On the oldest asteroid families in the main belt

Detalhes bibliográficos
Autor(a) principal: Carruba, V. [UNESP]
Data de Publicação: 2016
Outros Autores: Nesvorný, D., Aljbaae, S. [UNESP], Domingos, R. C. [UNESP], Huaman, M. [UNESP]
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UNESP
Texto Completo: http://dx.doi.org/10.1093/mnras/stw533
http://hdl.handle.net/11449/177998
Resumo: Asteroid families are groups of minor bodies produced by high-velocity collisions. After the initial dispersions of the parent bodies fragments, their orbits evolve because of several gravitational and non-gravitational effects, such as diffusion in mean-motion resonances, Yarkovsky and Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effects, close encounters of collisions, etc. The subsequent dynamical evolution of asteroid family members may cause some of the original fragments to travel beyond the conventional limits of the asteroid family. Eventually, the whole family will dynamically disperse and no longer be recognizable. A natural question that may arise concerns the time-scales for dispersion of large families. In particular, what is the oldest still recognizable family in the main belt? Are there any families that may date from the late stages of the late heavy bombardment and that could provide clues on our understanding of the primitive Solar system? In this work, we investigate the dynamical stability of seven of the allegedly oldest families in the asteroid main belt. Our results show that none of the seven studied families has a nominally mean estimated age older than 2.7 Gyr, assuming standard values for the parameters describing the strength of the Yarkovsky force. Most-paleo-families' that formed between 2.7 and 3.8 Gyr would be characterized by a very shallow size-frequency distribution, and could be recognizable only if located in a dynamically less active region (such as that of the Koronis family). V-type asteroids in the central main belt could be compatible with a formation from a paleo-Eunomia family.
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spelling On the oldest asteroid families in the main beltCelestial mechanicsMinor planets, asteroids: GeneralAsteroid families are groups of minor bodies produced by high-velocity collisions. After the initial dispersions of the parent bodies fragments, their orbits evolve because of several gravitational and non-gravitational effects, such as diffusion in mean-motion resonances, Yarkovsky and Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effects, close encounters of collisions, etc. The subsequent dynamical evolution of asteroid family members may cause some of the original fragments to travel beyond the conventional limits of the asteroid family. Eventually, the whole family will dynamically disperse and no longer be recognizable. A natural question that may arise concerns the time-scales for dispersion of large families. In particular, what is the oldest still recognizable family in the main belt? Are there any families that may date from the late stages of the late heavy bombardment and that could provide clues on our understanding of the primitive Solar system? In this work, we investigate the dynamical stability of seven of the allegedly oldest families in the asteroid main belt. Our results show that none of the seven studied families has a nominally mean estimated age older than 2.7 Gyr, assuming standard values for the parameters describing the strength of the Yarkovsky force. Most-paleo-families' that formed between 2.7 and 3.8 Gyr would be characterized by a very shallow size-frequency distribution, and could be recognizable only if located in a dynamically less active region (such as that of the Koronis family). V-type asteroids in the central main belt could be compatible with a formation from a paleo-Eunomia family.UNESP - Univ. Estadual Paulista Grupo de dinâmica Orbital e PlanetologiaDepartment of Space Studies Southwest Research InstituteUNESP - Univ. Estadual PaulistaUNESP - Univ. Estadual Paulista Grupo de dinâmica Orbital e PlanetologiaUNESP - Univ. Estadual PaulistaUniversidade Estadual Paulista (Unesp)Southwest Research InstituteCarruba, V. [UNESP]Nesvorný, D.Aljbaae, S. [UNESP]Domingos, R. C. [UNESP]Huaman, M. [UNESP]2018-12-11T17:28:06Z2018-12-11T17:28:06Z2016-03-17info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article3731-3738application/pdfhttp://dx.doi.org/10.1093/mnras/stw533Monthly Notices of the Royal Astronomical Society, v. 458, n. 4, p. 3731-3738, 2016.1365-29660035-8711http://hdl.handle.net/11449/17799810.1093/mnras/stw5332-s2.0-849650761812-s2.0-84965076181.pdf66521690834643270000-0002-0516-0420Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Society2,3462,346info:eu-repo/semantics/openAccess2024-07-02T14:28:50Zoai:repositorio.unesp.br:11449/177998Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T14:07:21.253856Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false
dc.title.none.fl_str_mv On the oldest asteroid families in the main belt
title On the oldest asteroid families in the main belt
spellingShingle On the oldest asteroid families in the main belt
Carruba, V. [UNESP]
Celestial mechanics
Minor planets, asteroids: General
title_short On the oldest asteroid families in the main belt
title_full On the oldest asteroid families in the main belt
title_fullStr On the oldest asteroid families in the main belt
title_full_unstemmed On the oldest asteroid families in the main belt
title_sort On the oldest asteroid families in the main belt
author Carruba, V. [UNESP]
author_facet Carruba, V. [UNESP]
Nesvorný, D.
Aljbaae, S. [UNESP]
Domingos, R. C. [UNESP]
Huaman, M. [UNESP]
author_role author
author2 Nesvorný, D.
Aljbaae, S. [UNESP]
Domingos, R. C. [UNESP]
Huaman, M. [UNESP]
author2_role author
author
author
author
dc.contributor.none.fl_str_mv Universidade Estadual Paulista (Unesp)
Southwest Research Institute
dc.contributor.author.fl_str_mv Carruba, V. [UNESP]
Nesvorný, D.
Aljbaae, S. [UNESP]
Domingos, R. C. [UNESP]
Huaman, M. [UNESP]
dc.subject.por.fl_str_mv Celestial mechanics
Minor planets, asteroids: General
topic Celestial mechanics
Minor planets, asteroids: General
description Asteroid families are groups of minor bodies produced by high-velocity collisions. After the initial dispersions of the parent bodies fragments, their orbits evolve because of several gravitational and non-gravitational effects, such as diffusion in mean-motion resonances, Yarkovsky and Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effects, close encounters of collisions, etc. The subsequent dynamical evolution of asteroid family members may cause some of the original fragments to travel beyond the conventional limits of the asteroid family. Eventually, the whole family will dynamically disperse and no longer be recognizable. A natural question that may arise concerns the time-scales for dispersion of large families. In particular, what is the oldest still recognizable family in the main belt? Are there any families that may date from the late stages of the late heavy bombardment and that could provide clues on our understanding of the primitive Solar system? In this work, we investigate the dynamical stability of seven of the allegedly oldest families in the asteroid main belt. Our results show that none of the seven studied families has a nominally mean estimated age older than 2.7 Gyr, assuming standard values for the parameters describing the strength of the Yarkovsky force. Most-paleo-families' that formed between 2.7 and 3.8 Gyr would be characterized by a very shallow size-frequency distribution, and could be recognizable only if located in a dynamically less active region (such as that of the Koronis family). V-type asteroids in the central main belt could be compatible with a formation from a paleo-Eunomia family.
publishDate 2016
dc.date.none.fl_str_mv 2016-03-17
2018-12-11T17:28:06Z
2018-12-11T17:28:06Z
dc.type.status.fl_str_mv info:eu-repo/semantics/publishedVersion
dc.type.driver.fl_str_mv info:eu-repo/semantics/article
format article
status_str publishedVersion
dc.identifier.uri.fl_str_mv http://dx.doi.org/10.1093/mnras/stw533
Monthly Notices of the Royal Astronomical Society, v. 458, n. 4, p. 3731-3738, 2016.
1365-2966
0035-8711
http://hdl.handle.net/11449/177998
10.1093/mnras/stw533
2-s2.0-84965076181
2-s2.0-84965076181.pdf
6652169083464327
0000-0002-0516-0420
url http://dx.doi.org/10.1093/mnras/stw533
http://hdl.handle.net/11449/177998
identifier_str_mv Monthly Notices of the Royal Astronomical Society, v. 458, n. 4, p. 3731-3738, 2016.
1365-2966
0035-8711
10.1093/mnras/stw533
2-s2.0-84965076181
2-s2.0-84965076181.pdf
6652169083464327
0000-0002-0516-0420
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv Monthly Notices of the Royal Astronomical Society
2,346
2,346
dc.rights.driver.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv 3731-3738
application/pdf
dc.source.none.fl_str_mv Scopus
reponame:Repositório Institucional da UNESP
instname:Universidade Estadual Paulista (UNESP)
instacron:UNESP
instname_str Universidade Estadual Paulista (UNESP)
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institution UNESP
reponame_str Repositório Institucional da UNESP
collection Repositório Institucional da UNESP
repository.name.fl_str_mv Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)
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