@Article{CarvalhoMorPraMouWin:2016:AnOrEv,
               author = "Carvalho, J. P. S. and Moraes, R. V. de and Prado, Antonio 
                         Fernando Bertachini de Almeida and Mour{\~a}o, D. C. and Winter, 
                         O. C.",
          affiliation = "{Universidade Federal do Rec{\^o}cavo da Bahia (UFRB)} and 
                         {Universidade Federal de S{\~a}o Paulo (UNIFESP)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Universidade Estadual 
                         Paulista (UNESP)} and {Universidade Estadual Paulista (UNESP)}",
                title = "Analysis of the orbital evolution of exoplanets",
              journal = "Computational and Applied Mathematics",
                 year = "2016",
               volume = "35",
               number = "3",
                pages = "847--863",
                month = "Oct.",
             keywords = "Astrodynamics, Planetary systems, Stellar dynamics, Exoplanets and 
                         third-body perturbation.",
             abstract = "An 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.",
                  doi = "10.1007/s40314-015-0270-z",
                  url = "http://dx.doi.org/10.1007/s40314-015-0270-z",
                 issn = "2238-3603",
             language = "en",
           targetfile = "Carvallho_Analysis.pdf",
        urlaccessdate = "27 abr. 2024"
}