The structure of the co-orbital stable regions as a function of the mass ratio
Autor(a) principal: | |
---|---|
Data de Publicação: | 2020 |
Outros Autores: | |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1093/MNRAS/STAA1727 http://hdl.handle.net/11449/208432 |
Resumo: | Although the search for extrasolar co-orbital bodies has not had success so far, it is believed that they must be as common as they are in the Solar system. Co-orbital systems have been widely studied, and there are several works on stability and even on formation. However, for the size and location of the stable regions, authors usually describe their results but do not provide a way to find them without numerical simulations, and, in most cases, the mass ratio value range is small. In this work, we study the structure of co-orbital stable regions for a wide range of mass ratio systems and build empirical equations to describe them. It allows estimating the size and location of co-orbital stable regions from a few system parameters. Thousands of massless particles were distributed in the co-orbital region of a massive secondary body and numerically simulated for a wide range of mass ratios (μ) adopting the planar circular restricted three-body problem. The results show that the upper limit of horseshoe regions is between 9.539 × 10−4 < μ < 1.192 × 10−3, which corresponds to a minimum angular distance from the secondary body to the separatrix of between 27.239o and 27.802o. We also found that the limit to existence of stability in the co-orbital region is about μ = 2.3313 × 10−2, much smaller than the value predicted by the linear theory. Polynomial functions to describe the stable region parameters were found, and they represent estimates of the angular and radial widths of the co-orbital stable regions for any system with 9.547 × 10−5 ≤ μ ≤ 2.331 × 10−2 |
id |
UNSP_dd79dc048c268357c5509fe2c6785742 |
---|---|
oai_identifier_str |
oai:repositorio.unesp.br:11449/208432 |
network_acronym_str |
UNSP |
network_name_str |
Repositório Institucional da UNESP |
repository_id_str |
2946 |
spelling |
The structure of the co-orbital stable regions as a function of the mass ratioCelestial mechanicsMethods: numericalMinor planets, asteroids: generalPlanets and satellites: dynamical evolution and stabilityAlthough the search for extrasolar co-orbital bodies has not had success so far, it is believed that they must be as common as they are in the Solar system. Co-orbital systems have been widely studied, and there are several works on stability and even on formation. However, for the size and location of the stable regions, authors usually describe their results but do not provide a way to find them without numerical simulations, and, in most cases, the mass ratio value range is small. In this work, we study the structure of co-orbital stable regions for a wide range of mass ratio systems and build empirical equations to describe them. It allows estimating the size and location of co-orbital stable regions from a few system parameters. Thousands of massless particles were distributed in the co-orbital region of a massive secondary body and numerically simulated for a wide range of mass ratios (μ) adopting the planar circular restricted three-body problem. The results show that the upper limit of horseshoe regions is between 9.539 × 10−4 < μ < 1.192 × 10−3, which corresponds to a minimum angular distance from the secondary body to the separatrix of between 27.239o and 27.802o. We also found that the limit to existence of stability in the co-orbital region is about μ = 2.3313 × 10−2, much smaller than the value predicted by the linear theory. Polynomial functions to describe the stable region parameters were found, and they represent estimates of the angular and radial widths of the co-orbital stable regions for any system with 9.547 × 10−5 ≤ μ ≤ 2.331 × 10−2Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)Grupo de Dinâmica Orbital e Planetologia UNESP – São Paulo State UniversityGrupo de Dinâmica Orbital e Planetologia UNESP – São Paulo State UniversityCNPq: 305210/2018-1Universidade Estadual Paulista (Unesp)Liberato, L. [UNESP]Winter, O. C. [UNESP]2021-06-25T11:12:04Z2021-06-25T11:12:04Z2020-01-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article3700-3707http://dx.doi.org/10.1093/MNRAS/STAA1727Monthly Notices of the Royal Astronomical Society, v. 496, n. 3, p. 3700-3707, 2020.1365-29660035-8711http://hdl.handle.net/11449/20843210.1093/MNRAS/STAA17272-s2.0-85101246116Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2024-07-02T14:28:57Zoai:repositorio.unesp.br:11449/208432Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T17:48:09.436934Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
The structure of the co-orbital stable regions as a function of the mass ratio |
title |
The structure of the co-orbital stable regions as a function of the mass ratio |
spellingShingle |
The structure of the co-orbital stable regions as a function of the mass ratio Liberato, L. [UNESP] Celestial mechanics Methods: numerical Minor planets, asteroids: general Planets and satellites: dynamical evolution and stability |
title_short |
The structure of the co-orbital stable regions as a function of the mass ratio |
title_full |
The structure of the co-orbital stable regions as a function of the mass ratio |
title_fullStr |
The structure of the co-orbital stable regions as a function of the mass ratio |
title_full_unstemmed |
The structure of the co-orbital stable regions as a function of the mass ratio |
title_sort |
The structure of the co-orbital stable regions as a function of the mass ratio |
author |
Liberato, L. [UNESP] |
author_facet |
Liberato, L. [UNESP] Winter, O. C. [UNESP] |
author_role |
author |
author2 |
Winter, O. C. [UNESP] |
author2_role |
author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (Unesp) |
dc.contributor.author.fl_str_mv |
Liberato, L. [UNESP] Winter, O. C. [UNESP] |
dc.subject.por.fl_str_mv |
Celestial mechanics Methods: numerical Minor planets, asteroids: general Planets and satellites: dynamical evolution and stability |
topic |
Celestial mechanics Methods: numerical Minor planets, asteroids: general Planets and satellites: dynamical evolution and stability |
description |
Although the search for extrasolar co-orbital bodies has not had success so far, it is believed that they must be as common as they are in the Solar system. Co-orbital systems have been widely studied, and there are several works on stability and even on formation. However, for the size and location of the stable regions, authors usually describe their results but do not provide a way to find them without numerical simulations, and, in most cases, the mass ratio value range is small. In this work, we study the structure of co-orbital stable regions for a wide range of mass ratio systems and build empirical equations to describe them. It allows estimating the size and location of co-orbital stable regions from a few system parameters. Thousands of massless particles were distributed in the co-orbital region of a massive secondary body and numerically simulated for a wide range of mass ratios (μ) adopting the planar circular restricted three-body problem. The results show that the upper limit of horseshoe regions is between 9.539 × 10−4 < μ < 1.192 × 10−3, which corresponds to a minimum angular distance from the secondary body to the separatrix of between 27.239o and 27.802o. We also found that the limit to existence of stability in the co-orbital region is about μ = 2.3313 × 10−2, much smaller than the value predicted by the linear theory. Polynomial functions to describe the stable region parameters were found, and they represent estimates of the angular and radial widths of the co-orbital stable regions for any system with 9.547 × 10−5 ≤ μ ≤ 2.331 × 10−2 |
publishDate |
2020 |
dc.date.none.fl_str_mv |
2020-01-01 2021-06-25T11:12:04Z 2021-06-25T11:12:04Z |
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/STAA1727 Monthly Notices of the Royal Astronomical Society, v. 496, n. 3, p. 3700-3707, 2020. 1365-2966 0035-8711 http://hdl.handle.net/11449/208432 10.1093/MNRAS/STAA1727 2-s2.0-85101246116 |
url |
http://dx.doi.org/10.1093/MNRAS/STAA1727 http://hdl.handle.net/11449/208432 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 496, n. 3, p. 3700-3707, 2020. 1365-2966 0035-8711 10.1093/MNRAS/STAA1727 2-s2.0-85101246116 |
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 |
3700-3707 |
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_ |
1808128860400648192 |