@InProceedings{MoraesCarPraWinMou:2014:OrEvPl,
               author = "Moraes, Rodolpho Vilhena de and Carvalho, Jean Paulo dos Santos 
                         and Prado, Antonio Fernando Bertachini de Almeida and Winter, 
                         Othon C and Mour{\~a}o, D. C.",
          affiliation = "{Universidade Federal de S{\~a}o Paulo (UNIFESP)} 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 = "Orbital evolution of planet around a binary star",
            booktitle = "Proceedings...",
                 year = "2014",
                pages = "9pp",
         organization = "IAA Conference on Dynamics \& Control of Space Systems, 2. 
                         (DYCOSS).",
             keywords = "astrodin{\^a}mica, mec{\^a}nica celeste.",
             abstract = "We study the secular dynamics of hierarchical (if there is a 
                         clearly defined binary and a third body which stays separate from 
                         the binary) triple systems composed by a Sun-like central star and 
                         a Jupiter-like planet, which are under the gravitational influence 
                         of a further perturbing star (brown dwarf). The main goal is to 
                         study the orbital evolution of the planet. In special, we 
                         investigate the orientation (inclination) and the shape 
                         (eccentricity) of its orbit. One key feature explored is the time 
                         needed for the first flip in its orientation (prograde to 
                         retrograde). The gravitational potential is developed in closed 
                         form up to the third order. We have compared the secular evolution 
                         of systems with and without the third order term of the disturbing 
                         potential. The R2 (quadrupole) and R3 (octupole) terms of the 
                         disturbing potential are developed without using the elimination 
                         of nodes. Numerical simulations were also performed to compare 
                         with the analytical model using the N-body simulations with the 
                         Mercury code. The results show that the analytical model are in 
                         agreement with the numeric simulations.",
  conference-location = "Roma",
      conference-year = "mar. 24-26, 2014",
                label = "lattes: 7340081273816424 3 MoraesCarvPradWint:2014:OrEvPl",
             language = "en",
           targetfile = "IAA-AAS-DyCoSS2-14-11-08.pdf",
               volume = "1",
        urlaccessdate = "20 abr. 2024"
}