Sphere of influence and gravitational capture radius: a dynamical approach
Autor(a) principal: | |
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Data de Publicação: | 2008 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1111/j.1365-2966.2008.13833.x http://hdl.handle.net/11449/42361 |
Resumo: | For problems in celestial mechanics that involve close encounters, it is necessary to determine the region where the gravitational influence of a body prevails over the influence of other bodies. From this need comes the concept of the sphere of influence. The models most used for the calculation of the radii of these spheres are the Hill sphere and the Laplace sphere. These are determined in terms of constant parameters, resulting in a fixed-size sphere, independent of the conditions of the encounter. In this paper, we present a numerical model for the sphere of influence, whose radius has been defined in terms of the initial relative velocity of the encounter, and of the mass ratio of the system considered. The same idea was applied to the delimitation of the regions where the phenomenon of temporary gravitational capture occurs, for some given initial conditions. With this goal, a numerical study was made through integrations of the restricted three-body problem and by monitoring the energy variation of the two-body problem. This study resulted in a complete mapping of the influence and capture regions, considering systems with amass ratio from 10(-1) to 10(-12), with the empirical functions for the calculation of these limits, called the capture radius and the influence radius. |
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Sphere of influence and gravitational capture radius: a dynamical approachmethods: numericalcelestial mechanicsSolar system: generalFor problems in celestial mechanics that involve close encounters, it is necessary to determine the region where the gravitational influence of a body prevails over the influence of other bodies. From this need comes the concept of the sphere of influence. The models most used for the calculation of the radii of these spheres are the Hill sphere and the Laplace sphere. These are determined in terms of constant parameters, resulting in a fixed-size sphere, independent of the conditions of the encounter. In this paper, we present a numerical model for the sphere of influence, whose radius has been defined in terms of the initial relative velocity of the encounter, and of the mass ratio of the system considered. The same idea was applied to the delimitation of the regions where the phenomenon of temporary gravitational capture occurs, for some given initial conditions. With this goal, a numerical study was made through integrations of the restricted three-body problem and by monitoring the energy variation of the two-body problem. This study resulted in a complete mapping of the influence and capture regions, considering systems with amass ratio from 10(-1) to 10(-12), with the empirical functions for the calculation of these limits, called the capture radius and the influence radius.Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)Inst Nacl Pesquisas Espaciais, BR-12201970 Sao Jose Dos Campos, SP, BrazilSão Paulo State Univ UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, BrazilObserv Nacl, BR-20921400 Rio de Janeiro, BrazilSão Paulo State Univ UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, BrazilWiley-Blackwell Publishing, IncInstituto Nacional de Pesquisas Espaciais (INPE)Universidade Estadual Paulista (Unesp)Observ NaclAraujo, R. A. N.Winter, O. C. [UNESP]Prado, A. F. B. A.Martins, R. Vieira2014-05-20T15:33:56Z2014-05-20T15:33:56Z2008-12-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article675-684application/pdfhttp://dx.doi.org/10.1111/j.1365-2966.2008.13833.xMonthly Notices of The Royal Astronomical Society. Malden: Wiley-blackwell Publishing, Inc, v. 391, n. 2, p. 675-684, 2008.0035-8711http://hdl.handle.net/11449/4236110.1111/j.1365-2966.2008.13833.xWOS:000261265300017WOS000261265300017.pdf0960024575647258Web of Sciencereponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Society5.1942,346info:eu-repo/semantics/openAccess2024-07-02T14:29:31Zoai:repositorio.unesp.br:11449/42361Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T21:40:34.753680Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Sphere of influence and gravitational capture radius: a dynamical approach |
title |
Sphere of influence and gravitational capture radius: a dynamical approach |
spellingShingle |
Sphere of influence and gravitational capture radius: a dynamical approach Araujo, R. A. N. methods: numerical celestial mechanics Solar system: general |
title_short |
Sphere of influence and gravitational capture radius: a dynamical approach |
title_full |
Sphere of influence and gravitational capture radius: a dynamical approach |
title_fullStr |
Sphere of influence and gravitational capture radius: a dynamical approach |
title_full_unstemmed |
Sphere of influence and gravitational capture radius: a dynamical approach |
title_sort |
Sphere of influence and gravitational capture radius: a dynamical approach |
author |
Araujo, R. A. N. |
author_facet |
Araujo, R. A. N. Winter, O. C. [UNESP] Prado, A. F. B. A. Martins, R. Vieira |
author_role |
author |
author2 |
Winter, O. C. [UNESP] Prado, A. F. B. A. Martins, R. Vieira |
author2_role |
author author author |
dc.contributor.none.fl_str_mv |
Instituto Nacional de Pesquisas Espaciais (INPE) Universidade Estadual Paulista (Unesp) Observ Nacl |
dc.contributor.author.fl_str_mv |
Araujo, R. A. N. Winter, O. C. [UNESP] Prado, A. F. B. A. Martins, R. Vieira |
dc.subject.por.fl_str_mv |
methods: numerical celestial mechanics Solar system: general |
topic |
methods: numerical celestial mechanics Solar system: general |
description |
For problems in celestial mechanics that involve close encounters, it is necessary to determine the region where the gravitational influence of a body prevails over the influence of other bodies. From this need comes the concept of the sphere of influence. The models most used for the calculation of the radii of these spheres are the Hill sphere and the Laplace sphere. These are determined in terms of constant parameters, resulting in a fixed-size sphere, independent of the conditions of the encounter. In this paper, we present a numerical model for the sphere of influence, whose radius has been defined in terms of the initial relative velocity of the encounter, and of the mass ratio of the system considered. The same idea was applied to the delimitation of the regions where the phenomenon of temporary gravitational capture occurs, for some given initial conditions. With this goal, a numerical study was made through integrations of the restricted three-body problem and by monitoring the energy variation of the two-body problem. This study resulted in a complete mapping of the influence and capture regions, considering systems with amass ratio from 10(-1) to 10(-12), with the empirical functions for the calculation of these limits, called the capture radius and the influence radius. |
publishDate |
2008 |
dc.date.none.fl_str_mv |
2008-12-01 2014-05-20T15:33:56Z 2014-05-20T15:33:56Z |
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/10.1111/j.1365-2966.2008.13833.x Monthly Notices of The Royal Astronomical Society. Malden: Wiley-blackwell Publishing, Inc, v. 391, n. 2, p. 675-684, 2008. 0035-8711 http://hdl.handle.net/11449/42361 10.1111/j.1365-2966.2008.13833.x WOS:000261265300017 WOS000261265300017.pdf 0960024575647258 |
url |
http://dx.doi.org/10.1111/j.1365-2966.2008.13833.x http://hdl.handle.net/11449/42361 |
identifier_str_mv |
Monthly Notices of The Royal Astronomical Society. Malden: Wiley-blackwell Publishing, Inc, v. 391, n. 2, p. 675-684, 2008. 0035-8711 10.1111/j.1365-2966.2008.13833.x WOS:000261265300017 WOS000261265300017.pdf 0960024575647258 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Monthly Notices of the Royal Astronomical Society 5.194 2,346 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
675-684 application/pdf |
dc.publisher.none.fl_str_mv |
Wiley-Blackwell Publishing, Inc |
publisher.none.fl_str_mv |
Wiley-Blackwell Publishing, Inc |
dc.source.none.fl_str_mv |
Web of Science 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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1808129345509654528 |