The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids
- Autores
- Beitz, E.; Blum, J.; Parisi, Mirta Gabriela; Trigo Rodriguez, J.
- Año de publicación
- 2016
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- 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 1014 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 Geofísicas
Instituto Argentino de Radioastronomía - Materia
-
Ciencias Astronómicas
asteroids: general
meteorites
meteoroids
meteors
methods: numerical
minor planets
planetary systems
planets and satellites: physical evolution - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/86489
Ver los metadatos del registro completo
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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:UNLP2025-09-29T11:16:45Zoai: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:13292025-09-29 11:16:45.513SEDICI (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 |
dc.description.none.fl_txt_mv |
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. Facultad de Ciencias Astronómicas y Geofísicas Instituto Argentino de Radioastronomía |
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) |
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