id string | question string | answer string | documents list |
|---|---|---|---|
(35107)_1991_VH_23165663 | Summarize the 'Origin' part of '(35107) 1991 VH'. | As with many binary near-Earth asteroids, the system is thought to have formed through rotational fissioning of a progenitor body due to spin-up by the YORP effect. The resulting mass shed from the progenitor body coalesced in orbit to form the satellite. | [
"(35107) 1991 VH β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH β Mas... |
(35107)_1991_VH_23165659 | Based on the article about '(35107) 1991 VH', describe the 'Spectral type' section. | In the SMASS taxonomy, is classified as a transitional Sk-type, which is an intermediary between the common stony S-type and the less frequent K-type asteroids. | [
"(35107) 1991 VH β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH β Mas... |
(35107)_1991_VH_23165654 | Reconstruct the content about 'Numbering and naming' from the article on '(35107) 1991 VH'. | This minor planet was numbered by the Minor Planet Center on 27 February 2002. It has not yet been named. | [
"(35107) 1991 VH β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH β Mas... |
(35107)_1991_VH_23165657 | Explain what '(35107) 1991 VH' covers in the 'Diameter, shape, and albedo' section. | High-resolution radar imaging from Goldstone and Arecibo Observatory in 2008 show that the primary is a roughly-spheroidal object with an equatorial ridge, bearing resemblance to a spinning top. This shape is not unique to as it been observed in other near-Earth asteroids; most notably 66391 Moshup, 101955 Bennu, and 1... | [
"(35107) 1991 VH β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0247 AU, which translates into approximately 9.6 lunar distances (LD). It has made multiple close approaches to Earth, with the closest being 0.0458 AU or 17.8 LD on 15 August 2008.",
"(35107) 1991 VH β Mas... |
(35671)_1998_SN165_24506617 | What information does the article about '(35671) 1998 SN165' provide? | , prov. designation:, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt object is a dwarf planet c... | [
"(35671) 1998 SN165\n\n, prov. designation:, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt... |
(35671)_1998_SN165_24506620 | What information does the article about '(35671) 1998 SN165' provide on 'Physical characteristics'? | has a blue-grey color (BB), with various color indices measured, giving a difference between the blue and red filter magnitude (BR) of 1.123 and 1.13, respectively. | [
"(35671) 1998 SN165\n\n, prov. designation:, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt... |
(35671)_1998_SN165_24506619 | What information does the article about '(35671) 1998 SN165' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 27 February 2002 and received the number in the minor planet catalog (M.P.C. 44869). , it has not been named. Acoording to the established naming conventions, it will receive a mythological or mythic name (not necessarily from Classical mythology), in particu... | [
"(35671) 1998 SN165\n\n, prov. designation:, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt... |
(357439)_2004_BL86_3093798 | Reconstruct the content about '2015 Earth approach' from the article on '(357439) 2004 BL86'. | On 26 January 2015 at 16:20 UTC, passed 1199600 km, or 3.1 lunar distances, from Earth. The asteroid briefly peaked around apparent magnitude 9 and was near the celestial equator. The asteroid was visible in telescopes with objectives of 100 mm or larger; high-end binoculars under a dark sky may also have worked. Near ... | [
"(357439) 2004 BL86 β 2015 Earth approach\n\nOn 26 January 2015 at 16:20 UTC, passed 1199600 km, or 3.1 lunar distances, from Earth. The asteroid briefly peaked around apparent magnitude 9 and was near the celestial equator. The asteroid was visible in telescopes with objectives of 100 mm or larger; high-end binocu... |
(357439)_2004_BL86_3093799 | Explain what '(357439) 2004 BL86' covers in the 'Satellite' section. | A minor-planet moon, provisionally designated, was first detected by ground-based telescopes by Joe Pollock and Petr Pravec. Observations by the Goldstone Deep Space Communications Complex and Green Bank Telescope confirmed that it is a binary asteroid with a secondary roughly 70 m across. The secondary is estimated to... | [
"(357439) 2004 BL86 β 2015 Earth approach\n\nOn 26 January 2015 at 16:20 UTC, passed 1199600 km, or 3.1 lunar distances, from Earth. The asteroid briefly peaked around apparent magnitude 9 and was near the celestial equator. The asteroid was visible in telescopes with objectives of 100 mm or larger; high-end binocu... |
(367789)_2011_AG5_395430 | Summarize the 'Older risks' part of '(367789) 2011 AG5'. | Virtual clones of the asteroid that fit the mid-2012 uncertainty region in the known trajectory showed four potential impacts between 2040 and 2047. It had a 1 in 500 chance of impacting the Earth on 5 February 2040. In September 2013, there was an opportunity to make additional observations of when it came within 0.98... | [
"(367789) 2011 AG5 β Older risks\n\nVirtual clones of the asteroid that fit the mid-2012 uncertainty region in the known trajectory showed four potential impacts between 2040 and 2047. It had a 1 in 500 chance of impacting the Earth on 5 February 2040. In September 2013, there was an opportunity to make additional ... |
(367789)_2011_AG5_395428 | Summarize the 'Description' part of '(367789) 2011 AG5'. | was discovered on 8 January 2011 by the Mount Lemmon Survey at an apparent magnitude of 19.6 using a 1.52 m reflecting telescope. Pan-STARRS precovery images from 8 November 2010 extended the observation arc to 317 days. Observations by the Gemini 8.2 m telescope at Mauna Kea recovered the asteroid on October 20, 21 an... | [
"(367789) 2011 AG5 β Older risks\n\nVirtual clones of the asteroid that fit the mid-2012 uncertainty region in the known trajectory showed four potential impacts between 2040 and 2047. It had a 1 in 500 chance of impacting the Earth on 5 February 2040. In September 2013, there was an opportunity to make additional ... |
(367789)_2011_AG5_395429 | Explain what '(367789) 2011 AG5' covers in the 'Description' section. | 2040 the asteroid will pass no closer than 0.0066 AU (~2.6 LD) from Earth. Until 21 December 2012 it was listed on the Sentry Risk Table with a rating on the Torino Scale of Level 1. A Torino rating of 1 is a routine discovery in which a pass near the Earth is predicted that poses no unusual level of danger. It is esti... | [
"(367789) 2011 AG5 β Older risks\n\nVirtual clones of the asteroid that fit the mid-2012 uncertainty region in the known trajectory showed four potential impacts between 2040 and 2047. It had a 1 in 500 chance of impacting the Earth on 5 February 2040. In September 2013, there was an opportunity to make additional ... |
(367789)_2011_AG5_395427 | Describe the content of the article about '(367789) 2011 AG5'. | , provisional designation, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It has a diameter of about 140 m. It was removed from the Sentry Risk Table on 21 December 2012 and as such it now has a rating of 0 on the Torino Scale. | [
"(367789) 2011 AG5 β Older risks\n\nVirtual clones of the asteroid that fit the mid-2012 uncertainty region in the known trajectory showed four potential impacts between 2040 and 2047. It had a 1 in 500 chance of impacting the Earth on 5 February 2040. In September 2013, there was an opportunity to make additional ... |
(369623)_2011_DY5_13272131 | From the article on '(369623) 2011 DY5', restate the 'Physical characteristics' content. | Based on a generic magnitude-to-diameter conversion, measures 3.2 kilometers in diameter for an absolute magnitude of 16.0 and an assumed albedo of 0.07, which is a typical value for a Tirela asteroid. As of 2018, no rotational lightcurve has been obtained from photometric observations. The asteroid's rotation period, ... | [
"(369623) 2011 DY5 β Physical characteristics\n\nBased on a generic magnitude-to-diameter conversion, measures 3.2 kilometers in diameter for an absolute magnitude of 16.0 and an assumed albedo of 0.07, which is a typical value for a Tirela asteroid. As of 2018, no rotational lightcurve has been obtained from photo... |
(369623)_2011_DY5_13272132 | Based on the article about '(369623) 2011 DY5', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 21 August 2013 (M.P.C. 84643). As of 2018, it has not been named. | [
"(369623) 2011 DY5 β Physical characteristics\n\nBased on a generic magnitude-to-diameter conversion, measures 3.2 kilometers in diameter for an absolute magnitude of 16.0 and an assumed albedo of 0.07, which is a typical value for a Tirela asteroid. As of 2018, no rotational lightcurve has been obtained from photo... |
(369623)_2011_DY5_13272129 | Summarize the following section from the article on '(369623) 2011 DY5'. | , provisional designation, is a Tirela asteroid from the outer regions of the asteroid belt, approximately 3.2 km in diameter. It was discovered on 30 August 2008, by French amateur astronomers Christophe Demeautis and Jean-Marie Lopez at the Pises Observatory in southern France. | [
"(369623) 2011 DY5 β Physical characteristics\n\nBased on a generic magnitude-to-diameter conversion, measures 3.2 kilometers in diameter for an absolute magnitude of 16.0 and an assumed albedo of 0.07, which is a typical value for a Tirela asteroid. As of 2018, no rotational lightcurve has been obtained from photo... |
(374158)_2004_UL_23050428 | Based on the article about '(374158) 2004 UL', describe the 'Physical characteristics' section. | is an assumed stony S-type asteroid. In October 2014, a rotational lightcurve for this asteroid was obtained from photometric observations by American astronomer Brian Warner at the CS3βPalmer Divide Station (U82) in Landers, California. It gave a longer-than average rotation period of 38 hours (most minor planets take... | [
"(374158) 2004 UL β Physical characteristics\n\nis an assumed stony S-type asteroid. In October 2014, a rotational lightcurve for this asteroid was obtained from photometric observations by American astronomer Brian Warner at the CS3βPalmer Divide Station (U82) in Landers, California. It gave a longer-than average ... |
(374158)_2004_UL_23050426 | Describe the content of the article about '(374158) 2004 UL'. | is a sub-kilometer asteroid on an outstandingly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. The object is known for having the second-smallest perihelion of any known asteroid, after. It was discovered on 18 October 2004 by the Lincoln Near-Earth Asteroid Res... | [
"(374158) 2004 UL β Physical characteristics\n\nis an assumed stony S-type asteroid. In October 2014, a rotational lightcurve for this asteroid was obtained from photometric observations by American astronomer Brian Warner at the CS3βPalmer Divide Station (U82) in Landers, California. It gave a longer-than average ... |
(374158)_2004_UL_23050427 | What does the article about '(374158) 2004 UL' say regarding 'Orbit and classification'? | This Apollo asteroid orbits the Sun at a distance of 0.09β2.44 AU once every 17 months (521 days; semi-major axis of 1.27 AU). Its orbit has an outstandingly high eccentricity of 0.93 and an inclination of 24Β° with respect to the ecliptic. Due to its orbit, it is also a Mercury-crosser, Venus-crosser and Mars-crosser. ... | [
"(374158) 2004 UL β Physical characteristics\n\nis an assumed stony S-type asteroid. In October 2014, a rotational lightcurve for this asteroid was obtained from photometric observations by American astronomer Brian Warner at the CS3βPalmer Divide Station (U82) in Landers, California. It gave a longer-than average ... |
(374158)_2004_UL_23050429 | Describe the 'Numbering and naming' section of the article about '(374158) 2004 UL'. | This minor planet was numbered by the Minor Planet Center on 18 October 2013 (M.P.C. 85347). As of 2018, it has not been named. | [
"(374158) 2004 UL β Physical characteristics\n\nis an assumed stony S-type asteroid. In October 2014, a rotational lightcurve for this asteroid was obtained from photometric observations by American astronomer Brian Warner at the CS3βPalmer Divide Station (U82) in Landers, California. It gave a longer-than average ... |
(38063)_1999_FH_23523092 | Describe the 'Orbit and classification' section of the article about '(38063) 1999 FH'. | orbits the Sun at a distance of 1.7β3.0 AU once every 3 years and 7 months (1,309 days). Its orbit has an eccentricity of 0.29 and an inclination of 12Β° with respect to the ecliptic. A first precovery was taken at Steward Observatory in 1992, extending the body's observation arc by 7 years prior to its official discove... | [
"(38063) 1999 FH β Orbit and classification\n\norbits the Sun at a distance of 1.7β3.0 AU once every 3 years and 7 months (1,309 days). Its orbit has an eccentricity of 0.29 and an inclination of 12Β° with respect to the ecliptic. A first precovery was taken at Steward Observatory in 1992, extending the body's obser... |
(38063)_1999_FH_23523094 | Describe the 'Slow rotator and tumbler' section of the article about '(38063) 1999 FH'. | In September 2014, American astronomer Robert Stephens obtained a rotational lightcurve from photometric observations taken at the Center for Solar System Studies (CS3, U81) in California. It gave an exceptionally long rotation period of 990 hours with a brightness amplitude of 0.55 magnitude (U=2), which makes it one ... | [
"(38063) 1999 FH β Orbit and classification\n\norbits the Sun at a distance of 1.7β3.0 AU once every 3 years and 7 months (1,309 days). Its orbit has an eccentricity of 0.29 and an inclination of 12Β° with respect to the ecliptic. A first precovery was taken at Steward Observatory in 1992, extending the body's obser... |
(38063)_1999_FH_23523096 | What information does the article about '(38063) 1999 FH' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 28 March 2002. As of 2018, it has not been named. | [
"(38063) 1999 FH β Orbit and classification\n\norbits the Sun at a distance of 1.7β3.0 AU once every 3 years and 7 months (1,309 days). Its orbit has an eccentricity of 0.29 and an inclination of 12Β° with respect to the ecliptic. A first precovery was taken at Steward Observatory in 1992, extending the body's obser... |
(38063)_1999_FH_23523095 | Reconstruct the content about 'Diameter and albedo' from the article on '(38063) 1999 FH'. | According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, measures 3.395 and 4.17 kilometers in diameter and its surface has an albedo of 0.287 and 0.176, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids o... | [
"(38063) 1999 FH β Orbit and classification\n\norbits the Sun at a distance of 1.7β3.0 AU once every 3 years and 7 months (1,309 days). Its orbit has an eccentricity of 0.29 and an inclination of 12Β° with respect to the ecliptic. A first precovery was taken at Steward Observatory in 1992, extending the body's obser... |
(385250)_2001_DH47_9033130 | Summarize the 'Origin' part of '(385250) 2001 DH47'. | Long-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka, calculations in both directions of time (4.5 Gyr into the past and 4.5 Gyr into the future) indicate that may be a primordial object, perhaps a survivor of the planetesimal populat... | [
"(385250) 2001 DH47\n\n, provisional designation, is a sub-kilometer asteroid and Mars trojan orbiting 60Β° behind the orbit of Mars near the.",
"(385250) 2001 DH47 β Origin\n\nLong-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka... |
(385250)_2001_DH47_9033131 | Reconstruct the content about 'Further reading' from the article on '(385250) 2001 DH47'. | 2001 DH47 Ivashchenko, Y., Ostafijchuk, P., Spahr, T. B. 2007, Minor Planet Electronic Circular, 2007-P09. ; Dynamics of Mars Trojans Scholl, H., Marzari, F., Tricarico, P. 2005, Icarus, Volume 175, Issue 2, pp. 397β408. ; Three new stable L5 Mars Trojans de la Fuente Marcos, C., de la Fuente Marcos, R. 2013, Monthly N... | [
"(385250) 2001 DH47\n\n, provisional designation, is a sub-kilometer asteroid and Mars trojan orbiting 60Β° behind the orbit of Mars near the.",
"(385250) 2001 DH47 β Origin\n\nLong-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka... |
(385250)_2001_DH47_9033128 | Reconstruct the content about 'Discovery, orbit and physical properties' from the article on '(385250) 2001 DH47'. | was discovered on 1 February 2001 by the Spacewatch program, observing from Steward Observatory, Kitt Peak and classified as Mars-crosser by the Minor Planet Center. Its orbit is characterized by low eccentricity (0.035), moderate inclination (24.4ΒΊ) and a semi-major axis of 1.52 AU. Its orbit is well determined as it ... | [
"(385250) 2001 DH47\n\n, provisional designation, is a sub-kilometer asteroid and Mars trojan orbiting 60Β° behind the orbit of Mars near the.",
"(385250) 2001 DH47 β Origin\n\nLong-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka... |
(385250)_2001_DH47_9033129 | Summarize the 'Mars trojan and orbital evolution' part of '(385250) 2001 DH47'. | It was identified as Mars trojan by H. Scholl, F. Marzari and P. Tricarico in 2005 and its dynamical half-lifetime was found to be of the order of the age of the Solar System. Recent calculations confirm that it is indeed a stable Mars trojan with a libration period of 1365 yr and an amplitude of 11Β°. These values as w... | [
"(385250) 2001 DH47\n\n, provisional designation, is a sub-kilometer asteroid and Mars trojan orbiting 60Β° behind the orbit of Mars near the.",
"(385250) 2001 DH47 β Origin\n\nLong-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka... |
(385343)_2002_LV_26180705 | Reconstruct the content about 'Close approaches' from the article on '(385343) 2002 LV'. | The asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in July 2002 at 0.112 AU. Its closest near-Earth ... | [
"(385343) 2002 LV β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in Ju... |
(385343)_2002_LV_26180706 | What information does the article about '(385343) 2002 LV' provide on 'Physical characteristics'? | Observations with the Spitzer Telescope characterized this object as an Sr-subtype that transitions from the common, stony S-type asteroids to the uncommon R-types. | [
"(385343) 2002 LV β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in Ju... |
(385343)_2002_LV_26180708 | Describe the 'Diameter and albedo' section of the article about '(385343) 2002 LV'. | According to post-cryogenic observations with the Spitzer Telescope during the ExploreNEOs survey, and observations carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures between 1.359 and 1.73 kilometers in diameter and its surface has an albedo between 0.15 and 0.2158... | [
"(385343) 2002 LV β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in Ju... |
(385343)_2002_LV_26180707 | Explain what '(385343) 2002 LV' covers in the 'Rotation period' section. | In July 2002, a rotational lightcurve of this asteroid was obtained from photometric observations by Petr Pravec at OndΕejov Observatory in the Czech Republic. Lightcurve analysis gave a well-defined rotation period of 6.195 hours with a high brightness amplitude of 0.93 magnitude, indicative for an elongated, non-sphe... | [
"(385343) 2002 LV β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in Ju... |
(385343)_2002_LV_26180704 | From the article on '(385343) 2002 LV', restate the 'Orbit and classification' content. | 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 0.9β3.7 AU once every 3 years and 6 months (1,286 days; semi-major axis of 2.31 AU). Its orbit has an eccentricity of 0.61 and an inclinat... | [
"(385343) 2002 LV β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in Ju... |
(385343)_2002_LV_26180703 | Describe the content of the article about '(385343) 2002 LV'. | (385343) 2002 LV, provisional designation, is a stony asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.5 km in diameter. It was discovered on 1 June 2002, by astronomers with the Lincoln Near-Earth Asteroid Research at the Linc... | [
"(385343) 2002 LV β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in Ju... |
(385343)_2002_LV_26180709 | What information does the article about '(385343) 2002 LV' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 14 February 2014 (M.P.C. 87072). As of 2018, it has not been named. | [
"(385343) 2002 LV β Close approaches\n\nThe asteroid has an Earth minimum orbital intersection distance of 0.0071 AU, which corresponds to 2.7 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In August 1935, it approached Earth at a nominal distance of 0.035 AU, and in Ju... |
(386454)_2008_XM_23050669 | Based on the article about '(386454) 2008 XM', describe the 'Physical characteristics' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 367 meters in diameter and its surface has an albedo of 0.128. As of 2016, the body's composition and spectral type, as well as its rotation period and shape remains unknown. | [
"(386454) 2008 XM β Physical characteristics\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 367 meters in diameter and its surface has an albedo of 0.128. As of 2016, the body's composition and spectral type, as well as its rotation... |
(386454)_2008_XM_23050668 | What information does the article about '(386454) 2008 XM' provide on 'Orbit and classification'? | The asteroid orbits the Sun at a distance of 0.1β2.3 AU once every 16 months (494 days). Its orbit has an eccentricity of 0.91 and an inclination of 5Β° with respect to the ecliptic. Due to its outstanding eccentricity, it is also a Mercury-crosser, Venus-crosser and Mars-crosser. It has the third-smallest perihelion of... | [
"(386454) 2008 XM β Physical characteristics\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 367 meters in diameter and its surface has an albedo of 0.128. As of 2016, the body's composition and spectral type, as well as its rotation... |
(386454)_2008_XM_23050667 | Summarize the following section from the article on '(386454) 2008 XM'. | (386454) 2008 XM is a highly eccentric, sub-kilometer-sized asteroid, with one of the smallest known perihelions among all minor planets. It is classified as near-Earth object of the Apollo group and was discovered on 2 December 2008, by the LINEAR program at Lincoln Laboratory's Experimental Test Site in Socorro, New ... | [
"(386454) 2008 XM β Physical characteristics\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 367 meters in diameter and its surface has an albedo of 0.128. As of 2016, the body's composition and spectral type, as well as its rotation... |
(386723)_2009_YE7_314509 | Describe the 'Absolute magnitude' section of the article about '(386723) 2009 YE7'. | an albedo of 0.09. However, it is probably much smaller than previously thought, since it is also suspected of being a highly reflective icy member of the Haumea family. has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detection of water ice on its surface. This means c... | [
"(386723) 2009 YE7 β Absolute magnitude\n\nan albedo of 0.09. However, it is probably much smaller than previously thought, since it is also suspected of being a highly reflective icy member of the Haumea family. has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detec... |
(386723)_2009_YE7_314506 | Based on the article about '(386723) 2009 YE7', describe the 'Classification' section. | is a classical Kuiper belt object: Its orbit is not controlled by an orbital resonance with Neptune, similar to 15760 Albion, but with a much greater orbital eccentricity and inclination. It completes one orbit around the Sun in just over 247 Earth years, at an average distance of about 44 AU. It came to perihelion aro... | [
"(386723) 2009 YE7 β Absolute magnitude\n\nan albedo of 0.09. However, it is probably much smaller than previously thought, since it is also suspected of being a highly reflective icy member of the Haumea family. has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detec... |
(386723)_2009_YE7_314507 | Based on the article about '(386723) 2009 YE7', describe the 'Precovery' section. | has been observed 70 times, with precovery images dating back to 2006, and has an orbital quality code of 4. | [
"(386723) 2009 YE7 β Absolute magnitude\n\nan albedo of 0.09. However, it is probably much smaller than previously thought, since it is also suspected of being a highly reflective icy member of the Haumea family. has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detec... |
(386723)_2009_YE7_314508 | Based on the article about '(386723) 2009 YE7', describe the 'Absolute magnitude' section. | The size of an object can be ascertained once its absolute magnitude (H) and its albedo (the proportion of light it reflects) are known. When was first discovered, it was believed to have an absolute magnitude (H) of 2.8, which would have made it the first bright KBO found from the southern hemisphere. has an absolut... | [
"(386723) 2009 YE7 β Absolute magnitude\n\nan albedo of 0.09. However, it is probably much smaller than previously thought, since it is also suspected of being a highly reflective icy member of the Haumea family. has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detec... |
(386723)_2009_YE7_314505 | Summarize the following section from the article on '(386723) 2009 YE7'. | ''', provisional designation ', is a trans-Neptunian object (TNO) discovered by David Rabinowitz on December 17, 2009 at the La Silla Observatory in Chile. | [
"(386723) 2009 YE7 β Absolute magnitude\n\nan albedo of 0.09. However, it is probably much smaller than previously thought, since it is also suspected of being a highly reflective icy member of the Haumea family. has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detec... |
(388188)_2006_DP14_23662981 | Describe the 'Physical characteristics' section of the article about '(388188) 2006 DP14'. | is an assumed stony S-type asteroid. This asteroid is a typical contact binary, with two distinctive lobes on either end that appear to be in contact, giving it a peanut-like shape. | [
"(388188) 2006 DP14 β Physical characteristics\n\nis an assumed stony S-type asteroid. This asteroid is a typical contact binary, with two distinctive lobes on either end that appear to be in contact, giving it a peanut-like shape.",
"(388188) 2006 DP14 β Close approaches\n\nThe asteroid has an Earth minimum orbi... |
(388188)_2006_DP14_23662980 | Describe the 'Close approaches' section of the article about '(388188) 2006 DP14'. | The asteroid has an Earth minimum orbit intersection distance (MOID) of 0.0163 AU, which corresponds to 6.4 lunar distances (LD). On 10 February 2014, it passed Earth close to this theoretical minimum distance at 6.25 LD, or 0.016032 AU. This makes is a potentially hazardous asteroid (PHA), a body with a threatening cl... | [
"(388188) 2006 DP14 β Physical characteristics\n\nis an assumed stony S-type asteroid. This asteroid is a typical contact binary, with two distinctive lobes on either end that appear to be in contact, giving it a peanut-like shape.",
"(388188) 2006 DP14 β Close approaches\n\nThe asteroid has an Earth minimum orbi... |
(388188)_2006_DP14_23662978 | Summarize the following section from the article on '(388188) 2006 DP14'. | ''', provisional designation ', is a sub-kilometer sized, peanut-shaped asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. This contact binary was discovered on 23 February 2006, by astronomers of the LINEAR program at the Lincoln Laboratory's E... | [
"(388188) 2006 DP14 β Physical characteristics\n\nis an assumed stony S-type asteroid. This asteroid is a typical contact binary, with two distinctive lobes on either end that appear to be in contact, giving it a peanut-like shape.",
"(388188) 2006 DP14 β Close approaches\n\nThe asteroid has an Earth minimum orbi... |
(388188)_2006_DP14_23662982 | What information does the article about '(388188) 2006 DP14' provide on 'Diameter, shape and albedo'? | On the night of 11 February 2014, NASA scientists conducted a radar imaging session using the 70-meter dish at Goldstone Observatory. These observations, using delay-Doppler radar imaging, revealed a 400Γ200 meters sized body, while the Collaborative Asteroid Lightcurve Link calculates a diameter of almost 500 meters, ... | [
"(388188) 2006 DP14 β Physical characteristics\n\nis an assumed stony S-type asteroid. This asteroid is a typical contact binary, with two distinctive lobes on either end that appear to be in contact, giving it a peanut-like shape.",
"(388188) 2006 DP14 β Close approaches\n\nThe asteroid has an Earth minimum orbi... |
(388188)_2006_DP14_23662979 | From the article on '(388188) 2006 DP14', restate the 'Classification and orbit' content. | is a member of the Apollo group, which are Earth-crossing asteroids and the largest group of near-Earth asteroids. It orbits the Sun at a distance of 0.3β2.4 AU once every 19 months (583 days; semi-major axis of 1.37 AU). Its orbit has a high eccentricity of 0.78 and an inclination of 12Β° with respect to the ecliptic. ... | [
"(388188) 2006 DP14 β Physical characteristics\n\nis an assumed stony S-type asteroid. This asteroid is a typical contact binary, with two distinctive lobes on either end that appear to be in contact, giving it a peanut-like shape.",
"(388188) 2006 DP14 β Close approaches\n\nThe asteroid has an Earth minimum orbi... |
(38984)_2000_UZ4_27855278 | Explain what '(38984) 2000 UZ4' covers in the 'Orbit and classification' section. | 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 unstable Griqua group, the orbits of the Zhongguos are stable over half a bil... | [
"(38984) 2000 UZ4 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 unstable Griqua group, th... |
(38984)_2000_UZ4_27855282 | What information does the article about '(38984) 2000 UZ4' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 28 March 2002, after its orbit had sufficiently been secured (M.P.C. 45198). As of 2018, it has not been named. | [
"(38984) 2000 UZ4 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 unstable Griqua group, th... |
(38984)_2000_UZ4_27855280 | What information does the article about '(38984) 2000 UZ4' provide on 'Rotation period'? | In January 2014, a rotational lightcurve of this asteroid was obtained from photometric observations in the R-band by astronomers at the Intermediate Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 19.20 hours with a high brightness amplitude of 0.70 magnitude, indicative of an el... | [
"(38984) 2000 UZ4 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 unstable Griqua group, th... |
(38984)_2000_UZ4_27855277 | Summarize the following section from the article on '(38984) 2000 UZ4'. | , provisional designation, is carbonaceous Zhongguo asteroid from the outermost regions of the asteroid belt, approximately 5 km in diameter. It was discovered on 24 October 2000, by astronomers with Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the... | [
"(38984) 2000 UZ4 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 unstable Griqua group, th... |
(38984)_2000_UZ4_27855281 | From the article on '(38984) 2000 UZ4', restate the 'Diameter and albedo' content. | The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057 and calculates a diameter of 4.87 kilometers based on an absolute magnitude of 15.29. | [
"(38984) 2000 UZ4 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 unstable Griqua group, th... |
(391211)_2006_HZ51_1206262 | What does the article about '(391211) 2006 HZ51' say regarding 'Rotation period'? | As of 2018, n rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remains unknown. | [
"(391211) 2006 HZ51 β Naming\n\nThis minor planet has not yet been named.",
"(391211) 2006 HZ51 β Rotation period\n\nAs of 2018, n rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remains unknown.",
"(391211) 2006 HZ51 β Orbit and classificatio... |
(391211)_2006_HZ51_1206259 | Summarize the 'Orbit and classification' part of '(391211) 2006 HZ51'. | is an Amor asteroid β a subgroup of near-Earth asteroids that approach the orbit of Earth from beyond, but do not cross it. It orbits the Sun at a distance of 1.04β2.75 AU once every 2 years and 7 months (955 days; semi-major axis of 1.90 AU). Its orbit has an eccentricity of 0.45 and an inclination of 12Β° with respect... | [
"(391211) 2006 HZ51 β Naming\n\nThis minor planet has not yet been named.",
"(391211) 2006 HZ51 β Rotation period\n\nAs of 2018, n rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remains unknown.",
"(391211) 2006 HZ51 β Orbit and classificatio... |
(391211)_2006_HZ51_1206261 | Summarize the 'Diameter and albedo' part of '(391211) 2006 HZ51'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 412 meters in diameter and its surface has an exceptionally high albedo of 0.415. Other source give an estimated diameter of 800 meters. | [
"(391211) 2006 HZ51 β Naming\n\nThis minor planet has not yet been named.",
"(391211) 2006 HZ51 β Rotation period\n\nAs of 2018, n rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remains unknown.",
"(391211) 2006 HZ51 β Orbit and classificatio... |
(391211)_2006_HZ51_1206260 | What does the article about '(391211) 2006 HZ51' say regarding 'Close approaches'? | has a minimum orbital intersection distance (MOID) with Earth of 0.035385 AU, which translates into 13.8 lunar distances. This makes it a potentially hazardous asteroid, a body with a threatening close approach to the Earth, due to its low MOID and large size (absolute magnitude of 18.5). Such asteroids are defined to ... | [
"(391211) 2006 HZ51 β Naming\n\nThis minor planet has not yet been named.",
"(391211) 2006 HZ51 β Rotation period\n\nAs of 2018, n rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remains unknown.",
"(391211) 2006 HZ51 β Orbit and classificatio... |
(392741)_2012_SQ31_27484339 | Based on the article about '(392741) 2012 SQ31', describe the 'Trans-Neptunian object' section. | On 11 August 2004, the asteroid was already observed as by astronomers at the Cerro Tololo Inter-American Observatory in Chile, but became a lost minor planet until 2012 due to a lack of follow-up observations. During this time, and with only two observations taken on the same day, it was thought to be a trans-Neptunia... | [
"(392741) 2012 SQ31 β Trans-Neptunian object\n\nOn 11 August 2004, the asteroid was already observed as by astronomers at the Cerro Tololo Inter-American Observatory in Chile, but became a lost minor planet until 2012 due to a lack of follow-up observations. During this time, and with only two observations taken on... |
(392741)_2012_SQ31_27484337 | Summarize the following section from the article on '(392741) 2012 SQ31'. | , provisional designation, is a sub-kilometer Florian asteroid from the inner regions of the asteroid belt, approximately 700 m in diameter. It was originally considered a trans-Neptunian object and lost minor planet during 2004β2012. The date of the official discovery was later set to 27 December 2009, and credited to... | [
"(392741) 2012 SQ31 β Trans-Neptunian object\n\nOn 11 August 2004, the asteroid was already observed as by astronomers at the Cerro Tololo Inter-American Observatory in Chile, but became a lost minor planet until 2012 due to a lack of follow-up observations. During this time, and with only two observations taken on... |
(392741)_2012_SQ31_27484338 | Reconstruct the content about 'Orbit and classification' from the article on '(392741) 2012 SQ31'. | a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt. It orbits the Sun in the inner asteroid belt at a distance of 1.9β2.6 AU once every 3 years and 5 months (1,242 days; semi-major axis of 2.26 AU). Its orbit has an eccentricity of 0.14 and an inclinat... | [
"(392741) 2012 SQ31 β Trans-Neptunian object\n\nOn 11 August 2004, the asteroid was already observed as by astronomers at the Cerro Tololo Inter-American Observatory in Chile, but became a lost minor planet until 2012 due to a lack of follow-up observations. During this time, and with only two observations taken on... |
(392741)_2012_SQ31_27484340 | Summarize the 'Physical characteristics' part of '(392741) 2012 SQ31'. | has been characterized as a member of the Flora family, which are stony S-type asteroids with albedo typically around 0.24, corresponding to that of the family's parent body, 8 Flora. Based on a generic magnitude-to-diameter conversion, measures 690 meters for an absolute magnitude of 18.0 and an assumed albedo of 0.24... | [
"(392741) 2012 SQ31 β Trans-Neptunian object\n\nOn 11 August 2004, the asteroid was already observed as by astronomers at the Cerro Tololo Inter-American Observatory in Chile, but became a lost minor planet until 2012 due to a lack of follow-up observations. During this time, and with only two observations taken on... |
(392741)_2012_SQ31_27484341 | Summarize the 'Numbering and naming' part of '(392741) 2012 SQ31'. | This minor planet was numbered by the Minor Planet Center on 15 April 2014 (M.P.C. 87941). As of 2018, it has not been named. | [
"(392741) 2012 SQ31 β Trans-Neptunian object\n\nOn 11 August 2004, the asteroid was already observed as by astronomers at the Cerro Tololo Inter-American Observatory in Chile, but became a lost minor planet until 2012 due to a lack of follow-up observations. During this time, and with only two observations taken on... |
(394130)_2006_HY51_1205893 | Reconstruct the content about 'Physical characteristics' from the article on '(394130) 2006 HY51'. | According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, measures 1.218 kilometers in diameter and its surface has an albedo of 0.157. The asteroid's composition and shape, as well as its rotation period remain unknown. It has an absolute magnitude of 17.2. | [
"(394130) 2006 HY51 β Naming\n\nAs of 2017, this minor planet remains unnamed.",
"(394130) 2006 HY51 β Physical characteristics\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, measures 1.218 kilometers in diameter and its surface has an alb... |
(394130)_2006_HY51_1205892 | Describe the 'Orbit and classification' section of the article about '(394130) 2006 HY51'. | orbits the Sun at a distance of 0.1β5.1 AU once every 4 years and 2 months (1,527 days). Its orbit has an eccentricity of 0.97 and an inclination of 33Β° with respect to the ecliptic. It is the asteroid with the third-smallest known perihelion of any known object orbiting the Sun. Its extreme orbital eccentricity brings... | [
"(394130) 2006 HY51 β Naming\n\nAs of 2017, this minor planet remains unnamed.",
"(394130) 2006 HY51 β Physical characteristics\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, measures 1.218 kilometers in diameter and its surface has an alb... |
(394130)_2006_HY51_1205891 | Summarize the following section from the article on '(394130) 2006 HY51'. | is a near-Earth object of the Apollo asteroid group with a high orbital eccentricity, approximately 1.2 kilometers in diameter. It was discovered on 26 April 2006, by LINEAR at Lincoln Lab's ETS in Socorro, New Mexico, United States. | [
"(394130) 2006 HY51 β Naming\n\nAs of 2017, this minor planet remains unnamed.",
"(394130) 2006 HY51 β Physical characteristics\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, measures 1.218 kilometers in diameter and its surface has an alb... |
(39546)_1992_DT5_13639289 | Summarize the 'Orbit and classification' part of '(39546) 1992 DT5'. | is an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50β100 kilometer-sized, carbon-rich parent body within the past several hundred million years. The family consist of nearly 2000 known members and its namesake is the aste... | [
"(39546) 1992 DT5 β Orbit and classification\n\nis an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50β100 kilometer-sized, carbon-rich parent body within the past several hundred million years. The family consist of ne... |
(39546)_1992_DT5_13639293 | Describe the 'Numbering and naming' section of the article about '(39546) 1992 DT5'. | This minor planet was numbered by the Minor Planet Center on 26 May 2002 (M.P.C. 45660). As of 2018, it has not been named. | [
"(39546) 1992 DT5 β Orbit and classification\n\nis an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50β100 kilometer-sized, carbon-rich parent body within the past several hundred million years. The family consist of ne... |
(39546)_1992_DT5_13639288 | What information does the article about '(39546) 1992 DT5' provide? | is a dark Hoffmeister asteroid and exceptionally slow rotator from the central region of the asteroid belt, approximately 5.3 km in diameter. The likely elongated C-type asteroid was discovered on 29 February 1992, by the UppsalaβESO Survey of Asteroids and Comets at ESO's La Silla astronomical observatory site in nort... | [
"(39546) 1992 DT5 β Orbit and classification\n\nis an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50β100 kilometer-sized, carbon-rich parent body within the past several hundred million years. The family consist of ne... |
(39546)_1992_DT5_13639291 | Explain what '(39546) 1992 DT5' covers in the 'Rotation period' section. | In September 2013, a rotational lightcurve for this asteroid was obtained from photometric observations in the R-band at the Palomar Transient Factory in California. It gave an exceptionally long rotation period of 1167 hours with an estimated error margin of Β±100 hours. According to the Light Curve Data Base (LCDB), i... | [
"(39546) 1992 DT5 β Orbit and classification\n\nis an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50β100 kilometer-sized, carbon-rich parent body within the past several hundred million years. The family consist of ne... |
(39546)_1992_DT5_13639290 | Describe the 'Physical characteristics' section of the article about '(39546) 1992 DT5'. | is an assumed carbonaceous C-type asteroid. The overall spectral type of the Hoffmeister family is that of an C- and F-type. | [
"(39546) 1992 DT5 β Orbit and classification\n\nis an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50β100 kilometer-sized, carbon-rich parent body within the past several hundred million years. The family consist of ne... |
(39546)_1992_DT5_13639292 | Reconstruct the content about 'Diameter and albedo' from the article on '(39546) 1992 DT5'. | The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057 and calculates a diameter of 5.3 kilometers based on an absolute magnitude of 15.09. | [
"(39546) 1992 DT5 β Orbit and classification\n\nis an attributed member of the very compact Hoffmeister family (519), which, based upon its low albedo, was most likely formed from the breakup of a 50β100 kilometer-sized, carbon-rich parent body within the past several hundred million years. The family consist of ne... |
(4+3)_cycloaddition_32975397 | Summarize the following section from the article on '(4+3) cycloaddition'. | Symmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-membered rings. A number of dienes have been empl... | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(4+3)_cycloaddition_32975401 | What does the article about '(4+3) cycloaddition' say regarding 'Scope and limitations'? | Reduction of Ξ±,Ξ±'-dihalo ketones is an effective method for the generation of oxyallyl cations for cycloaddition. Reducing agents used include copper-bronze., iron carbonyl complexes., and copper/zinc As mentioned previously, products exhibiting trans stereochemistry between the bridging atom and the oxyallyl substitue... | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(4+3)_cycloaddition_32975400 | Explain what '(4+3) cycloaddition' covers in the 'Stereochemistry' section. | Stereochemical control in the (4+3) cycloaddition is not as strict as in the Diels-Alder reaction, because the former often proceed through stepwise, polar pathways. Even when the reaction is concerted, complications may arise due to conformational dynamics in the oxyallyl component, which can exist in "W," "U," or "si... | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(4+3)_cycloaddition_32975403 | What information does the article about '(4+3) cycloaddition' provide on 'Comparison with other methods'? | Compared to annulations that form five- and six-membered rings, annulations that form seven-membered rings are relatively rare. Classical methods of cyclising linear precursors by the formation of a single carbon-carbon bond (such as the Prins reaction, shown below) form seven-membered rings efficiently in some cases. ... | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(4+3)_cycloaddition_32975404 | Summarize the 'Typical conditions' part of '(4+3) cycloaddition'. | Cycloadditions carried out under reductive conditions can generally be effected with commercially available reducing agents, although a few reducing agents require special preparation. Reductive reactions employing iron carbonyl complexes should be carried out in a well-ventilated fume hood, as free carbon monoxide may... | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(4+3)_cycloaddition_32975396 | Describe the content of the article about '(4+3) cycloaddition'. | A (4+3) cycloaddition is a cycloaddition between a four-atom Ο-system and a three-atom Ο-system to form a seven-membered ring. Allyl or oxyallyl cations (propenylium-2-olate) are commonly used three-atom Ο-systems, while a diene (such as butadiene) plays the role of the four-atom Ο-system. It represents one of the rela... | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(4+3)_cycloaddition_32975398 | Summarize the 'Prevailing mechanism' part of '(4+3) cycloaddition'. | Oxyallyl cations (propenyliumolates) may be generated under reductive, mildly basic, or photolytic conditions. Reduction of Ξ±,Ξ±'-dihalo ketones is a very popular method for generating symmetric oxyallyl cations. After formation of a metal enolate, dissociation of halide generates a positively charged oxyallyl intermedi... | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(4+3)_cycloaddition_32975402 | Based on the article about '(4+3) cycloaddition', describe the 'Synthetic applications' section. | A synthesis of Prelog-Djerassi lactone illustrates how stereocenters set during a (4+3) cyclization may be used later for stereochemical control. The oxabicyclo[3.2.1]octane products of cycloadditions involving furan may be opened using a variety of methods (8) | [
"(4+3) cycloaddition β Introduction\n\nSymmetry-allowed (4+3) cycloaddition is an attractive method for the formation of historically difficult-to-access seven-membered rings. Neutral dienes and cationic allyl systems (most commonly oxyallyl cations) may react in a concerted or stepwise fashion to give seven-member... |
(40314)_1999_KR16_26812674 | Based on the article about '(40314) 1999 KR16', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 26 May 2002. As of 2019, it has not been named. | [
"(40314) 1999 KR16 β Physical characteristics\n\nhas two solutions of its rotation period of 6 and 12 hours, respectively, and an albedo of 0.20.",
"(40314) 1999 KR16 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 May 2002. As of 2019, it has not been named.",
"(40314)... |
(40314)_1999_KR16_26812673 | What does the article about '(40314) 1999 KR16' say regarding 'Orbit and classification'? | The minor planet orbits the Sun at a distance of 34β65 AU once every 346 years (126,383 days; semi-major axis of 49.29 AU). Its orbit has an eccentricity of 0.31 and an inclination of 25Β° with respect to the ecliptic. | [
"(40314) 1999 KR16 β Physical characteristics\n\nhas two solutions of its rotation period of 6 and 12 hours, respectively, and an albedo of 0.20.",
"(40314) 1999 KR16 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 May 2002. As of 2019, it has not been named.",
"(40314)... |
(40314)_1999_KR16_26812672 | Summarize the following section from the article on '(40314) 1999 KR16'. | is a trans-Neptunian object on an eccentric orbit in the outermost region of the Solar System, approximately 254 km in diameter. It was discovered on 16 May 1999, by French astronomer Audrey Delsanti and Oliver Hainaut at ESOs La Silla Observatory in northern Chile. The very reddish object is a dwarf planet candidate a... | [
"(40314) 1999 KR16 β Physical characteristics\n\nhas two solutions of its rotation period of 6 and 12 hours, respectively, and an albedo of 0.20.",
"(40314) 1999 KR16 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 26 May 2002. As of 2019, it has not been named.",
"(40314)... |
(410777)_2009_FD_23181592 | What information does the article about '(410777) 2009 FD' provide on 'Future approaches'? | The JPL Small-Body Database shows that will make two very close approaches in the late 22nd century, in 2185 and 2190. As of 2016, the approach of 29 March 2185 had a 1 in 710 chance of impacting Earth. The nominal 2185 Earth approach distance was 0.009 AU. Orbit determination for 2190 is complicated by the 2185 close ... | [
"(410777) 2009 FD β Future approaches\n\nThe JPL Small-Body Database shows that will make two very close approaches in the late 22nd century, in 2185 and 2190. As of 2016, the approach of 29 March 2185 had a 1 in 710 chance of impacting Earth. The nominal 2185 Earth approach distance was 0.009 AU. Orbit determinati... |
(410777)_2009_FD_23181589 | Summarize the following section from the article on '(410777) 2009 FD'. | (410777) 2009 FD is a carbonaceous sub-kilometer asteroid and binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, discovered on 24 February 2009 by astronomers of the Spacewatch program at Kitt Peak National Observatory near Tucson, Arizona, in the United States. Until... | [
"(410777) 2009 FD β Future approaches\n\nThe JPL Small-Body Database shows that will make two very close approaches in the late 22nd century, in 2185 and 2190. As of 2016, the approach of 29 March 2185 had a 1 in 710 chance of impacting Earth. The nominal 2185 Earth approach distance was 0.009 AU. Orbit determinati... |
(410777)_2009_FD_23181591 | Explain what '(410777) 2009 FD' covers in the 'Binary' section. | NASA's Near Earth Program originally estimated its size to be 130 metres in diameter based on an assumed albedo of 0.15. This gave it an estimated mass of around 2,800,000 tonnes. But work by Amy Mainzer using NEOWISE data in 2014 showed that it could be as large as 472 metres with an albedo as low as 0.01. Because (K0... | [
"(410777) 2009 FD β Future approaches\n\nThe JPL Small-Body Database shows that will make two very close approaches in the late 22nd century, in 2185 and 2190. As of 2016, the approach of 29 March 2185 had a 1 in 710 chance of impacting Earth. The nominal 2185 Earth approach distance was 0.009 AU. Orbit determinati... |
(410777)_2009_FD_23181594 | Explain what '(410777) 2009 FD' covers in the 'Past Earth-impact estimates' section. | 14 June 2019, Alessio Del Vigna and colleagues published a new analysis, which incorporates astrometry taken in 2019. Using both JPL's Sentry as well as NEODyS's CLOMON-2 system, the new data allowed a 4-sigma detection of the Yarkovsky effect at 3.6 AU/Myr. The 2019 observations extended the observation arc from six y... | [
"(410777) 2009 FD β Future approaches\n\nThe JPL Small-Body Database shows that will make two very close approaches in the late 22nd century, in 2185 and 2190. As of 2016, the approach of 29 March 2185 had a 1 in 710 chance of impacting Earth. The nominal 2185 Earth approach distance was 0.009 AU. Orbit determinati... |
(410777)_2009_FD_23181593 | Reconstruct the content about 'Past Earth-impact estimates' from the article on '(410777) 2009 FD'. | In January 2011, near-Earth asteroid (with observations through 7 December 2010) was listed on the JPL Sentry Risk Table with a 1 in 435 chance of impacting Earth on 29 March 2185. In 2014 (with observations through 5 February 2014, creating an observation arc of 1807 days) the potential 2185 impact was ruled out. Usin... | [
"(410777) 2009 FD β Future approaches\n\nThe JPL Small-Body Database shows that will make two very close approaches in the late 22nd century, in 2185 and 2190. As of 2016, the approach of 29 March 2185 had a 1 in 710 chance of impacting Earth. The nominal 2185 Earth approach distance was 0.009 AU. Orbit determinati... |
(410777)_2009_FD_23181590 | What information does the article about '(410777) 2009 FD' provide on 'Discovery'? | was initially announced as discovered on 16 March 2009 by La Sagra Sky Survey. Because there were previous observations found in images taken by the Spacewatch survey some 3 weeks prior, on 24 February 2009, the Minor Planet Center assigned the discovery credit to Spacewatch under the discovery assignment rules. made a... | [
"(410777) 2009 FD β Future approaches\n\nThe JPL Small-Body Database shows that will make two very close approaches in the late 22nd century, in 2185 and 2190. As of 2016, the approach of 29 March 2185 had a 1 in 710 chance of impacting Earth. The nominal 2185 Earth approach distance was 0.009 AU. Orbit determinati... |
(416151)_2002_RQ25_28125931 | From the article on '(416151) 2002 RQ25', restate the 'Orbit and classification' content. | orbits the Sun at a distance of 0.8β1.5 AU once every 1 years and 2 months (428 days). Its orbit has an eccentricity of 0.31 and an inclination of 5Β° with respect to the ecliptic. The asteroid's minimum orbit intersection distance with Earth is 0.0499 AU, which is currently exactly at the threshold limit of 0.05 AU (or... | [
"(416151) 2002 RQ25 β Orbit and classification\n\norbits the Sun at a distance of 0.8β1.5 AU once every 1 years and 2 months (428 days). Its orbit has an eccentricity of 0.31 and an inclination of 5Β° with respect to the ecliptic. The asteroid's minimum orbit intersection distance with Earth is 0.0499 AU, which is c... |
(416151)_2002_RQ25_28125932 | Describe the 'Physical characteristics' section of the article about '(416151) 2002 RQ25'. | The carbonaceous C-type asteroid is also classified as a C/X-type body according to the survey carried out by NASA's Spitzer Space Telescope. | [
"(416151) 2002 RQ25 β Orbit and classification\n\norbits the Sun at a distance of 0.8β1.5 AU once every 1 years and 2 months (428 days). Its orbit has an eccentricity of 0.31 and an inclination of 5Β° with respect to the ecliptic. The asteroid's minimum orbit intersection distance with Earth is 0.0499 AU, which is c... |
(416151)_2002_RQ25_28125930 | Describe the content of the article about '(416151) 2002 RQ25'. | is a carbonaceous asteroid of the Apollo group, classified as near-Earth object and potentially hazardous asteroid, approximately 0.2 kilometers in diameter. It was discovered on 3 September 2002, by the Campo Imperatore Near-Earth Object Survey (CINEOS) at the Italian Campo Imperatore Observatory, located in the Abruz... | [
"(416151) 2002 RQ25 β Orbit and classification\n\norbits the Sun at a distance of 0.8β1.5 AU once every 1 years and 2 months (428 days). Its orbit has an eccentricity of 0.31 and an inclination of 5Β° with respect to the ecliptic. The asteroid's minimum orbit intersection distance with Earth is 0.0499 AU, which is c... |
(416151)_2002_RQ25_28125933 | Explain what '(416151) 2002 RQ25' covers in the 'Lightcurve' section. | A rotational lightcurve of was obtained from photometric observations made by American astronomer Brian Warner at his Palmer Divide Observatory, Colorado, in February 2015. The ambiguous lightcurve rendered a rotation period of 12.191 hours with a brightness variation of 0.72 magnitude (U=2+), while a second solution g... | [
"(416151) 2002 RQ25 β Orbit and classification\n\norbits the Sun at a distance of 0.8β1.5 AU once every 1 years and 2 months (428 days). Its orbit has an eccentricity of 0.31 and an inclination of 5Β° with respect to the ecliptic. The asteroid's minimum orbit intersection distance with Earth is 0.0499 AU, which is c... |
(417634)_2006_XG1_1917809 | What information does the article about '(417634) 2006 XG1' provide on 'Description'? | Originally listed with a Torino Scale hazard rating of 0, this was raised to a rating of 1 on 22 December 2006 as a result of additional observations and refinement of the orbital calculations. However, on 9 January 2007 it was returned to a rating of 0. It was removed from the Sentry Risk Table on 7 February 2007. It ... | [
"(417634) 2006 XG1 β Description\n\nOriginally listed with a Torino Scale hazard rating of 0, this was raised to a rating of 1 on 22 December 2006 as a result of additional observations and refinement of the orbital calculations. However, on 9 January 2007 it was returned to a rating of 0. It was removed from the S... |
(417634)_2006_XG1_1917808 | Describe the content of the article about '(417634) 2006 XG1'. | provisional designation, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, that had a low but non-zero probability of impacting Earth on 31 October 2041. The asteroid was discovered on 20 September 2006, by astronomers of the Catalina Sky Survey, using ... | [
"(417634) 2006 XG1 β Description\n\nOriginally listed with a Torino Scale hazard rating of 0, this was raised to a rating of 1 on 22 December 2006 as a result of additional observations and refinement of the orbital calculations. However, on 9 January 2007 it was returned to a rating of 0. It was removed from the S... |
(417634)_2006_XG1_1917810 | Explain what '(417634) 2006 XG1' covers in the 'Physical characteristics' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 418 meters in diameter and its surface has an albedo of 0.154. Previously, JPL's Sentry System estimated a diameter of 670 meters with a mass of 4.2 kg. | [
"(417634) 2006 XG1 β Description\n\nOriginally listed with a Torino Scale hazard rating of 0, this was raised to a rating of 1 on 22 December 2006 as a result of additional observations and refinement of the orbital calculations. However, on 9 January 2007 it was returned to a rating of 0. It was removed from the S... |
(419624)_2010_SO16_22985802 | Describe the content of the article about '(419624) 2010 SO16'. | is a sub-kilometer asteroid in a co-orbital configuration with Earth, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered by the Wide-field Infrared Survey Explorer space telescope (WISE) on 17 September 2010. | [
"(419624) 2010 SO16\n\nis a sub-kilometer asteroid in a co-orbital configuration with Earth, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered by the Wide-field Infrared Survey Explorer space telescope (WISE) on 17 September 2010.",
"(419624) 2010 SO16 β Des... |
(419624)_2010_SO16_22985804 | Based on the article about '(419624) 2010 SO16', describe the 'Description' section. | its orbit is neither less than nor greater than 1 AU, but oscillates between approximately 0.996 and 1.004 AU, with a period of about 350 years. In its ~350 yr horseshoe cycle, it never approaches Earth more closely than about 0.15 AU, alternately trailing and leading. According to various simulations will remain in th... | [
"(419624) 2010 SO16\n\nis a sub-kilometer asteroid in a co-orbital configuration with Earth, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered by the Wide-field Infrared Survey Explorer space telescope (WISE) on 17 September 2010.",
"(419624) 2010 SO16 β Des... |
(419624)_2010_SO16_22985803 | Reconstruct the content about 'Description' from the article on '(419624) 2010 SO16'. | The orbit was described by Apostolos Christou and David Asher at the Armagh Observatory in Northern Ireland. The object has an absolute magnitude of 20.5. Observations by the discovering WISE telescope give a diameter of 357 meters and an albedo of 0.084. has a horseshoe orbit that allows it to stably share Earth's orb... | [
"(419624) 2010 SO16\n\nis a sub-kilometer asteroid in a co-orbital configuration with Earth, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered by the Wide-field Infrared Survey Explorer space telescope (WISE) on 17 September 2010.",
"(419624) 2010 SO16 β Des... |
(42301)_2001_UR163_3107907 | Reconstruct the content about 'Classification and orbit' from the article on '(42301) 2001 UR163'. | has been characterized as a dwarf planet candidate. Based on assumptions and estimates, Michael Brown gives it a "likely"-status on his website, which is the third highest status after "near certainty" and "highly likely" (also see his classification table). The object orbits the Sun at a distance of 37.0β66.6 AU once ... | [
"(42301) 2001 UR163 β Classification and orbit\n\nhas been characterized as a dwarf planet candidate. Based on assumptions and estimates, Michael Brown gives it a \"likely\"-status on his website, which is the third highest status after \"near certainty\" and \"highly likely\" (also see his classification table). T... |
(42301)_2001_UR163_3107910 | Describe the 'Diameter and albedo' section of the article about '(42301) 2001 UR163'. | measures approximately 352 km in diameter with a high albedo of 0.209. Based on previous estimates published on the Lightcurve Data Base and on Michael Brown's website, measures between 531 km and 583 km, using an assumed intermediate surface albedo of 0.09 to 0.10 with an absolute magnitude of 4.49 and 4.4, respectiv... | [
"(42301) 2001 UR163 β Classification and orbit\n\nhas been characterized as a dwarf planet candidate. Based on assumptions and estimates, Michael Brown gives it a \"likely\"-status on his website, which is the third highest status after \"near certainty\" and \"highly likely\" (also see his classification table). T... |
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