The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems
Autor(a) principal: | |
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Data de Publicação: | 2023 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1093/mnras/stad314 http://hdl.handle.net/11449/249991 |
Resumo: | Exomoons are a missing piece of exoplanetary science. Recently, two promising candidates were proposed, Kepler-1625 b-I and Kepler-1708 b-I. While the latter still lacks a dynamical analysis of its stability, Kepler-1625 b-I has already been the subject of several studies regarding its stability and origin. Moreover, previous works have shown that this satellite system could harbour at least two stable massive moons. Motivated by these results, we explored the stability of co-orbital exomoons using the candidates Kepler-1625 b-I and Kepler-1708 b-I as case studies. To do so, we performed numerical simulations of systems composed of the star, planet, and the co-orbital pair formed by the proposed candidates and another massive body. For the additional satellite, we varied its mass and size from a Mars-like to the case where both satellites have the same physical characteristics. We investigated the co-orbital region around the Lagrangian equilibrium point L4 of the system, setting the orbital separation between the satellites from θmin = 30◦ to θmax = 90◦. Our results show that stability islands are possible in the co-orbital region of Kepler-1708 b-I as a function of the co-orbital companion's mass and angular separation. Also, we identified that resonances of librational frequencies, especially the 2:1 resonance, can constrain the mass of the co-orbital companion. On the other hand, we found that the proximity between the host planet and the star makes the co-orbital region around Kepler-1625 b-I unstable for a massive companion. Finally, we provide TTV profiles for a planet orbited by co-orbital exomoons. |
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The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systemsplanetsplanets and satellites: dynamical evolution and stabilitysatellites: individual (Kepler-1625 b-I, Kepler-1708 b-I)Exomoons are a missing piece of exoplanetary science. Recently, two promising candidates were proposed, Kepler-1625 b-I and Kepler-1708 b-I. While the latter still lacks a dynamical analysis of its stability, Kepler-1625 b-I has already been the subject of several studies regarding its stability and origin. Moreover, previous works have shown that this satellite system could harbour at least two stable massive moons. Motivated by these results, we explored the stability of co-orbital exomoons using the candidates Kepler-1625 b-I and Kepler-1708 b-I as case studies. To do so, we performed numerical simulations of systems composed of the star, planet, and the co-orbital pair formed by the proposed candidates and another massive body. For the additional satellite, we varied its mass and size from a Mars-like to the case where both satellites have the same physical characteristics. We investigated the co-orbital region around the Lagrangian equilibrium point L4 of the system, setting the orbital separation between the satellites from θmin = 30◦ to θmax = 90◦. Our results show that stability islands are possible in the co-orbital region of Kepler-1708 b-I as a function of the co-orbital companion's mass and angular separation. Also, we identified that resonances of librational frequencies, especially the 2:1 resonance, can constrain the mass of the co-orbital companion. On the other hand, we found that the proximity between the host planet and the star makes the co-orbital region around Kepler-1625 b-I unstable for a massive companion. Finally, we provide TTV profiles for a planet orbited by co-orbital exomoons.Advanced Scientific Computing ResearchUniversidade Estadual PaulistaFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)UNESP São Paulo State University Grupo de Dinâmica Orbital & Planetologia, GuaratinguetáUC3M Univ. Carlos III de Madrid Bioengineering and Aerospace Engineering Department, LeganésIRF Swedish Institute of Space Physics, KirunaUNESP São Paulo State University Grupo de Dinâmica Orbital & Planetologia, GuaratinguetáFAPESP: 2016/24561-0CNPq: 305210/2018-1CAPES: 88887.310463/2018-00Universidade Estadual Paulista (UNESP)Bioengineering and Aerospace Engineering DepartmentSwedish Institute of Space PhysicsMoraes, R. A. [UNESP]Borderes-Motta, G.Winter, O. C. [UNESP]Mourão, D. C. [UNESP]2023-07-29T16:14:48Z2023-07-29T16:14:48Z2023-04-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article2163-2177http://dx.doi.org/10.1093/mnras/stad314Monthly Notices of the Royal Astronomical Society, v. 520, n. 2, p. 2163-2177, 2023.1365-29660035-8711http://hdl.handle.net/11449/24999110.1093/mnras/stad3142-s2.0-85160321611Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2023-07-29T16:14:48Zoai:repositorio.unesp.br:11449/249991Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462023-07-29T16:14:48Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems |
title |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems |
spellingShingle |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems Moraes, R. A. [UNESP] planets planets and satellites: dynamical evolution and stability satellites: individual (Kepler-1625 b-I, Kepler-1708 b-I) |
title_short |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems |
title_full |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems |
title_fullStr |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems |
title_full_unstemmed |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems |
title_sort |
The dynamics of co-orbital giant exomoons - applications for the Kepler-1625 b and Kepler-1708 b satellite systems |
author |
Moraes, R. A. [UNESP] |
author_facet |
Moraes, R. A. [UNESP] Borderes-Motta, G. Winter, O. C. [UNESP] Mourão, D. C. [UNESP] |
author_role |
author |
author2 |
Borderes-Motta, G. Winter, O. C. [UNESP] Mourão, D. C. [UNESP] |
author2_role |
author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (UNESP) Bioengineering and Aerospace Engineering Department Swedish Institute of Space Physics |
dc.contributor.author.fl_str_mv |
Moraes, R. A. [UNESP] Borderes-Motta, G. Winter, O. C. [UNESP] Mourão, D. C. [UNESP] |
dc.subject.por.fl_str_mv |
planets planets and satellites: dynamical evolution and stability satellites: individual (Kepler-1625 b-I, Kepler-1708 b-I) |
topic |
planets planets and satellites: dynamical evolution and stability satellites: individual (Kepler-1625 b-I, Kepler-1708 b-I) |
description |
Exomoons are a missing piece of exoplanetary science. Recently, two promising candidates were proposed, Kepler-1625 b-I and Kepler-1708 b-I. While the latter still lacks a dynamical analysis of its stability, Kepler-1625 b-I has already been the subject of several studies regarding its stability and origin. Moreover, previous works have shown that this satellite system could harbour at least two stable massive moons. Motivated by these results, we explored the stability of co-orbital exomoons using the candidates Kepler-1625 b-I and Kepler-1708 b-I as case studies. To do so, we performed numerical simulations of systems composed of the star, planet, and the co-orbital pair formed by the proposed candidates and another massive body. For the additional satellite, we varied its mass and size from a Mars-like to the case where both satellites have the same physical characteristics. We investigated the co-orbital region around the Lagrangian equilibrium point L4 of the system, setting the orbital separation between the satellites from θmin = 30◦ to θmax = 90◦. Our results show that stability islands are possible in the co-orbital region of Kepler-1708 b-I as a function of the co-orbital companion's mass and angular separation. Also, we identified that resonances of librational frequencies, especially the 2:1 resonance, can constrain the mass of the co-orbital companion. On the other hand, we found that the proximity between the host planet and the star makes the co-orbital region around Kepler-1625 b-I unstable for a massive companion. Finally, we provide TTV profiles for a planet orbited by co-orbital exomoons. |
publishDate |
2023 |
dc.date.none.fl_str_mv |
2023-07-29T16:14:48Z 2023-07-29T16:14:48Z 2023-04-01 |
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/stad314 Monthly Notices of the Royal Astronomical Society, v. 520, n. 2, p. 2163-2177, 2023. 1365-2966 0035-8711 http://hdl.handle.net/11449/249991 10.1093/mnras/stad314 2-s2.0-85160321611 |
url |
http://dx.doi.org/10.1093/mnras/stad314 http://hdl.handle.net/11449/249991 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 520, n. 2, p. 2163-2177, 2023. 1365-2966 0035-8711 10.1093/mnras/stad314 2-s2.0-85160321611 |
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 |
2163-2177 |
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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1799964824518524928 |