On the age of the Beagle secundary asteroid family

Detalhes bibliográficos
Autor(a) principal: Carruba, V. [UNESP]
Data de Publicação: 2018
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UNESP
Texto Completo: http://dx.doi.org/10.1016/j.pss.2018.08.004
http://hdl.handle.net/11449/180168
Resumo: The Beagle family is a C-type subgroup of the Themis family, in the outer main belt. Previous works suggested that it could be younger than 20 Myr and a possible source for the dust in the i≃1.4∘ α zodiacal dust band. Here we took advantage of a much larger database for Beagle family members to revisit previous age estimates of this group. Standard dating techniques based on the family V-shape or on Monte Carlo methods of Yarkovsky and YORP mobility suggest that i) there might be a dichotomy for the inner and outer part of the Beagle family, which may be either two separate families or the product of an anisotropic ejection velocity field and that ii) the age of the possibly younger outer part of the Beagle family should be 35−35 +65 Myr. The past convergence of Beagle longitude of the node is compatible with a family age of ≃14 Myr, when (1678) Glarona is used as a reference orbit. Without further information on Beagle members spin states, however, only very lower limits on the family age can be currently obtained when the Yarkovksy force is accounted for.
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spelling On the age of the Beagle secundary asteroid familyAsteroids: generalAsteroids: individual: (656) BeagleCelestial mechanicsMinor planetsThe Beagle family is a C-type subgroup of the Themis family, in the outer main belt. Previous works suggested that it could be younger than 20 Myr and a possible source for the dust in the i≃1.4∘ α zodiacal dust band. Here we took advantage of a much larger database for Beagle family members to revisit previous age estimates of this group. Standard dating techniques based on the family V-shape or on Monte Carlo methods of Yarkovsky and YORP mobility suggest that i) there might be a dichotomy for the inner and outer part of the Beagle family, which may be either two separate families or the product of an anisotropic ejection velocity field and that ii) the age of the possibly younger outer part of the Beagle family should be 35−35 +65 Myr. The past convergence of Beagle longitude of the node is compatible with a family age of ≃14 Myr, when (1678) Glarona is used as a reference orbit. Without further information on Beagle members spin states, however, only very lower limits on the family age can be currently obtained when the Yarkovksy force is accounted for.California Institute of TechnologyConselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)São Paulo State University (UNESP) School of Natural Sciences and EngineeringSão Paulo State University (UNESP) School of Natural Sciences and EngineeringCNPq: 305453/2011-4Universidade Estadual Paulista (Unesp)Carruba, V. [UNESP]2018-12-11T17:38:27Z2018-12-11T17:38:27Z2018-01-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleapplication/pdfhttp://dx.doi.org/10.1016/j.pss.2018.08.004Planetary and Space Science.0032-0633http://hdl.handle.net/11449/18016810.1016/j.pss.2018.08.0042-s2.0-850530547782-s2.0-85053054778.pdfScopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengPlanetary and Space Science1,065info:eu-repo/semantics/openAccess2024-07-02T14:29:31Zoai:repositorio.unesp.br:11449/180168Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T22:35:49.610080Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false
dc.title.none.fl_str_mv On the age of the Beagle secundary asteroid family
title On the age of the Beagle secundary asteroid family
spellingShingle On the age of the Beagle secundary asteroid family
Carruba, V. [UNESP]
Asteroids: general
Asteroids: individual: (656) Beagle
Celestial mechanics
Minor planets
title_short On the age of the Beagle secundary asteroid family
title_full On the age of the Beagle secundary asteroid family
title_fullStr On the age of the Beagle secundary asteroid family
title_full_unstemmed On the age of the Beagle secundary asteroid family
title_sort On the age of the Beagle secundary asteroid family
author Carruba, V. [UNESP]
author_facet Carruba, V. [UNESP]
author_role author
dc.contributor.none.fl_str_mv Universidade Estadual Paulista (Unesp)
dc.contributor.author.fl_str_mv Carruba, V. [UNESP]
dc.subject.por.fl_str_mv Asteroids: general
Asteroids: individual: (656) Beagle
Celestial mechanics
Minor planets
topic Asteroids: general
Asteroids: individual: (656) Beagle
Celestial mechanics
Minor planets
description The Beagle family is a C-type subgroup of the Themis family, in the outer main belt. Previous works suggested that it could be younger than 20 Myr and a possible source for the dust in the i≃1.4∘ α zodiacal dust band. Here we took advantage of a much larger database for Beagle family members to revisit previous age estimates of this group. Standard dating techniques based on the family V-shape or on Monte Carlo methods of Yarkovsky and YORP mobility suggest that i) there might be a dichotomy for the inner and outer part of the Beagle family, which may be either two separate families or the product of an anisotropic ejection velocity field and that ii) the age of the possibly younger outer part of the Beagle family should be 35−35 +65 Myr. The past convergence of Beagle longitude of the node is compatible with a family age of ≃14 Myr, when (1678) Glarona is used as a reference orbit. Without further information on Beagle members spin states, however, only very lower limits on the family age can be currently obtained when the Yarkovksy force is accounted for.
publishDate 2018
dc.date.none.fl_str_mv 2018-12-11T17:38:27Z
2018-12-11T17:38:27Z
2018-01-01
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/10.1016/j.pss.2018.08.004
Planetary and Space Science.
0032-0633
http://hdl.handle.net/11449/180168
10.1016/j.pss.2018.08.004
2-s2.0-85053054778
2-s2.0-85053054778.pdf
url http://dx.doi.org/10.1016/j.pss.2018.08.004
http://hdl.handle.net/11449/180168
identifier_str_mv Planetary and Space Science.
0032-0633
10.1016/j.pss.2018.08.004
2-s2.0-85053054778
2-s2.0-85053054778.pdf
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv Planetary and Space Science
1,065
dc.rights.driver.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv 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
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