The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids

Most meteorites are fragments from recent collisions experienced in the asteroid belt. In such a hypervelocity collision, the smaller collision partner is destroyed, whereas a crater on the asteroid is formed or it is entirely disrupted, too. The present size distribution of the asteroid belt sugges...

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Detalles Bibliográficos
Autores: Beitz, E., Blum, J., Parisi, Mirta Gabriela, Trigo Rodriguez, J.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2016
País:Argentina
Institución:Universidad Nacional de La Plata
Repositorio:SEDICI (UNLP)
Idioma:inglés
OAI Identifier:oai:sedici.unlp.edu.ar:10915/86489
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/86489
Access Level:acceso abierto
Palabra clave:Ciencias Astronómicas
asteroids: general
meteorites
meteoroids
meteors
methods: numerical
minor planets
planetary systems
planets and satellites: physical evolution
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spelling The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroidsBeitz, E.Blum, J.Parisi, Mirta GabrielaTrigo Rodriguez, J.Ciencias Astronómicasasteroids: generalmeteoritesmeteoroidsmeteorsmethods: numericalminor planetsplanetary systemsplanets and satellites: physical evolutionMost meteorites are fragments from recent collisions experienced in the asteroid belt. In such a hypervelocity collision, the smaller collision partner is destroyed, whereas a crater on the asteroid is formed or it is entirely disrupted, too. The present size distribution of the asteroid belt suggests that an asteroid with a 100 km radius is encountered 10<SUP>14</SUP> times during the lifetime of the solar system by objects larger than 10 cm in radius; the formed craters cover the surface of the asteroid about 100 times. We present a Monte Carlo code that takes into account the statistical bombardment of individual infinitesimally small surface elements, the subsequent compaction of the underlying material, and the formation of a crater and a regolith layer. For the entire asteroid, 10,000 individual surface elements are calculated. We compare the ejected material from the calculated craters with the shock stage of meteorites with low petrologic type and find that these most likely stem from smaller parent bodies that do not possess a significant regolith layer. For larger objects, which accrete a regolith layer, a prediction of the thickness depending on the largest visible crater can be made. Additionally, we compare the crater distribution of an object initially 100 km in radius with the shape model of the asteroid (21) Lutetia, assuming it to be initially formed spherical with a radius that is equal to its longest present ellipsoid length. Here we find the shapes of both objects to show resemblance to each other.Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de Radioastronomía2016info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/86489enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/824/1/12info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2024-05-08T12:54:42Zoai:sedici.unlp.edu.ar:10915/86489Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292024-05-08 12:54:43.146SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
title The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
spellingShingle The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
Beitz, E.
Ciencias Astronómicas
asteroids: general
meteorites
meteoroids
meteors
methods: numerical
minor planets
planetary systems
planets and satellites: physical evolution
title_short The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
title_full The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
title_fullStr The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
title_full_unstemmed The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
title_sort The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
dc.creator.none.fl_str_mv Beitz, E.
Blum, J.
Parisi, Mirta Gabriela
Trigo Rodriguez, J.
author Beitz, E.
author_facet Beitz, E.
Blum, J.
Parisi, Mirta Gabriela
Trigo Rodriguez, J.
author_role author
author2 Blum, J.
Parisi, Mirta Gabriela
Trigo Rodriguez, J.
author2_role author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
asteroids: general
meteorites
meteoroids
meteors
methods: numerical
minor planets
planetary systems
planets and satellites: physical evolution
topic Ciencias Astronómicas
asteroids: general
meteorites
meteoroids
meteors
methods: numerical
minor planets
planetary systems
planets and satellites: physical evolution
description Most meteorites are fragments from recent collisions experienced in the asteroid belt. In such a hypervelocity collision, the smaller collision partner is destroyed, whereas a crater on the asteroid is formed or it is entirely disrupted, too. The present size distribution of the asteroid belt suggests that an asteroid with a 100 km radius is encountered 10<SUP>14</SUP> times during the lifetime of the solar system by objects larger than 10 cm in radius; the formed craters cover the surface of the asteroid about 100 times. We present a Monte Carlo code that takes into account the statistical bombardment of individual infinitesimally small surface elements, the subsequent compaction of the underlying material, and the formation of a crater and a regolith layer. For the entire asteroid, 10,000 individual surface elements are calculated. We compare the ejected material from the calculated craters with the shock stage of meteorites with low petrologic type and find that these most likely stem from smaller parent bodies that do not possess a significant regolith layer. For larger objects, which accrete a regolith layer, a prediction of the thickness depending on the largest visible crater can be made. Additionally, we compare the crater distribution of an object initially 100 km in radius with the shape model of the asteroid (21) Lutetia, assuming it to be initially formed spherical with a radius that is equal to its longest present ellipsoid length. Here we find the shapes of both objects to show resemblance to each other.
publishDate 2016
dc.date.none.fl_str_mv 2016
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/86489
url http://sedici.unlp.edu.ar/handle/10915/86489
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-637X
info:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/824/1/12
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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