Planet dispersal in binary systems during transient multiple star phases
Dipartimento di Fisica, University of Padova, Via Marzolo 8, 35131 Padova, Italy e-mail: firstname.lastname@example.org
2 LAM, Traverse du Siphon, BP 8, Les Trois Luc, 13376 Marseille Cedex 12, France e-mail: email@example.com
Accepted: 31 May 2007
Aims.If a significant fraction of binary star systems spent some time as inclined triple systems, either during their formation process or as the outcome of several close dynamical encounters in a crowded stellar environemnt, then the number of planets in binaries would be significantly lower than around single stars. The stellar chaotic phase preceding the instability of the triple system and the wide oscillations in eccentricity and inclination of the companion star due to the high mutual inclination between the companion and the singleton would quickly eject planets orbiting the binary in S-type orbits.
Methods.We perform numerical simulations of the dynamical evolution of hierarchical triple star systems with planets hosted around the primary star of the inner binary. Different values of mutual inclination, binary separation and singleton initial semimajor axis are explored in a statistical way.
Results.We find that a significant mutual inclination im between the singleton and the binary is a key factor for instability of the planetary system. When im is larger than ~ the fraction of planets in the binary surviving the chaotic phase of the triple declines dramatically. The combination of eccentricity and inclination oscillations of the binary companion induced by the secular perturbations of the singleton and the sequence of close encounters preceding the ejection of one star fully destabilize a planetary system extending beyond 1 AU from the star. For im around the percentage of surviving planets is lower than 20% for all binaries with a semimajor axis smaller than 200 AU.
Conclusions.The frequency of planets in binaries with low separation may be strongly reduced by the residence of the pair in the past in a temporary inclined hierarchical triple.
Key words: methods: N-body simulations / stars: planetary systems
© ESO, 2007