On the age of the Beagle secundary asteroid family
Autor(a) principal: | |
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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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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 |
|
_version_ |
1808129441841283072 |