On the erigone family and the z2 secular resonance

Detalhes bibliográficos
Autor(a) principal: Carruba, V. [UNESP]
Data de Publicação: 2016
Outros Autores: Aljbaae, S. [UNESP], Winter, O. C. [UNESP]
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UNESP
Texto Completo: http://dx.doi.org/10.1093/mnras/stv2430
http://hdl.handle.net/11449/177838
Resumo: The Erigone family is a C-type group in the inner main belt. Its age has been estimated by several researchers to be less then 300 Myr, so it is a relatively young cluster. Yarko-YORP Monte Carlo methods to study the chronology of the Erigone family confirm results obtained by other groups. The Erigone family, however, is also characterized by its interaction with the z2 secular resonance. While less than 15 per cent of its members are currently in librating states of this resonance, the number of objects, members of the dynamical group, in resonant states is high enough to allow us to use the study of dynamics inside the z2 resonance to set constraints on the family age. Like the ν6 and z1 secular resonances, the z2 resonance is characterized by one stable equilibrium point at σ = 180° in the z2 resonance plane (σ, dσ/dt), where σ is the resonant angle of the z2 resonance. Diffusion in this plane occurs on time-scales of ≃ 12 Myr, which sets a lower limit on the Erigone family age. Finally, the minimum time needed to reach a steady-state population of z2 librators is about 90 Myr, which allows us to impose another, independent constraint on the group age.
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spelling On the erigone family and the z2 secular resonanceCelestialmechanicsMinor planets, asteroids: generalMinor planets, asteroids: individual: ErigoneThe Erigone family is a C-type group in the inner main belt. Its age has been estimated by several researchers to be less then 300 Myr, so it is a relatively young cluster. Yarko-YORP Monte Carlo methods to study the chronology of the Erigone family confirm results obtained by other groups. The Erigone family, however, is also characterized by its interaction with the z2 secular resonance. While less than 15 per cent of its members are currently in librating states of this resonance, the number of objects, members of the dynamical group, in resonant states is high enough to allow us to use the study of dynamics inside the z2 resonance to set constraints on the family age. Like the ν6 and z1 secular resonances, the z2 resonance is characterized by one stable equilibrium point at σ = 180° in the z2 resonance plane (σ, dσ/dt), where σ is the resonant angle of the z2 resonance. Diffusion in this plane occurs on time-scales of ≃ 12 Myr, which sets a lower limit on the Erigone family age. Finally, the minimum time needed to reach a steady-state population of z2 librators is about 90 Myr, which allows us to impose another, independent constraint on the group age.Grupo de dinâmica Orbital e Planetologia UNESP Univ. Estadual PaulistaDepartment of Space Studies Southwest Research InstituteGrupo de dinâmica Orbital e Planetologia UNESP Univ. Estadual PaulistaUniversidade Estadual Paulista (Unesp)Southwest Research InstituteCarruba, V. [UNESP]Aljbaae, S. [UNESP]Winter, O. C. [UNESP]2018-12-11T17:27:22Z2018-12-11T17:27:22Z2016-01-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article2279-2288application/pdfhttp://dx.doi.org/10.1093/mnras/stv2430Monthly Notices of the Royal Astronomical Society, v. 455, n. 3, p. 2279-2288, 2016.1365-29660035-8711http://hdl.handle.net/11449/17783810.1093/mnras/stv24302-s2.0-849591273132-s2.0-84959127313.pdfScopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Society2,3462,346info:eu-repo/semantics/openAccess2024-07-02T14:29:20Zoai:repositorio.unesp.br:11449/177838Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T19:16:32.103714Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false
dc.title.none.fl_str_mv On the erigone family and the z2 secular resonance
title On the erigone family and the z2 secular resonance
spellingShingle On the erigone family and the z2 secular resonance
Carruba, V. [UNESP]
Celestialmechanics
Minor planets, asteroids: general
Minor planets, asteroids: individual: Erigone
title_short On the erigone family and the z2 secular resonance
title_full On the erigone family and the z2 secular resonance
title_fullStr On the erigone family and the z2 secular resonance
title_full_unstemmed On the erigone family and the z2 secular resonance
title_sort On the erigone family and the z2 secular resonance
author Carruba, V. [UNESP]
author_facet Carruba, V. [UNESP]
Aljbaae, S. [UNESP]
Winter, O. C. [UNESP]
author_role author
author2 Aljbaae, S. [UNESP]
Winter, O. C. [UNESP]
author2_role author
author
dc.contributor.none.fl_str_mv Universidade Estadual Paulista (Unesp)
Southwest Research Institute
dc.contributor.author.fl_str_mv Carruba, V. [UNESP]
Aljbaae, S. [UNESP]
Winter, O. C. [UNESP]
dc.subject.por.fl_str_mv Celestialmechanics
Minor planets, asteroids: general
Minor planets, asteroids: individual: Erigone
topic Celestialmechanics
Minor planets, asteroids: general
Minor planets, asteroids: individual: Erigone
description The Erigone family is a C-type group in the inner main belt. Its age has been estimated by several researchers to be less then 300 Myr, so it is a relatively young cluster. Yarko-YORP Monte Carlo methods to study the chronology of the Erigone family confirm results obtained by other groups. The Erigone family, however, is also characterized by its interaction with the z2 secular resonance. While less than 15 per cent of its members are currently in librating states of this resonance, the number of objects, members of the dynamical group, in resonant states is high enough to allow us to use the study of dynamics inside the z2 resonance to set constraints on the family age. Like the ν6 and z1 secular resonances, the z2 resonance is characterized by one stable equilibrium point at σ = 180° in the z2 resonance plane (σ, dσ/dt), where σ is the resonant angle of the z2 resonance. Diffusion in this plane occurs on time-scales of ≃ 12 Myr, which sets a lower limit on the Erigone family age. Finally, the minimum time needed to reach a steady-state population of z2 librators is about 90 Myr, which allows us to impose another, independent constraint on the group age.
publishDate 2016
dc.date.none.fl_str_mv 2016-01-01
2018-12-11T17:27:22Z
2018-12-11T17:27:22Z
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/stv2430
Monthly Notices of the Royal Astronomical Society, v. 455, n. 3, p. 2279-2288, 2016.
1365-2966
0035-8711
http://hdl.handle.net/11449/177838
10.1093/mnras/stv2430
2-s2.0-84959127313
2-s2.0-84959127313.pdf
url http://dx.doi.org/10.1093/mnras/stv2430
http://hdl.handle.net/11449/177838
identifier_str_mv Monthly Notices of the Royal Astronomical Society, v. 455, n. 3, p. 2279-2288, 2016.
1365-2966
0035-8711
10.1093/mnras/stv2430
2-s2.0-84959127313
2-s2.0-84959127313.pdf
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 2279-2288
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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