Orbital evolution of planet around a binary star
Autor(a) principal: | |
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Data de Publicação: | 2015 |
Outros Autores: | , , , |
Tipo de documento: | Artigo de conferência |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://hdl.handle.net/11449/178024 |
Resumo: | We study the secular dynamics of hierarchical (if there is a clearly defined binary and a third body which stays separate from the binary) triple systems composed by a Sun-like central star and a Jupiter-like planet, which are under the gravitational influence of a further perturbing star (brown dwarf). The main goal is to study the orbital evolution of the planet. In special, we investigate the orientation (inclination) and the shape (eccentricity) of its orbit. One key feature explored is the time needed for the first flip in its orientation (prograde to retrograde). The gravitational potential is developed in closed form up to the third order. We have compared the secular evolution of systems with and without the third order term of the disturbing potential. The R2 (quadrupole) and R3 (octupole) terms of the disturbing potential are developed without using the elimination of nodes. Numerical simulations were also performed to compare with the analytical model using the N-body simulations with the Mercury code. The results show that the analytical model are in agreement with the numeric simulations. |
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Repositório Institucional da UNESP |
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spelling |
Orbital evolution of planet around a binary starWe study the secular dynamics of hierarchical (if there is a clearly defined binary and a third body which stays separate from the binary) triple systems composed by a Sun-like central star and a Jupiter-like planet, which are under the gravitational influence of a further perturbing star (brown dwarf). The main goal is to study the orbital evolution of the planet. In special, we investigate the orientation (inclination) and the shape (eccentricity) of its orbit. One key feature explored is the time needed for the first flip in its orientation (prograde to retrograde). The gravitational potential is developed in closed form up to the third order. We have compared the secular evolution of systems with and without the third order term of the disturbing potential. The R2 (quadrupole) and R3 (octupole) terms of the disturbing potential are developed without using the elimination of nodes. Numerical simulations were also performed to compare with the analytical model using the N-body simulations with the Mercury code. The results show that the analytical model are in agreement with the numeric simulations.UNIFESP-Instituto de Ciência e Tecnologia Universidade Federal de Saõ PauloDivision of Space Mechanics and Control INPEUNESP-Univ Estadual PaulistaUNESP-Univ Estadual PaulistaUniversidade Federal de São Paulo (UNIFESP)INPEUniversidade Estadual Paulista (Unesp)Vilhena De Moraes, R.Carvalho, J. P.S.Prado, A. F.B.A.Winter, O. C. [UNESP]Mourão, D. C. [UNESP]2018-12-11T17:28:16Z2018-12-11T17:28:16Z2015-01-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObject1219-1227Advances in the Astronautical Sciences, v. 153, p. 1219-1227.0065-3438http://hdl.handle.net/11449/1780242-s2.0-84968736733Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengAdvances in the Astronautical Sciences0,187info:eu-repo/semantics/openAccess2024-07-02T14:29:48Zoai:repositorio.unesp.br:11449/178024Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T22:32:59.041287Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Orbital evolution of planet around a binary star |
title |
Orbital evolution of planet around a binary star |
spellingShingle |
Orbital evolution of planet around a binary star Vilhena De Moraes, R. |
title_short |
Orbital evolution of planet around a binary star |
title_full |
Orbital evolution of planet around a binary star |
title_fullStr |
Orbital evolution of planet around a binary star |
title_full_unstemmed |
Orbital evolution of planet around a binary star |
title_sort |
Orbital evolution of planet around a binary star |
author |
Vilhena De Moraes, R. |
author_facet |
Vilhena De Moraes, R. Carvalho, J. P.S. Prado, A. F.B.A. Winter, O. C. [UNESP] Mourão, D. C. [UNESP] |
author_role |
author |
author2 |
Carvalho, J. P.S. Prado, A. F.B.A. Winter, O. C. [UNESP] Mourão, D. C. [UNESP] |
author2_role |
author author author author |
dc.contributor.none.fl_str_mv |
Universidade Federal de São Paulo (UNIFESP) INPE Universidade Estadual Paulista (Unesp) |
dc.contributor.author.fl_str_mv |
Vilhena De Moraes, R. Carvalho, J. P.S. Prado, A. F.B.A. Winter, O. C. [UNESP] Mourão, D. C. [UNESP] |
description |
We study the secular dynamics of hierarchical (if there is a clearly defined binary and a third body which stays separate from the binary) triple systems composed by a Sun-like central star and a Jupiter-like planet, which are under the gravitational influence of a further perturbing star (brown dwarf). The main goal is to study the orbital evolution of the planet. In special, we investigate the orientation (inclination) and the shape (eccentricity) of its orbit. One key feature explored is the time needed for the first flip in its orientation (prograde to retrograde). The gravitational potential is developed in closed form up to the third order. We have compared the secular evolution of systems with and without the third order term of the disturbing potential. The R2 (quadrupole) and R3 (octupole) terms of the disturbing potential are developed without using the elimination of nodes. Numerical simulations were also performed to compare with the analytical model using the N-body simulations with the Mercury code. The results show that the analytical model are in agreement with the numeric simulations. |
publishDate |
2015 |
dc.date.none.fl_str_mv |
2015-01-01 2018-12-11T17:28:16Z 2018-12-11T17:28:16Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/conferenceObject |
format |
conferenceObject |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
Advances in the Astronautical Sciences, v. 153, p. 1219-1227. 0065-3438 http://hdl.handle.net/11449/178024 2-s2.0-84968736733 |
identifier_str_mv |
Advances in the Astronautical Sciences, v. 153, p. 1219-1227. 0065-3438 2-s2.0-84968736733 |
url |
http://hdl.handle.net/11449/178024 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Advances in the Astronautical Sciences 0,187 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
1219-1227 |
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_ |
1808129436189458432 |