The Zelima asteroid family: Resonant configuration and rotational fission clusters

Detalhes bibliográficos
Autor(a) principal: Carruba, V. [UNESP]
Data de Publicação: 2020
Outros Autores: Ribeiro, J. V. [UNESP]
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UNESP
Texto Completo: http://dx.doi.org/10.1016/j.pss.2019.104810
http://hdl.handle.net/11449/201401
Resumo: Asteroid families are groups of asteroids that are identifiable in domains of proper elements. They may be the outcome of a collision, or the product of rotational fission. Among collisional families, young asteroid families are of interest because they preserve information on the original ejection velocity field with which the asteroid fragments were expelled, and because they may host a significant population of clusters produced by rotational fission among their members. The recently identified Zelima asteroid family is unique because, apart from its very young age of less than 3 Myr, is also interacting with the z1 secular resonance, making it the third asteroid family in this peculiar configuration, after the Agnia and Padua families, and the only one for which all members are in z1 librating states. Because of its extremely young age, the orbits of its members are still very clustered in the domain (σ,dσ/dt), with σ=ϖ−ϖ6+Ω−Ω6 the resonant argument of the z1 resonance. This allow for precisely dating the family with a method not available for any other main belt group. The Zelima family, based on this argument, should be 2.5±1.5 Myr old, and conserved quantities of the z1 secular resonance show that its ejection velocity field is in a range of 1.1−0.2 +0.6 of the escape velocity from the parent body, in agreement with general results for cratering collisional families. Finally, 41.7% of the members of the Zelima family are also members of possible fission clusters, confirming the trend observed for other very young families, like the Jones and Lorre groups.
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spelling The Zelima asteroid family: Resonant configuration and rotational fission clustersAsteroids: generalAsteroids: individual: (633) ZelimaCelestial mechanicsMinor planetsAsteroid families are groups of asteroids that are identifiable in domains of proper elements. They may be the outcome of a collision, or the product of rotational fission. Among collisional families, young asteroid families are of interest because they preserve information on the original ejection velocity field with which the asteroid fragments were expelled, and because they may host a significant population of clusters produced by rotational fission among their members. The recently identified Zelima asteroid family is unique because, apart from its very young age of less than 3 Myr, is also interacting with the z1 secular resonance, making it the third asteroid family in this peculiar configuration, after the Agnia and Padua families, and the only one for which all members are in z1 librating states. Because of its extremely young age, the orbits of its members are still very clustered in the domain (σ,dσ/dt), with σ=ϖ−ϖ6+Ω−Ω6 the resonant argument of the z1 resonance. This allow for precisely dating the family with a method not available for any other main belt group. The Zelima family, based on this argument, should be 2.5±1.5 Myr old, and conserved quantities of the z1 secular resonance show that its ejection velocity field is in a range of 1.1−0.2 +0.6 of the escape velocity from the parent body, in agreement with general results for cratering collisional families. Finally, 41.7% of the members of the Zelima family are also members of possible fission clusters, confirming the trend observed for other very young families, like the Jones and Lorre groups.Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)Conselho 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 EngineeringFAPESP: 18/20999-6CNPq: 301577/2017-0Universidade Estadual Paulista (Unesp)Carruba, V. [UNESP]Ribeiro, J. V. [UNESP]2020-12-12T02:31:34Z2020-12-12T02:31:34Z2020-03-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://dx.doi.org/10.1016/j.pss.2019.104810Planetary and Space Science, v. 182.0032-0633http://hdl.handle.net/11449/20140110.1016/j.pss.2019.1048102-s2.0-85076595539Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengPlanetary and Space Scienceinfo:eu-repo/semantics/openAccess2024-07-02T14:29:31Zoai:repositorio.unesp.br:11449/201401Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T22:02:42.634184Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false
dc.title.none.fl_str_mv The Zelima asteroid family: Resonant configuration and rotational fission clusters
title The Zelima asteroid family: Resonant configuration and rotational fission clusters
spellingShingle The Zelima asteroid family: Resonant configuration and rotational fission clusters
Carruba, V. [UNESP]
Asteroids: general
Asteroids: individual: (633) Zelima
Celestial mechanics
Minor planets
title_short The Zelima asteroid family: Resonant configuration and rotational fission clusters
title_full The Zelima asteroid family: Resonant configuration and rotational fission clusters
title_fullStr The Zelima asteroid family: Resonant configuration and rotational fission clusters
title_full_unstemmed The Zelima asteroid family: Resonant configuration and rotational fission clusters
title_sort The Zelima asteroid family: Resonant configuration and rotational fission clusters
author Carruba, V. [UNESP]
author_facet Carruba, V. [UNESP]
Ribeiro, J. V. [UNESP]
author_role author
author2 Ribeiro, J. V. [UNESP]
author2_role author
dc.contributor.none.fl_str_mv Universidade Estadual Paulista (Unesp)
dc.contributor.author.fl_str_mv Carruba, V. [UNESP]
Ribeiro, J. V. [UNESP]
dc.subject.por.fl_str_mv Asteroids: general
Asteroids: individual: (633) Zelima
Celestial mechanics
Minor planets
topic Asteroids: general
Asteroids: individual: (633) Zelima
Celestial mechanics
Minor planets
description Asteroid families are groups of asteroids that are identifiable in domains of proper elements. They may be the outcome of a collision, or the product of rotational fission. Among collisional families, young asteroid families are of interest because they preserve information on the original ejection velocity field with which the asteroid fragments were expelled, and because they may host a significant population of clusters produced by rotational fission among their members. The recently identified Zelima asteroid family is unique because, apart from its very young age of less than 3 Myr, is also interacting with the z1 secular resonance, making it the third asteroid family in this peculiar configuration, after the Agnia and Padua families, and the only one for which all members are in z1 librating states. Because of its extremely young age, the orbits of its members are still very clustered in the domain (σ,dσ/dt), with σ=ϖ−ϖ6+Ω−Ω6 the resonant argument of the z1 resonance. This allow for precisely dating the family with a method not available for any other main belt group. The Zelima family, based on this argument, should be 2.5±1.5 Myr old, and conserved quantities of the z1 secular resonance show that its ejection velocity field is in a range of 1.1−0.2 +0.6 of the escape velocity from the parent body, in agreement with general results for cratering collisional families. Finally, 41.7% of the members of the Zelima family are also members of possible fission clusters, confirming the trend observed for other very young families, like the Jones and Lorre groups.
publishDate 2020
dc.date.none.fl_str_mv 2020-12-12T02:31:34Z
2020-12-12T02:31:34Z
2020-03-01
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.2019.104810
Planetary and Space Science, v. 182.
0032-0633
http://hdl.handle.net/11449/201401
10.1016/j.pss.2019.104810
2-s2.0-85076595539
url http://dx.doi.org/10.1016/j.pss.2019.104810
http://hdl.handle.net/11449/201401
identifier_str_mv Planetary and Space Science, v. 182.
0032-0633
10.1016/j.pss.2019.104810
2-s2.0-85076595539
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv Planetary and Space Science
dc.rights.driver.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
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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