On the erigone family and the z2 secular resonance
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/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. |
id |
UNSP_786ae2f1764b48269ddf027445dc084b |
---|---|
oai_identifier_str |
oai:repositorio.unesp.br:11449/177838 |
network_acronym_str |
UNSP |
network_name_str |
Repositório Institucional da UNESP |
repository_id_str |
2946 |
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 |
|
_version_ |
1808129044514865152 |