations of gave a monomodal lightcurve with slow rotation period of 30.6 hours, suggesting a rather spherical shape with significant albedo patchiness. An alternative period solution of a bimodal lightcurve is considered less likely. It would double the period and imply an ellipsoidal shape with an ax... | [
"(574372) 2010 JO179 — Diameter and albedo\n\nThe object's mean diameter has been estimated to measure 574 and 735 kilometers, with an assumed albedo of 0.09, by Michael Brown and the Johnston's Archive respectively, while the discoverers estimate a diameter of 600–900 kilometers with an estimated albedo of 0.21 to... |
(574372)_2010_JO179_2712584 | Explain what '(574372) 2010 JO179' covers in the 'First observation and orbit' section. | The Minor Planet Center credits the object's first official observation on 10 May 2010 to Pan-STARRS at Haleakala Observatory, Hawaii, United States. The observations were made by Pan-STARRS Outer Solar System Survey. There are 4 February 1951 precovery images from the Palomar Observatory Sky Survey, extending the obse... | [
"(574372) 2010 JO179 — Diameter and albedo\n\nThe object's mean diameter has been estimated to measure 574 and 735 kilometers, with an assumed albedo of 0.09, by Michael Brown and the Johnston's Archive respectively, while the discoverers estimate a diameter of 600–900 kilometers with an estimated albedo of 0.21 to... |
(574372)_2010_JO179_2712583 | Summarize the following section from the article on '(574372) 2010 JO179'. | , provisional designation:, is a large, high-order resonant trans-Neptunian object in the outermost regions of the Solar System, approximately 700 km in diameter. Long-term observations suggest that the object is in a meta-stable 5:21 resonance with Neptune. Other sources classify it as a scattered disc object. It is p... | [
"(574372) 2010 JO179 — Diameter and albedo\n\nThe object's mean diameter has been estimated to measure 574 and 735 kilometers, with an assumed albedo of 0.09, by Michael Brown and the Johnston's Archive respectively, while the discoverers estimate a diameter of 600–900 kilometers with an estimated albedo of 0.21 to... |
(5836)_1993_MF_26468352 | Summarize the following section from the article on '(5836) 1993 MF'. | is a highly eccentric, stony asteroid, classified as a near-Earth object of the Amor group of asteroids, approximately 3 kilometers in diameter. It was discovered on 22 June 1993, by American astronomers Eleanor Helin and Kenneth Lawrence at the U.S. Palomar Observatory in California. | [
"(5836) 1993 MF\n\nis a highly eccentric, stony asteroid, classified as a near-Earth object of the Amor group of asteroids, approximately 3 kilometers in diameter. It was discovered on 22 June 1993, by American astronomers Eleanor Helin and Kenneth Lawrence at the U.S. Palomar Observatory in California.",
"(5836)... |
(5836)_1993_MF_26468353 | Summarize the 'Classification and orbit' part of '(5836) 1993 MF'. | The stony S-type asteroid orbits the Sun at a distance of 1.1–3.7 AU once every 3 years and 10 months (1,392 days). Its orbit has an eccentricity of 0.54 and an inclination of 8° with respect to the ecliptic. It has an Earth minimum orbital intersection distance of nearly 0.184 AU, which corresponds to 71.8 lunar dista... | [
"(5836) 1993 MF\n\nis a highly eccentric, stony asteroid, classified as a near-Earth object of the Amor group of asteroids, approximately 3 kilometers in diameter. It was discovered on 22 June 1993, by American astronomers Eleanor Helin and Kenneth Lawrence at the U.S. Palomar Observatory in California.",
"(5836)... |
(5836)_1993_MF_26468354 | What information does the article about '(5836) 1993 MF' provide on 'Physical characteristics'? | Since the 1990s, and up to June 2016, four well-defined rotational lightcurves were obtained for this asteroid from photometric observations, giving a rotation period of approximately 4.95 hours with a high brightness variation between 0.53 and 0.82 in magnitude, indicating that the asteroid has a non-spheroidal shape.... | [
"(5836) 1993 MF\n\nis a highly eccentric, stony asteroid, classified as a near-Earth object of the Amor group of asteroids, approximately 3 kilometers in diameter. It was discovered on 22 June 1993, by American astronomers Eleanor Helin and Kenneth Lawrence at the U.S. Palomar Observatory in California.",
"(5836)... |
(585310)_2017_YZ1_31696163 | What information does the article about '(585310) 2017 YZ1' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 10 August 2021, receiving the number in the minor planet catalog (M.P.C. 133609). , it has not been named. | [
"(585310) 2017 YZ1 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 10 August 2021, receiving the number in the minor planet catalog (M.P.C. 133609). , it has not been named.",
"(585310) 2017 YZ1\n\n, provisional designation:, is a sub-kilometer asteroid on an eccentric orbit... |
(585310)_2017_YZ1_31696160 | What information does the article about '(585310) 2017 YZ1' provide? | , provisional designation:, is a sub-kilometer asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 250 m in diameter. It was first observed on 20 December 2017, by astronomers with the Mount Lemmon Survey at Mount Lemmon Observatory near ... | [
"(585310) 2017 YZ1 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 10 August 2021, receiving the number in the minor planet catalog (M.P.C. 133609). , it has not been named.",
"(585310) 2017 YZ1\n\n, provisional designation:, is a sub-kilometer asteroid on an eccentric orbit... |
(585310)_2017_YZ1_31696162 | What information does the article about '(585310) 2017 YZ1' provide on 'Risk assessment'? | The 9 January 2018 solution with a 15-day observation arc was listed at Torino scale 1 with a 1:21,000 chance of impacting Earth on 30 June 2047. By 9 January 2018, the geocentric 30 June 2047 uncertainty region had shrunk to ±50 million km. With a longer 20 day observation arc, it dropped to Torino scale 0 and had a 1... | [
"(585310) 2017 YZ1 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 10 August 2021, receiving the number in the minor planet catalog (M.P.C. 133609). , it has not been named.",
"(585310) 2017 YZ1\n\n, provisional designation:, is a sub-kilometer asteroid on an eccentric orbit... |
(585310)_2017_YZ1_31696161 | Reconstruct the content about 'Orbit and classification' from the article on '(585310) 2017 YZ1'. | is a member of the Apollo asteroids, which cross the orbit of Earth. Apollo's are the largest group of near-Earth objects with nearly 10 thousand known objects. It orbits the Sun at a distance of 0.88–1.77 AU once every 18 months (558 days; semi-major axis of 1.33 AU). Its orbit has an eccentricity of 0.33 and an incli... | [
"(585310) 2017 YZ1 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 10 August 2021, receiving the number in the minor planet catalog (M.P.C. 133609). , it has not been named.",
"(585310) 2017 YZ1\n\n, provisional designation:, is a sub-kilometer asteroid on an eccentric orbit... |
(589683)_2010_RF43_27305815 | What information does the article about '(589683) 2010 RF43' provide? | , provisionally designated:, is a large trans-Neptunian object orbiting in the scattered disc in the outermost regions of the Solar System. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observatory in northern Chile. | [
"(589683) 2010 RF43\n\n, provisionally designated:, is a large trans-Neptunian object orbiting in the scattered disc in the outermost regions of the Solar System. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observa... |
(589683)_2010_RF43_27305817 | What information does the article about '(589683) 2010 RF43' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 20 September 2021, receiving the number in the minor planet catalog (M.P.C. 135075). , it has not been named. | [
"(589683) 2010 RF43\n\n, provisionally designated:, is a large trans-Neptunian object orbiting in the scattered disc in the outermost regions of the Solar System. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observa... |
(589683)_2010_RF43_27305816 | Explain what '(589683) 2010 RF43' covers in the 'Orbit and classification' section. | orbits the Sun at a distance of 37.5–61.9 AU once every 350 years and 4 months (127,948 days; semi-major axis of 49.7 AU). Its orbit has an eccentricity of 0.25 and an inclination of 31° with respect to the ecliptic. The body's observation arc begins with a precovery observation taken at Siding Spring Observatory in Au... | [
"(589683) 2010 RF43\n\n, provisionally designated:, is a large trans-Neptunian object orbiting in the scattered disc in the outermost regions of the Solar System. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observa... |
(589683)_2010_RF43_27305819 | Summarize the 'Rotation period' part of '(589683) 2010 RF43'. | As of 2020, no rotational lightcurve of this object has been obtained from photometric observations. The object's rotation period, pole and shape remain unknown. | [
"(589683) 2010 RF43\n\n, provisionally designated:, is a large trans-Neptunian object orbiting in the scattered disc in the outermost regions of the Solar System. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observa... |
(6037)_1988_EG_29474188 | Describe the content of the article about '(6037) 1988 EG'. | , is an eccentric, stony asteroid, classified as near-Earth object and potentially hazardous asteroid. It belongs to the group of Apollo asteroids and measures approximately half a kilometer in diameter. It was discovered by American astronomer Jeff T. Alu at the U.S. Palomar Observatory, California, on 12 March 1988. | [
"(6037) 1988 EG\n\n, is an eccentric, stony asteroid, classified as near-Earth object and potentially hazardous asteroid. It belongs to the group of Apollo asteroids and measures approximately half a kilometer in diameter. It was discovered by American astronomer Jeff T. Alu at the U.S. Palomar Observatory, Califor... |
(6037)_1988_EG_29474191 | What does the article about '(6037) 1988 EG' say regarding 'Diameter and albedo'? | The Collaborative Asteroid Lightcurve Link (CALL) assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 540 meters, based on an absolute magnitude of 18.7. Observations with the Spitzer Space Telescope using its Infrared Array Camera at wavelengths between 3.6 and 8.0 micrometers, gave an a... | [
"(6037) 1988 EG\n\n, is an eccentric, stony asteroid, classified as near-Earth object and potentially hazardous asteroid. It belongs to the group of Apollo asteroids and measures approximately half a kilometer in diameter. It was discovered by American astronomer Jeff T. Alu at the U.S. Palomar Observatory, Califor... |
(6037)_1988_EG_29474190 | From the article on '(6037) 1988 EG', restate the 'Lightcurve' content. | An ambiguous lightcurve was obtained through photometric observations by Czech astronomer Petr Pravec in 1998. The light-curve gave a rotation period of 2.76 hours with a brightness amplitude of 0.20 in magnitude. The alternative period solution is 2.919 hours with an amplitude of 0.22 in magnitude (U=2). | [
"(6037) 1988 EG\n\n, is an eccentric, stony asteroid, classified as near-Earth object and potentially hazardous asteroid. It belongs to the group of Apollo asteroids and measures approximately half a kilometer in diameter. It was discovered by American astronomer Jeff T. Alu at the U.S. Palomar Observatory, Califor... |
(6037)_1988_EG_29474189 | Describe the 'Classification and orbit' section of the article about '(6037) 1988 EG'. | The S-type asteroid orbits the Sun at a distance of 0.6–1.9 AU once every 1 years and 5 months (523 days). Its orbit has an eccentricity of 0.50 and an inclination of 3° with respect to the ecliptic. The asteroid has an Earth minimum orbit intersection distance (MOID) of 0.0243 AU. In combination with its size, this ma... | [
"(6037) 1988 EG\n\n, is an eccentric, stony asteroid, classified as near-Earth object and potentially hazardous asteroid. It belongs to the group of Apollo asteroids and measures approximately half a kilometer in diameter. It was discovered by American astronomer Jeff T. Alu at the U.S. Palomar Observatory, Califor... |
(60621)_2000_FE8_8285775 | Describe the 'Satellite' section of the article about '(60621) 2000 FE8'. | Like many objects of the Kuiper belt and scattered disc, has a satellite. Provisionally designated S/2007 (60621) 1, the satellite was discovered by the Hubble Space Telescope seven years after itself was found. The moon orbits at 1180 kilometres away from, completing one orbit in approximately 7 days. It is thought to... | [
"(60621) 2000 FE8 — Satellite\n\nLike many objects of the Kuiper belt and scattered disc, has a satellite. Provisionally designated S/2007 (60621) 1, the satellite was discovered by the Hubble Space Telescope seven years after itself was found. The moon orbits at 1180 kilometres away from, completing one orbit in a... |
(60621)_2000_FE8_8285774 | From the article on '(60621) 2000 FE8', restate the 'Resonance with Neptune' content. | is part of a group of trans-Neptunian objects that orbit in a 2:5 resonance with Neptune. That means that for every five orbits that Neptune completes, makes only two. Several other objects are in the same orbital resonance, the largest of which is. | [
"(60621) 2000 FE8 — Satellite\n\nLike many objects of the Kuiper belt and scattered disc, has a satellite. Provisionally designated S/2007 (60621) 1, the satellite was discovered by the Hubble Space Telescope seven years after itself was found. The moon orbits at 1180 kilometres away from, completing one orbit in a... |
(60621)_2000_FE8_8285772 | Summarize the following section from the article on '(60621) 2000 FE8'. | is a resonant and binary trans-Neptunian object, approximately 146 km in diameter, located in the outermost region of the Solar System. It was discovered on 27 March 2000, by astronomers John Kavelaars, Brett Gladman, Jean-Marc Petit and Matthew Holman at Mauna Kea Observatory on Hawaii. This distant object resides in ... | [
"(60621) 2000 FE8 — Satellite\n\nLike many objects of the Kuiper belt and scattered disc, has a satellite. Provisionally designated S/2007 (60621) 1, the satellite was discovered by the Hubble Space Telescope seven years after itself was found. The moon orbits at 1180 kilometres away from, completing one orbit in a... |
(60621)_2000_FE8_8285773 | Explain what '(60621) 2000 FE8' covers in the 'Orbit' section. | has an extremely eccentric orbit which crosses the paths of many other trans-Neptunian objects, including almost all of the dwarf planets and dwarf planet candidates. As a result, its position alternates between the Kuiper belt and the scattered disc. | [
"(60621) 2000 FE8 — Satellite\n\nLike many objects of the Kuiper belt and scattered disc, has a satellite. Provisionally designated S/2007 (60621) 1, the satellite was discovered by the Hubble Space Telescope seven years after itself was found. The moon orbits at 1180 kilometres away from, completing one orbit in a... |
(60621)_2000_FE8_8285776 | From the article on '(60621) 2000 FE8', restate the 'Numbering' content. | This minor planet was numbered by the Minor Planet Center on 14 June 2003. , it has not been named. | [
"(60621) 2000 FE8 — Satellite\n\nLike many objects of the Kuiper belt and scattered disc, has a satellite. Provisionally designated S/2007 (60621) 1, the satellite was discovered by the Hubble Space Telescope seven years after itself was found. The moon orbits at 1180 kilometres away from, completing one orbit in a... |
(6178)_1986_DA_10091573 | Reconstruct the content about 'Physical characteristics' from the article on '(6178) 1986 DA'. | The metallic M-type asteroid is notable for being significantly more radar-reflective than other asteroids. Radar measurements suggest it is composed of nickel and iron and that it was derived from the center of a much larger object that experienced melting and differentiation. The observed radar albedo was 0.58 and th... | [
"(6178) 1986 DA — Physical characteristics\n\nThe metallic M-type asteroid is notable for being significantly more radar-reflective than other asteroids. Radar measurements suggest it is composed of nickel and iron and that it was derived from the center of a much larger object that experienced melting and differen... |
(6178)_1986_DA_10091574 | From the article on '(6178) 1986 DA', restate the 'Rotation and shape' content. | It was most probably formed from a larger body through a catastrophic collision with another object. Radar measurements of this body indicate that the surface is relatively smooth on scales of less than a meter, but it is highly irregular on scales of 10–100 meters. Several lightcurve analysis gave it a concurrin... | [
"(6178) 1986 DA — Physical characteristics\n\nThe metallic M-type asteroid is notable for being significantly more radar-reflective than other asteroids. Radar measurements suggest it is composed of nickel and iron and that it was derived from the center of a much larger object that experienced melting and differen... |
(6178)_1986_DA_10091576 | Summarize the 'Mining considerations' part of '(6178) 1986 DA'. | The asteroid achieved its most notable recognition when scientists revealed that it contained over "10,000 tons of gold and 100,000 tons of platinum", or an approximate value at the time of its discovery of "$90 billion for the gold and a cool trillion dollars for the platinum, plus loose change for the asteroid's 10 b... | [
"(6178) 1986 DA — Physical characteristics\n\nThe metallic M-type asteroid is notable for being significantly more radar-reflective than other asteroids. Radar measurements suggest it is composed of nickel and iron and that it was derived from the center of a much larger object that experienced melting and differen... |
(6178)_1986_DA_10091572 | Reconstruct the content about 'Orbit and classification' from the article on '(6178) 1986 DA'. | As an eccentric Amor asteroid has an Earth minimum orbit intersection distance of 0.1922 AU and approaches the orbit of Earth from the outside but does not cross it. It crosses however the orbit of Mars and can be classified as a Mars-crosser and also approaches the orbit of Jupiter within 0.5 AU. The asteroid orbits t... | [
"(6178) 1986 DA — Physical characteristics\n\nThe metallic M-type asteroid is notable for being significantly more radar-reflective than other asteroids. Radar measurements suggest it is composed of nickel and iron and that it was derived from the center of a much larger object that experienced melting and differen... |
(6178)_1986_DA_10091575 | Based on the article about '(6178) 1986 DA', describe the 'Diameter and albedo' section. | According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid has an albedo of 0.08 and 0.16, and a diameter of 3.1 to 3.2 kilometers, respectively. The Collaborative Asteroid Lightcurve Link selects 3.15 kilometers as best result, while the first es... | [
"(6178) 1986 DA — Physical characteristics\n\nThe metallic M-type asteroid is notable for being significantly more radar-reflective than other asteroids. Radar measurements suggest it is composed of nickel and iron and that it was derived from the center of a much larger object that experienced melting and differen... |
(6265)_1985_TW3_29869882 | Summarize the 'Diameter and albedo' part of '(6265) 1985 TW3'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287. The Johnston's archive derives a diameter of 4.81 km and 1.16 km for the primary and secondary, r... | [
"(6265) 1985 TW3 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287. The Johnston's archive derives a diameter of 4.81 k... |
(6265)_1985_TW3_29869877 | Describe the 'Orbit and classification' section of the article about '(6265) 1985 TW3'. | is a non-family asteroid from the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Flora family (402), a giant asteroid family and the largest family... | [
"(6265) 1985 TW3 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287. The Johnston's archive derives a diameter of 4.81 k... |
(6265)_1985_TW3_29869880 | Based on the article about '(6265) 1985 TW3', describe the 'Rotation period' section. | In June 2010, a rotational lightcurve of was obtained from photometric observations by Australian astronomers David Higgins and Julian Oey at the Hunters Hill and Leura Observatory. Lightcurve analysis gave a well-defined rotation period of 2.709 hours with a brightness variation of 0.35 magnitude (U=3). Several concu... | [
"(6265) 1985 TW3 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287. The Johnston's archive derives a diameter of 4.81 k... |
(6265)_1985_TW3_29869876 | Reconstruct the content from the article about '(6265) 1985 TW3'. | , provisional designation, is a background asteroid and binary system from the inner regions of the asteroid belt. It was discovered on 11 October 1985, by astronomer by T. F. Fric and Richard Gilbrech at the Palomar Observatory in California. It is the only minor-planet discovery for these two astronomers. The stony L... | [
"(6265) 1985 TW3 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287. The Johnston's archive derives a diameter of 4.81 k... |
(6265)_1985_TW3_29869878 | Describe the 'Numbering and naming' section of the article about '(6265) 1985 TW3'. | This minor planet was permanently numbered by the Minor Planet Center on 17 March 1995 (M.P.C. 24890–24891). As of 2018, it has not been named. | [
"(6265) 1985 TW3 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287. The Johnston's archive derives a diameter of 4.81 k... |
(6382)_1988_EL_31003168 | Based on the article about '(6382) 1988 EL', describe the 'Diameter and albedo' section. | According to two different data sets from space-based survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 4.9 and 5.3 kilometers in diameter and its surface has an albedo of 0.19 and 0.25, respectively, while the Collaborative Asteroid Lightcurve Link assumes ... | [
"(6382) 1988 EL — Diameter and albedo\n\nAccording to two different data sets from space-based survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 4.9 and 5.3 kilometers in diameter and its surface has an albedo of 0.19 and 0.25, respectively, while the Col... |
(6382)_1988_EL_31003165 | What information does the article about '(6382) 1988 EL' provide? | , is a stony Hungaria asteroid from the inner regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 14 March 1988, by American astronomer Jeffrey Alu at the U.S. Palomar Observatory, California. | [
"(6382) 1988 EL — Diameter and albedo\n\nAccording to two different data sets from space-based survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 4.9 and 5.3 kilometers in diameter and its surface has an albedo of 0.19 and 0.25, respectively, while the Col... |
(6382)_1988_EL_31003166 | From the article on '(6382) 1988 EL', restate the 'Orbit and classification' content. | The presumed E-type asteroid may not be a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System, but an unrelated interloper, which intruded into the Hungaria orbital space, as indicated by a lower albedos from observations by the NEOWISE mission. It orbits the Sun... | [
"(6382) 1988 EL — Diameter and albedo\n\nAccording to two different data sets from space-based survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 4.9 and 5.3 kilometers in diameter and its surface has an albedo of 0.19 and 0.25, respectively, while the Col... |
(6382)_1988_EL_31003167 | What does the article about '(6382) 1988 EL' say regarding 'Rotation period'? | Between February 2005 and January 2015, American astronomer Brian D. Warner obtained 5 rotational lightcurves for this asteroid from photometric observations at the CS3–Palmer Divide Station in Colorado. The lightcurves gave a well-defined rotation period of 2.892–2.898 hours with a low brightness variation between 0.0... | [
"(6382) 1988 EL — Diameter and albedo\n\nAccording to two different data sets from space-based survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 4.9 and 5.3 kilometers in diameter and its surface has an albedo of 0.19 and 0.25, respectively, while the Col... |
(65407)_2002_RP120_4680755 | What information does the article about '(65407) 2002 RP120' provide? | ''', provisional designation ', is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the United States. The unusual obj... | [
"(65407) 2002 RP120\n\n''', provisional designation ', is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the Uni... |
(65407)_2002_RP120_4680759 | Based on the article about '(65407) 2002 RP120', describe the 'Rotation period' section. | In October 2010, a rotational lightcurve of was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 200 hours with a brightness amplitude of 0.6 magnitude, indicative of an elongated, non-spherical shape (U=2). With a rotation period above 100 hou... | [
"(65407) 2002 RP120\n\n''', provisional designation ', is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the Uni... |
(65407)_2002_RP120_4680757 | What does the article about '(65407) 2002 RP120' say regarding 'Numbering and naming'? | This minor planet was permanently numbered by the Minor Planet Center on 14 June 2003 (M.P.C. 48994). As of 2018, it has not been named. | [
"(65407) 2002 RP120\n\n''', provisional designation ', is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the Uni... |
(65407)_2002_RP120_4680756 | Explain what '(65407) 2002 RP120' covers in the 'Orbit and classification' section. | is a member of the damocloids, with a retrograde orbit and a negative TJupiter of −0.8340. It is also a trans-Neptunian object, as its orbit has a semi-major axis larger than that of Neptune (30.1 AU). The Minor Planet Center lists it as a critical object, centaur, and (other) unusual minor planet due to an orbital ecc... | [
"(65407) 2002 RP120\n\n''', provisional designation ', is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the Uni... |
(65407)_2002_RP120_4680760 | Explain what '(65407) 2002 RP120' covers in the 'Diameter and albedo' section. | According to the survey of minor-planet albedos of bodies in a comet-like orbit, carried out by Yanga Fernández in collaboration with David Jewitt and Scott Sheppard at the Institute for Astronomy, Hawaii, measures 14.6 kilometers in diameter and its surface has an albedo of 0.098. Johnston's archive gives a rounded f... | [
"(65407) 2002 RP120\n\n''', provisional designation ', is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the Uni... |
(66063)_1998_RO1_29259616 | Reconstruct the content about 'Moon' from the article on '(66063) 1998 RO1'. | has one moon,. This moon was discovered from lightcurve observations going from 13 to 28 September 2013, and was confirmed by radar observations from the Arecibo Observatory one year later. It is in a very close orbit to, with a semi-major axis of 800 m and an eccentricity of 0.06, giving it a periapsis of 752 m and an... | [
"(66063) 1998 RO1 — Moon\n\nhas one moon,. This moon was discovered from lightcurve observations going from 13 to 28 September 2013, and was confirmed by radar observations from the Arecibo Observatory one year later. It is in a very close orbit to, with a semi-major axis of 800 m and an eccentricity of 0.06, givin... |
(66063)_1998_RO1_29259615 | Summarize the 'Interaction with Earth' part of '(66063) 1998 RO1'. | 's orbit is very eccentric, with an aphelion beyond the orbit of Mars and a perihelion inside the orbit of Mercury. It has an orbital period of 360.29 days (0.99 years) and makes close approaches to Earth. But makes closer approaches to other inner planets, especially Mars. Its closest approach to a planet between 1950... | [
"(66063) 1998 RO1 — Moon\n\nhas one moon,. This moon was discovered from lightcurve observations going from 13 to 28 September 2013, and was confirmed by radar observations from the Arecibo Observatory one year later. It is in a very close orbit to, with a semi-major axis of 800 m and an eccentricity of 0.06, givin... |
(66063)_1998_RO1_29259617 | Reconstruct the content about 'Numbering and naming' from the article on '(66063) 1998 RO1'. | This minor planet was numbered by the Minor Planet Center on 10 September 2003. As of 2018, it has not been named. | [
"(66063) 1998 RO1 — Moon\n\nhas one moon,. This moon was discovered from lightcurve observations going from 13 to 28 September 2013, and was confirmed by radar observations from the Arecibo Observatory one year later. It is in a very close orbit to, with a semi-major axis of 800 m and an eccentricity of 0.06, givin... |
(7025)_1993_QA_32875782 | From the article on '(7025) 1993 QA', restate the 'Close approaches' content. | The asteroid has an Earth minimum orbital intersection distance of 0.0645 AU, which translates into 25.1 lunar distances. On 6 February 1996 it transited Earth at a nominal distance of 0.07080 AU. The body's next encounter with Earth below 0.1 AU will occur on 8 February 2048, at a distance of 0.06275 AU. | [
"(7025) 1993 QA — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0645 AU, which translates into 25.1 lunar distances. On 6 February 1996 it transited Earth at a nominal distance of 0.07080 AU. The body's next encounter with Earth below 0.1 AU will occur on 8 February 2048, ... |
(7025)_1993_QA_32875785 | Explain what '(7025) 1993 QA' 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 498 meters in diameter and its surface has a high albedo of 0.340. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a diameter of 770 meters base... | [
"(7025) 1993 QA — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0645 AU, which translates into 25.1 lunar distances. On 6 February 1996 it transited Earth at a nominal distance of 0.07080 AU. The body's next encounter with Earth below 0.1 AU will occur on 8 February 2048, ... |
(7025)_1993_QA_32875781 | Explain what '(7025) 1993 QA' covers in the 'Orbit and classification' section. | is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Conversely, it is classified as a non-Earth crossing Amor asteroid by the Minor Planet Center, due to its near-threshold perihelion of 1.011 AU. It orbits the Sun at a distance of 1.01–1.94 AU once every 21 months (655 days; semi-major axis ... | [
"(7025) 1993 QA — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0645 AU, which translates into 25.1 lunar distances. On 6 February 1996 it transited Earth at a nominal distance of 0.07080 AU. The body's next encounter with Earth below 0.1 AU will occur on 8 February 2048, ... |
(7025)_1993_QA_32875784 | Summarize the 'Rotation period' part of '(7025) 1993 QA'. | In the late 1990s, two rotational lightcurves of were obtained from photometric observations by European astronomers. Lightcurve analysis gave an identical, well-defined rotation period of 2.5057 hours with a brightness amplitude of 0.32 and 0.50 magnitude, respectively (U=3/3). Its period is near the cohesionless spin... | [
"(7025) 1993 QA — Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0645 AU, which translates into 25.1 lunar distances. On 6 February 1996 it transited Earth at a nominal distance of 0.07080 AU. The body's next encounter with Earth below 0.1 AU will occur on 8 February 2048, ... |
(7335)_1989_JA_13940146 | What information does the article about '(7335) 1989 JA' provide on 'Physical characteristics'? | During its discovery in May 1989, radiometric observations for this asteroid at Arecibo and Goldstone Observatory rendered a rotation period of 12 hours (U=n.a.). According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 0.93 kilometers in diameter a... | [
"(7335) 1989 JA — Naming\n\nAs of 2019, remains unnamed.",
"(7335) 1989 JA — Physical characteristics\n\nDuring its discovery in May 1989, radiometric observations for this asteroid at Arecibo and Goldstone Observatory rendered a rotation period of 12 hours (U=n.a.). According to the survey carried out by the NEO... |
(7335)_1989_JA_13940145 | Based on the article about '(7335) 1989 JA', describe the 'Orbit and classification' section. | The S-type asteroid orbits the Sun at a distance of 0.9–2.6 AU once every 2 years and 4 months (861 days). Its orbit has an eccentricity of 0.48 and an inclination of 15° with respect to the ecliptic. The first observation was made at the discovering observatory in April 1989, extending the asteroid's observation arc b... | [
"(7335) 1989 JA — Naming\n\nAs of 2019, remains unnamed.",
"(7335) 1989 JA — Physical characteristics\n\nDuring its discovery in May 1989, radiometric observations for this asteroid at Arecibo and Goldstone Observatory rendered a rotation period of 12 hours (U=n.a.). According to the survey carried out by the NEO... |
(7348)_1993_FJ22_17132512 | Explain what '(7348) 1993 FJ22' covers in the 'Diameter and albedo' section. | The Collaborative Asteroid Lightcurve Link (CALL) assumes a low albedo of 0.08 for the asteroid's surface and calculates a diameter of 9.9 kilometers, based on an absolute magnitude of 13.38. | [
"(7348) 1993 FJ22 — Diameter and albedo\n\nThe Collaborative Asteroid Lightcurve Link (CALL) assumes a low albedo of 0.08 for the asteroid's surface and calculates a diameter of 9.9 kilometers, based on an absolute magnitude of 13.38.",
"(7348) 1993 FJ22\n\nis a carbonaceous, Themistian asteroid from the outer re... |
(7348)_1993_FJ22_17132509 | Summarize the following section from the article on '(7348) 1993 FJ22'. | is a carbonaceous, Themistian asteroid from the outer region of the asteroid belt, about 10 kilometers in diameter. It was discovered on 21 March 1993, by the Uppsala-ESO Survey of Asteroids and Comets (UESAC) at ESO's La Silla Observatory site in northern Chile. | [
"(7348) 1993 FJ22 — Diameter and albedo\n\nThe Collaborative Asteroid Lightcurve Link (CALL) assumes a low albedo of 0.08 for the asteroid's surface and calculates a diameter of 9.9 kilometers, based on an absolute magnitude of 13.38.",
"(7348) 1993 FJ22\n\nis a carbonaceous, Themistian asteroid from the outer re... |
(7348)_1993_FJ22_17132511 | Based on the article about '(7348) 1993 FJ22', describe the 'Lightcurves' section. | In 2014, two rotational lightcurves of this asteroid were obtained from photometric observations in the R-band at the U.S. Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 3.4735 and 3.470 hours with a brightness variation of 0.10 and 0.13 in magnitude, respectively (U=2/2). | [
"(7348) 1993 FJ22 — Diameter and albedo\n\nThe Collaborative Asteroid Lightcurve Link (CALL) assumes a low albedo of 0.08 for the asteroid's surface and calculates a diameter of 9.9 kilometers, based on an absolute magnitude of 13.38.",
"(7348) 1993 FJ22\n\nis a carbonaceous, Themistian asteroid from the outer re... |
(7348)_1993_FJ22_17132510 | Reconstruct the content about 'Classification and orbit' from the article on '(7348) 1993 FJ22'. | The dark C-type asteroid is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.8–3.4 AU once every 5 years and 5 months (1,987 days). Its orbit has an eccentricity of 0.11 and an inclination of 1° ... | [
"(7348) 1993 FJ22 — Diameter and albedo\n\nThe Collaborative Asteroid Lightcurve Link (CALL) assumes a low albedo of 0.08 for the asteroid's surface and calculates a diameter of 9.9 kilometers, based on an absolute magnitude of 13.38.",
"(7348) 1993 FJ22\n\nis a carbonaceous, Themistian asteroid from the outer re... |
(7482)_1994_PC1_20209487 | Summarize the 'Diameter and albedo' part of '(7482) 1994 PC1'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.052 kilometers in diameter and its surface has an albedo of 0.277. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.20 and calculates a diameter of 1.30 kilometers based on an absolute m... | [
"(7482) 1994 PC1 — Naming\n\nAs of 2021, this minor planet has not been named.",
"(7482) 1994 PC1 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.052 kilometers in diameter and its surface has an albedo of 0.277. The Col... |
(7482)_1994_PC1_20209486 | What information does the article about '(7482) 1994 PC1' provide on 'Rotation period'? | In 1998, a rotational lightcurve of was obtained from photometric observations by Petr Pravec. Lightcurve analysis gave a well-defined rotation period of 2.5999 hours with a brightness amplitude of 0.29 magnitude (U=3). | [
"(7482) 1994 PC1 — Naming\n\nAs of 2021, this minor planet has not been named.",
"(7482) 1994 PC1 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.052 kilometers in diameter and its surface has an albedo of 0.277. The Col... |
(7482)_1994_PC1_20209484 | What does the article about '(7482) 1994 PC1' say regarding 'Orbit and classification'? | orbits the Sun at a distance of 0.9–1.8 AU once every 1 years and 7 months (572 days). Its orbit has an eccentricity of 0.33 and an inclination of 33° with respect to the ecliptic. On 17 January 1933, it passed 0.00752 AU from Earth. On 18 January 2022, it will pass 0.01324 AU from Earth. | [
"(7482) 1994 PC1 — Naming\n\nAs of 2021, this minor planet has not been named.",
"(7482) 1994 PC1 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.052 kilometers in diameter and its surface has an albedo of 0.277. The Col... |
(7482)_1994_PC1_20209488 | Reconstruct the content about '2022 flyby' from the article on '(7482) 1994 PC1'. | On 19 January 2022, will pass just outside of 5 lunar distances of Earth, with a peak magnitude of about 10 placing just outside the reach of common binoculars. | [
"(7482) 1994 PC1 — Naming\n\nAs of 2021, this minor planet has not been named.",
"(7482) 1994 PC1 — Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.052 kilometers in diameter and its surface has an albedo of 0.277. The Col... |
(75482)_1999_XC173_13638825 | Based on the article about '(75482) 1999 XC173', describe the 'Classification and orbit' section. | The body is classified as a S-type member of the Vesta family by the Collaborative Asteroid Lightcurve Link Light Curve Data Base (LCDB). It orbits the Sun at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,328 days). Its orbit has an eccentricity of 0.08 and an inclination of 6° with respect to the eclipti... | [
"(75482) 1999 XC173 — Classification and orbit\n\nThe body is classified as a S-type member of the Vesta family by the Collaborative Asteroid Lightcurve Link Light Curve Data Base (LCDB). It orbits the Sun at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,328 days). Its orbit has an eccentricity of 0.0... |
(75482)_1999_XC173_13638824 | Reconstruct the content from the article about '(75482) 1999 XC173'. | is a stony Vestian asteroid and an exceptionally slow rotating body from the inner regions of the asteroid belt, approximately 3 kilometers in diameter. It was discovered on 10 December 1999, by LINEAR at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico, United States. | [
"(75482) 1999 XC173 — Classification and orbit\n\nThe body is classified as a S-type member of the Vesta family by the Collaborative Asteroid Lightcurve Link Light Curve Data Base (LCDB). It orbits the Sun at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,328 days). Its orbit has an eccentricity of 0.0... |
(75482)_1999_XC173_13638827 | What information does the article about '(75482) 1999 XC173' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 15 April 2004. As of 2018, it has not been named. | [
"(75482) 1999 XC173 — Classification and orbit\n\nThe body is classified as a S-type member of the Vesta family by the Collaborative Asteroid Lightcurve Link Light Curve Data Base (LCDB). It orbits the Sun at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,328 days). Its orbit has an eccentricity of 0.0... |
(75482)_1999_XC173_13638826 | Summarize the 'Physical characteristics' part of '(75482) 1999 XC173'. | A rotational lightcurve was obtained for this asteroid from photometric observations at the Californian Palomar Transient Factory in September 2013. It gave a rotation period of 1234 hours with an estimated error margin of ±90 hours. , it is the 6th slowest rotating minor planet known to exist. Its high brightness vari... | [
"(75482) 1999 XC173 — Classification and orbit\n\nThe body is classified as a S-type member of the Vesta family by the Collaborative Asteroid Lightcurve Link Light Curve Data Base (LCDB). It orbits the Sun at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,328 days). Its orbit has an eccentricity of 0.0... |
(7563)_1988_BC_17132758 | Summarize the 'Lightcurves' part of '(7563) 1988 BC'. | In January 2010, a rotational lightcurve of was obtained from photometric observations by Pierre Antonini at the Bédoin Observatory in southeastern France. Lightcurve analysis gave a rotation period of 6.539 hours with a brightness variation of 0.30 in magnitude (U=3). A previous 2006-observation by American astronome... | [
"(7563) 1988 BC — Naming\n\nAs of 2018, remains unnamed.",
"(7563) 1988 BC — Lightcurves\n\nIn January 2010, a rotational lightcurve of was obtained from photometric observations by Pierre Antonini at the Bédoin Observatory in southeastern France. Lightcurve analysis gave a rotation period of 6.539 hours with a... |
(7563)_1988_BC_17132759 | From the article on '(7563) 1988 BC', 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, the asteroid has a low albedo of between 0.048 and 0.08, with a diameter between 12.04 and 17.27 kilometers. Despite the results from the space-based observations, the Collaborativ... | [
"(7563) 1988 BC — Naming\n\nAs of 2018, remains unnamed.",
"(7563) 1988 BC — Lightcurves\n\nIn January 2010, a rotational lightcurve of was obtained from photometric observations by Pierre Antonini at the Bédoin Observatory in southeastern France. Lightcurve analysis gave a rotation period of 6.539 hours with a... |
(7563)_1988_BC_17132756 | Describe the 'Classification and orbit' section of the article about '(7563) 1988 BC'. | is non-family asteroid of the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.1–3.3 AU once every 4 years and 5 months (1,602 days; semi-major axis of 2.68 AU). Its orbit has an eccentricity of 0.23 and an inclination of 13° with respect to the ecliptic. | [
"(7563) 1988 BC — Naming\n\nAs of 2018, remains unnamed.",
"(7563) 1988 BC — Lightcurves\n\nIn January 2010, a rotational lightcurve of was obtained from photometric observations by Pierre Antonini at the Bédoin Observatory in southeastern France. Lightcurve analysis gave a rotation period of 6.539 hours with a... |
(78799)_2002_XW93_12469015 | From the article on '(78799) 2002 XW93', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 15 April 2004. As of 2018, it has not been named. | [
"(78799) 2002 XW93 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 15 April 2004. As of 2018, it has not been named.",
"(78799) 2002 XW93\n\n, provisional designation, is a trans-Neptunian object and centaur from the outer Solar System, approximately 500 - 600 km in diameter... |
(78799)_2002_XW93_12469013 | What information does the article about '(78799) 2002 XW93' provide? | , provisional designation, is a trans-Neptunian object and centaur from the outer Solar System, approximately 500 - 600 km in diameter. It was discovered on 10 December 2002, by astronomers at the Palomar Observatory in California. | [
"(78799) 2002 XW93 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 15 April 2004. As of 2018, it has not been named.",
"(78799) 2002 XW93\n\n, provisional designation, is a trans-Neptunian object and centaur from the outer Solar System, approximately 500 - 600 km in diameter... |
(78799)_2002_XW93_12469014 | Explain what '(78799) 2002 XW93' covers in the 'Orbit and physical characteristics' section. | orbits the Sun at a distance of 27.9–46.8 AU once every 228 years and 4 months (83,410 days; semi-major axis of 37.36 AU). Its orbit has an eccentricity of 0.25 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken Palo... | [
"(78799) 2002 XW93 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 15 April 2004. As of 2018, it has not been named.",
"(78799) 2002 XW93\n\n, provisional designation, is a trans-Neptunian object and centaur from the outer Solar System, approximately 500 - 600 km in diameter... |
(79983)_1999_DF9_8701825 | Reconstruct the content about 'Classification and orbit' from the article on '(79983) 1999 DF9'. | The carbonaceous minor planet is a classical Kuiper belt object or "cubewano", which are not in an orbital resonance with Neptune and do not cross the giant planet's orbit. It orbits the Sun at a distance of 39.8–53.6 AU once every 319 years and 1 month (116,560 days). Its orbit has an eccentricity of 0.15 and an incli... | [
"(79983) 1999 DF9 — Classification and orbit\n\nThe carbonaceous minor planet is a classical Kuiper belt object or \"cubewano\", which are not in an orbital resonance with Neptune and do not cross the giant planet's orbit. It orbits the Sun at a distance of 39.8–53.6 AU once every 319 years and 1 month (116,560 day... |
(79983)_1999_DF9_8701827 | Reconstruct the content about 'Numbering and naming' from the article on '(79983) 1999 DF9'. | This minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named. | [
"(79983) 1999 DF9 — Classification and orbit\n\nThe carbonaceous minor planet is a classical Kuiper belt object or \"cubewano\", which are not in an orbital resonance with Neptune and do not cross the giant planet's orbit. It orbits the Sun at a distance of 39.8–53.6 AU once every 319 years and 1 month (116,560 day... |
(79983)_1999_DF9_8701826 | Describe the 'Physical characteristics' section of the article about '(79983) 1999 DF9'. | In February 2001, a rotational lightcurve was published for this minor planet from photometric observations by Portuguese astronomer Pedro Lacerda and the discovering astronomer Jane Luu. Lightcurve analysis gave a relatively short rotation period of 6.65 hours with a brightness variation of 0.40 magnitude (U=2). The C... | [
"(79983) 1999 DF9 — Classification and orbit\n\nThe carbonaceous minor planet is a classical Kuiper belt object or \"cubewano\", which are not in an orbital resonance with Neptune and do not cross the giant planet's orbit. It orbits the Sun at a distance of 39.8–53.6 AU once every 319 years and 1 month (116,560 day... |
(79983)_1999_DF9_8701824 | Based on the article about '(79983) 1999 DF9', describe the 'Discovery' section. | It was discovered on 20 February 1999, by American and British astronomers Jane Luu, Chad Trujillo and David C. Jewitt at the U.S. Kitt Peak National Observatory in Arizona. As no precoveries were taken, the minor planet's observation arc begins with its discovery observation in 1999. | [
"(79983) 1999 DF9 — Classification and orbit\n\nThe carbonaceous minor planet is a classical Kuiper belt object or \"cubewano\", which are not in an orbital resonance with Neptune and do not cross the giant planet's orbit. It orbits the Sun at a distance of 39.8–53.6 AU once every 319 years and 1 month (116,560 day... |
(8201)_1994_AH2_27911687 | What information does the article about '(8201) 1994 AH2' provide? | is a highly eccentric, rare-type asteroid, classified as near-Earth object of the Apollo group of asteroids, approximately 2 kilometers in diameter. It was discovered on 5 January 1994, by Australian amateur astronomer Gordon Garradd during the AANEAS survey at the Siding Spring Observatory, Australia. It has an Earth ... | [
"(8201) 1994 AH2 — Physical characteristics\n\nIn the SMASS classification, is characterized as a rare O-type asteroid.",
"(8201) 1994 AH2 — Naming\n\nAs of 2017, remains unnamed.",
"(8201) 1994 AH2\n\nis a highly eccentric, rare-type asteroid, classified as near-Earth object of the Apollo group of asteroids, a... |
(8201)_1994_AH2_27911690 | Describe the 'Rotation period' section of the article about '(8201) 1994 AH2'. | In the late 1990s, Czech astronomer Petr Pravec obtained two rotational lightcurves for this asteroid from photometric observations taken at the Ondřejov Observatory, Czech Republic. They gave a longer-than average rotation period of 23.949 and 24 hours with a brightness variation of 0.27 and 0.3 magnitude, respectivel... | [
"(8201) 1994 AH2 — Physical characteristics\n\nIn the SMASS classification, is characterized as a rare O-type asteroid.",
"(8201) 1994 AH2 — Naming\n\nAs of 2017, remains unnamed.",
"(8201) 1994 AH2\n\nis a highly eccentric, rare-type asteroid, classified as near-Earth object of the Apollo group of asteroids, a... |
(8201)_1994_AH2_27911688 | What information does the article about '(8201) 1994 AH2' provide on 'Orbit and classification'? | The asteroid orbits the Sun at a distance of 0.7–4.3 AU once every 4.04 years (1,477 days). Its orbit has an eccentricity of 0.71 and an inclination of 10° with respect to the ecliptic. It is a member of the Alinda group of asteroids with a 3:1 resonance with Jupiter that has excited the eccentricity of the orbit over ... | [
"(8201) 1994 AH2 — Physical characteristics\n\nIn the SMASS classification, is characterized as a rare O-type asteroid.",
"(8201) 1994 AH2 — Naming\n\nAs of 2017, remains unnamed.",
"(8201) 1994 AH2\n\nis a highly eccentric, rare-type asteroid, classified as near-Earth object of the Apollo group of asteroids, a... |
(8201)_1994_AH2_27911691 | Reconstruct the content about 'Diameter and albedo' from the article on '(8201) 1994 AH2'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 1.86 kilometers in diameter and its surface has an albedo of 0.154. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.18 and calculates a diameter of 2.17 kilometers, based on ... | [
"(8201) 1994 AH2 — Physical characteristics\n\nIn the SMASS classification, is characterized as a rare O-type asteroid.",
"(8201) 1994 AH2 — Naming\n\nAs of 2017, remains unnamed.",
"(8201) 1994 AH2\n\nis a highly eccentric, rare-type asteroid, classified as near-Earth object of the Apollo group of asteroids, a... |
(82075)_2000_YW134_32126217 | What does the article about '(82075) 2000 YW134' say regarding 'Orbit and classification'? | orbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its official discovery observation by Spacewatch on 26 December... | [
"(82075) 2000 YW134 — Orbit and classification\n\norbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its offic... |
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