On the stability of additional moons orbiting Kepler-1625 b
Autor(a) principal: | |
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Data de Publicação: | 2022 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1093/mnras/stab3576 http://hdl.handle.net/11449/234272 |
Resumo: | Since it was proposed, the exomoon candidate Kepler-1625 b-I has changed the way we see satellite systems. Because of its unusual physical characteristics, many questions about the stability and origin of this candidate have been raised. Currently, we have enough theoretical studies to show that if Kepler-1625 b-I is indeed confirmed, it will be stable. Regarding its origin, previous works indicated that the most likely scenario is capture, although conditions for in situ formation have also been investigated. In this work, we assume that Kepler-1625 b-I is an exomoon and study the possibility of an additional, massive exomoon being stable in the same system. To model this scenario, we perform N-body simulations of a system including the planet, Kepler-1625 b-I, and one extra Earth-like satellite. Based on previous results, the satellites in our system will be exposed to tidal interactions with the planet and to gravitational effects owing to the rotation of the planet. We find that the satellite system around Kepler-1625 b is capable of harbouring two massive satellites. The extra Earth-like satellite can be stable in various locations between the planet and Kepler-1625 b-I, with a preference for regions inside $25\, R_{\rm p}$. Our results suggest that the strong tidal interaction between the planet and the satellites is an important mechanism to ensure the stability of satellites in circular orbits closer to the planet, while the 2:1 mean motion resonance between the Earth-like satellite and Kepler-1625 b-I would provide stability for satellites in wider orbits. |
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On the stability of additional moons orbiting Kepler-1625 bplanets and satellites: dynamical evolution and stabilityplanets and satellites: individual: Kepler-1625 b-ISince it was proposed, the exomoon candidate Kepler-1625 b-I has changed the way we see satellite systems. Because of its unusual physical characteristics, many questions about the stability and origin of this candidate have been raised. Currently, we have enough theoretical studies to show that if Kepler-1625 b-I is indeed confirmed, it will be stable. Regarding its origin, previous works indicated that the most likely scenario is capture, although conditions for in situ formation have also been investigated. In this work, we assume that Kepler-1625 b-I is an exomoon and study the possibility of an additional, massive exomoon being stable in the same system. To model this scenario, we perform N-body simulations of a system including the planet, Kepler-1625 b-I, and one extra Earth-like satellite. Based on previous results, the satellites in our system will be exposed to tidal interactions with the planet and to gravitational effects owing to the rotation of the planet. We find that the satellite system around Kepler-1625 b is capable of harbouring two massive satellites. The extra Earth-like satellite can be stable in various locations between the planet and Kepler-1625 b-I, with a preference for regions inside $25\, R_{\rm p}$. Our results suggest that the strong tidal interaction between the planet and the satellites is an important mechanism to ensure the stability of satellites in circular orbits closer to the planet, while the 2:1 mean motion resonance between the Earth-like satellite and Kepler-1625 b-I would provide stability for satellites in wider orbits.UNESP Universidade Estadual Paulista Grupo de Dinâmica Orbital and Planetologia, São PauloBioengineering and Aerospace Engineering Department Universidad Carlos III de Madrid, LeganCrossed D sign©sUNESP Universidade Estadual Paulista Grupo de Dinâmica Orbital and Planetologia, São PauloUniversidade Estadual Paulista (UNESP)Universidad Carlos III de MadridMoraes, R. A. [UNESP]Borderes-Motta, G.Winter, O. C. [UNESP]Monteiro, J. [UNESP]2022-05-01T15:46:10Z2022-05-01T15:46:10Z2022-02-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article2583-2596http://dx.doi.org/10.1093/mnras/stab3576Monthly Notices of the Royal Astronomical Society, v. 510, n. 2, p. 2583-2596, 2022.1365-29660035-8711http://hdl.handle.net/11449/23427210.1093/mnras/stab35762-s2.0-85126462985Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2022-05-01T15:46:10Zoai:repositorio.unesp.br:11449/234272Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462022-05-01T15:46:10Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
On the stability of additional moons orbiting Kepler-1625 b |
title |
On the stability of additional moons orbiting Kepler-1625 b |
spellingShingle |
On the stability of additional moons orbiting Kepler-1625 b Moraes, R. A. [UNESP] planets and satellites: dynamical evolution and stability planets and satellites: individual: Kepler-1625 b-I |
title_short |
On the stability of additional moons orbiting Kepler-1625 b |
title_full |
On the stability of additional moons orbiting Kepler-1625 b |
title_fullStr |
On the stability of additional moons orbiting Kepler-1625 b |
title_full_unstemmed |
On the stability of additional moons orbiting Kepler-1625 b |
title_sort |
On the stability of additional moons orbiting Kepler-1625 b |
author |
Moraes, R. A. [UNESP] |
author_facet |
Moraes, R. A. [UNESP] Borderes-Motta, G. Winter, O. C. [UNESP] Monteiro, J. [UNESP] |
author_role |
author |
author2 |
Borderes-Motta, G. Winter, O. C. [UNESP] Monteiro, J. [UNESP] |
author2_role |
author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (UNESP) Universidad Carlos III de Madrid |
dc.contributor.author.fl_str_mv |
Moraes, R. A. [UNESP] Borderes-Motta, G. Winter, O. C. [UNESP] Monteiro, J. [UNESP] |
dc.subject.por.fl_str_mv |
planets and satellites: dynamical evolution and stability planets and satellites: individual: Kepler-1625 b-I |
topic |
planets and satellites: dynamical evolution and stability planets and satellites: individual: Kepler-1625 b-I |
description |
Since it was proposed, the exomoon candidate Kepler-1625 b-I has changed the way we see satellite systems. Because of its unusual physical characteristics, many questions about the stability and origin of this candidate have been raised. Currently, we have enough theoretical studies to show that if Kepler-1625 b-I is indeed confirmed, it will be stable. Regarding its origin, previous works indicated that the most likely scenario is capture, although conditions for in situ formation have also been investigated. In this work, we assume that Kepler-1625 b-I is an exomoon and study the possibility of an additional, massive exomoon being stable in the same system. To model this scenario, we perform N-body simulations of a system including the planet, Kepler-1625 b-I, and one extra Earth-like satellite. Based on previous results, the satellites in our system will be exposed to tidal interactions with the planet and to gravitational effects owing to the rotation of the planet. We find that the satellite system around Kepler-1625 b is capable of harbouring two massive satellites. The extra Earth-like satellite can be stable in various locations between the planet and Kepler-1625 b-I, with a preference for regions inside $25\, R_{\rm p}$. Our results suggest that the strong tidal interaction between the planet and the satellites is an important mechanism to ensure the stability of satellites in circular orbits closer to the planet, while the 2:1 mean motion resonance between the Earth-like satellite and Kepler-1625 b-I would provide stability for satellites in wider orbits. |
publishDate |
2022 |
dc.date.none.fl_str_mv |
2022-05-01T15:46:10Z 2022-05-01T15:46:10Z 2022-02-01 |
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/10.1093/mnras/stab3576 Monthly Notices of the Royal Astronomical Society, v. 510, n. 2, p. 2583-2596, 2022. 1365-2966 0035-8711 http://hdl.handle.net/11449/234272 10.1093/mnras/stab3576 2-s2.0-85126462985 |
url |
http://dx.doi.org/10.1093/mnras/stab3576 http://hdl.handle.net/11449/234272 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 510, n. 2, p. 2583-2596, 2022. 1365-2966 0035-8711 10.1093/mnras/stab3576 2-s2.0-85126462985 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Monthly Notices of the Royal Astronomical Society |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
2583-2596 |
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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1799965373303357440 |