The mass ratio of the two components – called the "primary" and "secondary" of a binary system – is an important characteristic. Most binary asteroids have a large mass ratio, i.e. a relatively small satellite in orbit around the main component. Systems with a small minor-planet moon – also called "companion" or simply "satellite" – include 87 Sylvia, 107 Camilla, 45 Eugenia, 121 Hermione, 130 Elektra, 22 Kalliope, 283 Emma, 379 Huenna, 243 Ida and 4337 Arecibo (in order of decreasing primary size). Some binary systems have a mass ratio near unity, i.e., two components of similar mass. They include 90 Antiope, 2006 VW139, 2017 YE5 and 69230 Hermes, with average component diameters of 86, 1.8, 0.9 and 0.8 km, respectively.
Several theories have been posited to explain the formation of binary-asteroid systems. Many systems have significant macro-porosity (a "rubble-pile" interior). The satellites orbiting large main-belt asteroids such as 22 Kalliope, 45 Eugenia or 87 Sylvia may have formed by disruption of a parent body after impact or fission after an oblique impact. Trans-Neptunian binaries may have formed during the formation of the Solar System by mutual capture or three-body interaction. Near-Earth asteroids, which orbit in the inner part of the Solar System, most likely form by spin-up and mass shedding,[2] likely as a result of the YORP effect. Numerical simulations suggest that when solar energy spins a “rubble pile” asteroid to a sufficiently fast rate by the YORP effect, material is thrown from the asteroid's equator.[3] This process also exposes fresh material at the poles of the asteroid.[3][4]
Galleryedit
Time-lapse video of binary main-belt comet 2006 VW139 (288P)[5]
Artist's impression of the double asteroid 90 Antiope
Wikimedia Commons has media related to Binary asteroids.
^Margot, Jean-Luc; Pravec, Petr; Taylor, Patrick; Carry, Benoît; Jacobson, Seth (2015). "Asteroid Systems: Binaries, Triples, and Pairs". In Michel, Patrick; DeMeo, Francesca E.; Bottke, William F. (eds.). Asteroids IV. p. 355. arXiv:1504.00034. Bibcode:2015aste.book..355M. doi:10.2458/azu_uapress_9780816532131-ch019. ISBN9780816532131. S2CID 56278100.
^Margot, Jean-Luc; et al. (2002). "Binary Asteroids in the Near-Earth Object Population". Science. 296 (5572): 1445–1448. Bibcode:2002Sci...296.1445M. doi:10.1126/science.1072094. PMID 11951001. S2CID 8768432.
^ abWalsh, Kevin J.; Richardson, DC; Michel, P (June 2008). "Rotational breakup as the origin of small binary asteroids". Nature. 454 (7201): 188–191. Bibcode:2008Natur.454..188W. doi:10.1038/nature07078. PMID 18615078. S2CID 4418744.
^Study Puts Solar Spin on Asteroids, their Moons & Earth Impacts Newswise, Retrieved 14 July 2008.
^"Hubble discovers a unique type of object in the Solar System". www.spacetelescope.org. Retrieved 21 September 2017.
January 01, 1970
binary, asteroid, also, minor, planet, moon, binary, asteroid, system, asteroids, orbiting, their, common, barycenter, binary, nature, discovered, when, galileo, spacecraft, flew, asteroid, 1993, since, then, numerous, binary, asteroids, several, triple, aster. See also Minor planet moon A binary asteroid is a system of two asteroids orbiting their common barycenter The binary nature of 243 Ida was discovered when the Galileo spacecraft flew by the asteroid in 1993 Since then numerous binary asteroids and several triple asteroids have been detected 1 Binary asteroid 243 Ida with its small minor planet moon Dactyl as seen by Galileo Binary near Earth asteroid 65803 Didymos and its moon Dimorphos imaged by the Double Asteroid Redirection Test spacecraft The mass ratio of the two components called the primary and secondary of a binary system is an important characteristic Most binary asteroids have a large mass ratio i e a relatively small satellite in orbit around the main component Systems with a small minor planet moon also called companion or simply satellite include 87 Sylvia 107 Camilla 45 Eugenia 121 Hermione 130 Elektra 22 Kalliope 283 Emma 379 Huenna 243 Ida and 4337 Arecibo in order of decreasing primary size Some binary systems have a mass ratio near unity i e two components of similar mass They include 90 Antiope 2006 VW139 2017 YE5 and 69230 Hermes with average component diameters of 86 1 8 0 9 and 0 8 km respectively Contents 1 Description 2 Gallery 3 See also 4 ReferencesDescription editSeveral theories have been posited to explain the formation of binary asteroid systems Many systems have significant macro porosity a rubble pile interior The satellites orbiting large main belt asteroids such as 22 Kalliope 45 Eugenia or 87 Sylvia may have formed by disruption of a parent body after impact or fission after an oblique impact Trans Neptunian binaries may have formed during the formation of the Solar System by mutual capture or three body interaction Near Earth asteroids which orbit in the inner part of the Solar System most likely form by spin up and mass shedding 2 likely as a result of the YORP effect Numerical simulations suggest that when solar energy spins a rubble pile asteroid to a sufficiently fast rate by the YORP effect material is thrown from the asteroid s equator 3 This process also exposes fresh material at the poles of the asteroid 3 4 Gallery edit nbsp Time lapse video of binary main belt comet 2006 VW139 288P 5 nbsp Artist s impression of the double asteroid 90 AntiopeSee also editMinor planet moon List of minor planets with moons Subsatellite also known as Moonmoon A satellite that orbits a natural satellite Contact binary small Solar System body Triple asteroids 153591 2001 SN263 and 136617 1994 CCReferences edit nbsp Wikimedia Commons has media related to Binary asteroids Margot Jean Luc Pravec Petr Taylor Patrick Carry Benoit Jacobson Seth 2015 Asteroid Systems Binaries Triples and Pairs In Michel Patrick DeMeo Francesca E Bottke William F eds Asteroids IV p 355 arXiv 1504 00034 Bibcode 2015aste book 355M doi 10 2458 azu uapress 9780816532131 ch019 ISBN 9780816532131 S2CID 56278100 Margot Jean Luc et al 2002 Binary Asteroids in the Near Earth Object Population Science 296 5572 1445 1448 Bibcode 2002Sci 296 1445M doi 10 1126 science 1072094 PMID 11951001 S2CID 8768432 a b Walsh Kevin J Richardson DC Michel P June 2008 Rotational breakup as the origin of small binary asteroids Nature 454 7201 188 191 Bibcode 2008Natur 454 188W doi 10 1038 nature07078 PMID 18615078 S2CID 4418744 Study Puts Solar Spin on Asteroids their Moons amp Earth Impacts Newswise Retrieved 14 July 2008 Hubble discovers a unique type of object in the Solar System www spacetelescope org Retrieved 21 September 2017 Retrieved from https en wikipedia org w index php title Binary asteroid amp oldid 1136459091, wikipedia, wiki, book, books, library,
