On the oldest asteroid families in the main belt
Autor(a) principal: | |
---|---|
Data de Publicação: | 2016 |
Outros Autores: | , , , |
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. |
id |
UNSP_b7c22757e73277fc90ebf29c42955a10 |
---|---|
oai_identifier_str |
oai:repositorio.unesp.br:11449/177998 |
network_acronym_str |
UNSP |
network_name_str |
Repositório Institucional da UNESP |
repository_id_str |
2946 |
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) |
instacron_str |
UNESP |
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) |
repository.mail.fl_str_mv |
|
_version_ |
1808128318295244800 |