Collisional and dynamical evolution of the main belt and NEA population

Autores
de Elia, Gonzalo Carlos; Brunini, Adrian
Año de publicación
2007
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. In this paper, we analyze the collisional evolution of the Main Belt and NEA population taking into account the major dynamical features present in both populations. Methods. To do this, we divide the asteroid belt into three semimajor axis zones, whose boundaries are given by the V6, secular resonance, and the 3:1, 5:2 and 2:1 mean motion resonances with Jupiter, treating them as strong sources of dynamical removal. We also consider the action of the Yarkovsky effect and diffusive resonances as mechanisms of mass depletion. This treatment allows us to calculate the direct collisional injection into the powerful resonances, to study the collisional exchange of mass between the different regions of the Main Belt and to analyze the provenance of the NEA objects. Results. Our model is in agreement with the major observational constraints associated with the Main Belt and NEA populations, such as their size distributions, the collisional history of Vesta, the number of large asteroid families and the cosmic-ray exposure (CRE) ages of meteorites. We find that none of the dynamical and collisional mechanisms included in our treatment are able to mix material between the three studied main belt regions, since more than 99% of the final mass of every ring of our model of the Main Belt is represented by primordial material. In addition, our results supports that the Yarkovsky effect is the most important process that removes material from the asteroid Main Belt, rather than collisional injection into the major resonances. With regards to the provenance of the NEAs, our work shows that ∼94% of the NEA population comes from the region inside the 5:2 mean motion resonance. © ESO 2007.
Fil: de Elia, Gonzalo Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Brunini, Adrian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Materia
METHODS: N-BODY SIMULATIONS
METHODS: NUMERICAL
MINOR PLANETS, ASTEROIDS
SOLAR SYSTEM: FORMATION
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/54390
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/54390
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Collisional and dynamical evolution of the main belt and NEA populationde Elia, Gonzalo CarlosBrunini, AdrianMETHODS: N-BODY SIMULATIONSMETHODS: NUMERICALMINOR PLANETS, ASTEROIDSSOLAR SYSTEM: FORMATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. In this paper, we analyze the collisional evolution of the Main Belt and NEA population taking into account the major dynamical features present in both populations. Methods. To do this, we divide the asteroid belt into three semimajor axis zones, whose boundaries are given by the V6, secular resonance, and the 3:1, 5:2 and 2:1 mean motion resonances with Jupiter, treating them as strong sources of dynamical removal. We also consider the action of the Yarkovsky effect and diffusive resonances as mechanisms of mass depletion. This treatment allows us to calculate the direct collisional injection into the powerful resonances, to study the collisional exchange of mass between the different regions of the Main Belt and to analyze the provenance of the NEA objects. Results. Our model is in agreement with the major observational constraints associated with the Main Belt and NEA populations, such as their size distributions, the collisional history of Vesta, the number of large asteroid families and the cosmic-ray exposure (CRE) ages of meteorites. We find that none of the dynamical and collisional mechanisms included in our treatment are able to mix material between the three studied main belt regions, since more than 99% of the final mass of every ring of our model of the Main Belt is represented by primordial material. In addition, our results supports that the Yarkovsky effect is the most important process that removes material from the asteroid Main Belt, rather than collisional injection into the major resonances. With regards to the provenance of the NEAs, our work shows that ∼94% of the NEA population comes from the region inside the 5:2 mean motion resonance. © ESO 2007.Fil: de Elia, Gonzalo Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Brunini, Adrian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaEDP Sciences2007-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/54390de Elia, Gonzalo Carlos; Brunini, Adrian; Collisional and dynamical evolution of the main belt and NEA population; EDP Sciences; Astronomy and Astrophysics; 466; 3; 5-2007; 1159-11770004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066046info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/18/aa6046-06/aa6046-06.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:06:08Zoai:ri.conicet.gov.ar:11336/54390instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:06:08.75CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Collisional and dynamical evolution of the main belt and NEA population
title Collisional and dynamical evolution of the main belt and NEA population
spellingShingle Collisional and dynamical evolution of the main belt and NEA population
de Elia, Gonzalo Carlos
METHODS: N-BODY SIMULATIONS
METHODS: NUMERICAL
MINOR PLANETS, ASTEROIDS
SOLAR SYSTEM: FORMATION
title_short Collisional and dynamical evolution of the main belt and NEA population
title_full Collisional and dynamical evolution of the main belt and NEA population
title_fullStr Collisional and dynamical evolution of the main belt and NEA population
title_full_unstemmed Collisional and dynamical evolution of the main belt and NEA population
title_sort Collisional and dynamical evolution of the main belt and NEA population
dc.creator.none.fl_str_mv de Elia, Gonzalo Carlos
Brunini, Adrian
author de Elia, Gonzalo Carlos
author_facet de Elia, Gonzalo Carlos
Brunini, Adrian
author_role author
author2 Brunini, Adrian
author2_role author
dc.subject.none.fl_str_mv METHODS: N-BODY SIMULATIONS
METHODS: NUMERICAL
MINOR PLANETS, ASTEROIDS
SOLAR SYSTEM: FORMATION
topic METHODS: N-BODY SIMULATIONS
METHODS: NUMERICAL
MINOR PLANETS, ASTEROIDS
SOLAR SYSTEM: FORMATION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. In this paper, we analyze the collisional evolution of the Main Belt and NEA population taking into account the major dynamical features present in both populations. Methods. To do this, we divide the asteroid belt into three semimajor axis zones, whose boundaries are given by the V6, secular resonance, and the 3:1, 5:2 and 2:1 mean motion resonances with Jupiter, treating them as strong sources of dynamical removal. We also consider the action of the Yarkovsky effect and diffusive resonances as mechanisms of mass depletion. This treatment allows us to calculate the direct collisional injection into the powerful resonances, to study the collisional exchange of mass between the different regions of the Main Belt and to analyze the provenance of the NEA objects. Results. Our model is in agreement with the major observational constraints associated with the Main Belt and NEA populations, such as their size distributions, the collisional history of Vesta, the number of large asteroid families and the cosmic-ray exposure (CRE) ages of meteorites. We find that none of the dynamical and collisional mechanisms included in our treatment are able to mix material between the three studied main belt regions, since more than 99% of the final mass of every ring of our model of the Main Belt is represented by primordial material. In addition, our results supports that the Yarkovsky effect is the most important process that removes material from the asteroid Main Belt, rather than collisional injection into the major resonances. With regards to the provenance of the NEAs, our work shows that ∼94% of the NEA population comes from the region inside the 5:2 mean motion resonance. © ESO 2007.
Fil: de Elia, Gonzalo Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Brunini, Adrian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
description Aims. In this paper, we analyze the collisional evolution of the Main Belt and NEA population taking into account the major dynamical features present in both populations. Methods. To do this, we divide the asteroid belt into three semimajor axis zones, whose boundaries are given by the V6, secular resonance, and the 3:1, 5:2 and 2:1 mean motion resonances with Jupiter, treating them as strong sources of dynamical removal. We also consider the action of the Yarkovsky effect and diffusive resonances as mechanisms of mass depletion. This treatment allows us to calculate the direct collisional injection into the powerful resonances, to study the collisional exchange of mass between the different regions of the Main Belt and to analyze the provenance of the NEA objects. Results. Our model is in agreement with the major observational constraints associated with the Main Belt and NEA populations, such as their size distributions, the collisional history of Vesta, the number of large asteroid families and the cosmic-ray exposure (CRE) ages of meteorites. We find that none of the dynamical and collisional mechanisms included in our treatment are able to mix material between the three studied main belt regions, since more than 99% of the final mass of every ring of our model of the Main Belt is represented by primordial material. In addition, our results supports that the Yarkovsky effect is the most important process that removes material from the asteroid Main Belt, rather than collisional injection into the major resonances. With regards to the provenance of the NEAs, our work shows that ∼94% of the NEA population comes from the region inside the 5:2 mean motion resonance. © ESO 2007.
publishDate 2007
dc.date.none.fl_str_mv 2007-05
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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://hdl.handle.net/11336/54390
de Elia, Gonzalo Carlos; Brunini, Adrian; Collisional and dynamical evolution of the main belt and NEA population; EDP Sciences; Astronomy and Astrophysics; 466; 3; 5-2007; 1159-1177
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/54390
identifier_str_mv de Elia, Gonzalo Carlos; Brunini, Adrian; Collisional and dynamical evolution of the main belt and NEA population; EDP Sciences; Astronomy and Astrophysics; 466; 3; 5-2007; 1159-1177
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066046
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/18/aa6046-06/aa6046-06.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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