Stability of coorbital planets around binaries

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MetadadosDescriçãoIdioma
Autor(es): dc.contributorUniversität Tübingen-
Autor(es): dc.contributorImperial College London-
Autor(es): dc.contributorValdosta State University-
Autor(es): dc.contributorUniversidade Estadual Paulista (UNESP)-
Autor(es): dc.creatorAdelbert, Stefan-
Autor(es): dc.creatorPenzlin, Anna B. T.-
Autor(es): dc.creatorSchäfer, Christoph M.-
Autor(es): dc.creatorKley, Wilhelm-
Autor(es): dc.creatorQuarles, Billy-
Autor(es): dc.creatorSfair, Rafael-
Data de aceite: dc.date.accessioned2025-08-21T21:48:06Z-
Data de disponibilização: dc.date.available2025-08-21T21:48:06Z-
Data de envio: dc.date.issued2025-04-29-
Data de envio: dc.date.issued2023-11-30-
Fonte completa do material: dc.identifierhttp://dx.doi.org/10.1051/0004-6361/202244329-
Fonte completa do material: dc.identifierhttps://hdl.handle.net/11449/298153-
Fonte: dc.identifier.urihttp://educapes.capes.gov.br/handle/11449/298153-
Descrição: dc.descriptionIn previous hydrodynamical simulations, we found a mechanism for nearly circular binary stars, such as Kepler-413, to trap two planets in a stable 1:1 resonance. Therefore, the stability of coorbital configurations becomes a relevant question for planet formation around binary stars. For this work, we investigated the coorbital planet stability using a Kepler-413 analogue as an example and then expanded the parameters to study a general n-body stability of planet pairs in eccentric horseshoe orbits around binaries. The stability was tested by evolving the planet orbits for 105 binary periods with varying initial semi-major axes and planet eccentricities. The unstable region of a single circumbinary planet is used as a comparison to the investigated coorbital configurations in this work. We confirm previous findings on the stability of single planets and find a first order linear relation between the orbit eccentricity ep and pericentre to identify stable orbits for various binary configurations. Such a linear relation is also found for the stability of 1:1 resonant planets around binaries. Stable orbits for eccentric horseshoe configurations exist with a pericentre closer than seven binary separations and, in the case of Kepler-413, the pericentre of the first stable orbit can be approximated by rc,peri = (2.90 ep + 2.46) abin-
Descrição: dc.descriptionInstitut für Astronomie und Astrophysik Universität Tübingen, Auf der Morgenstelle 10-
Descrição: dc.descriptionAstrophysics Group Department of Physics Imperial College London, Prince Consort Rd-
Descrição: dc.descriptionDepartment of Applied Mathematics and Physics Valdosta State University-
Descrição: dc.descriptionGrupo de Dinâmica Orbital e Planetologia São Paulo State University Unesp, Guaratinguetá-
Descrição: dc.descriptionGrupo de Dinâmica Orbital e Planetologia São Paulo State University Unesp, Guaratinguetá-
Idioma: dc.languageen-
Relação: dc.relationAstronomy and Astrophysics-
???dc.source???: dc.sourceScopus-
Palavras-chave: dc.subjectBinaries: general-
Palavras-chave: dc.subjectPlanets and satellites: dynamical evolution and stability-
Título: dc.titleStability of coorbital planets around binaries-
Tipo de arquivo: dc.typelivro digital-
Aparece nas coleções:Repositório Institucional - Unesp

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