Analysis of the orbital evolution of exoplanets

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dc.contributor.authorCarvalho, J. P.S.
dc.contributor.authorde Moraes, R. Vilhena
dc.contributor.authorPrado, A. F.B.A.
dc.contributor.authorMourão, D. C. [UNESP]
dc.contributor.authorWinter, O. C. [UNESP]
dc.contributor.institutionUniversidade Federal do Recôcavo da Bahia
dc.contributor.institutionUniversidade Federal de São Paulo (UNIFESP)
dc.contributor.institutionINPE
dc.contributor.institutionUniversidade Estadual Paulista (Unesp)
dc.date.accessioned2018-12-11T17:29:44Z
dc.date.available2018-12-11T17:29:44Z
dc.date.issued2016-10-01
dc.description.abstractAn exoplanet, or extrasolar planet, is a planet that does not orbit the Sun, but is around a different star, stellar remnant, or brown dwarf. Up to now, about 1900 exoplanets were discovered. To better understand the dynamics of these exoplanets, a study with respect to possible collisions of the planet with the central star is shown here. We present an expanded model in a small parameter that takes into account up to the fifth order to analyze the effect of this potential in the orbital elements of the extrasolar planet. Numerical simulations were also performed using the N-body simulations, using the software Mercury, to compare the results with the ones obtained by the analytical model. The numerical simulations are presented in two stages: one considering the celestial bodies as point masses and the other one taking into account their dimensions. This analysis showed that the planet collided with the central star in the moment of the first inversion for orbits with high inclinations in various situations. The results of the simulations of the equations developed in this study are consistent with the N-body numerical simulations. We analyze also the flip of the inclination taking into account the coupling of the perturbations of the third body, effect due to the precession of periastron and the tide effect. In general, we find that such perturbations combined delay the time of first inversion, but do not keep the planet in a prograde or retrograde orbit.en
dc.description.affiliationUFRB Centro de Ciência e Tecnologia em Energia e Sustentabilidade Universidade Federal do Recôcavo da Bahia
dc.description.affiliationUNIFESP Instituto de Ciência e Tecnologia Universidade Federal de São Paulo
dc.description.affiliationDivision of Space Mechanics and Control INPE
dc.description.affiliationUNESP Univ Estadual Paulista
dc.description.affiliationUnespUNESP Univ Estadual Paulista
dc.format.extent847-863
dc.identifierhttp://dx.doi.org/10.1007/s40314-015-0270-z
dc.identifier.citationComputational and Applied Mathematics, v. 35, n. 3, p. 847-863, 2016.
dc.identifier.doi10.1007/s40314-015-0270-z
dc.identifier.file2-s2.0-84989822055.pdf
dc.identifier.issn1807-0302
dc.identifier.issn0101-8205
dc.identifier.scopus2-s2.0-84989822055
dc.identifier.urihttp://hdl.handle.net/11449/178312
dc.language.isoeng
dc.relation.ispartofComputational and Applied Mathematics
dc.relation.ispartofsjr0,272
dc.rights.accessRightsAcesso aberto
dc.sourceScopus
dc.subjectAstrodynamics
dc.subjectExoplanets and third-body perturbation
dc.subjectPlanetary systems
dc.subjectStellar dynamics
dc.titleAnalysis of the orbital evolution of exoplanetsen
dc.typeArtigo

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