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Planet-planet scattering in presence of a companion star

By SpaceRef Editor
December 13, 2021
Filed under , , ,

Francesco Marzari, Makiko Nagasawa, Krzyszof Goździewski

Planet Planet scattering is a leading dynamical mechanism invoked to explain the present orbital distribution of exoplanets. Many stars belong to binary systems, therefore it is important to understand how this mechanism works in presence of a companion star. We focus on systems of three planets orbiting the primary star and estimate the timescale for instability finding that it scales with the keplerian period for systems that have the same ratio between inner planet and binary semimajor axes. An empirical formula is also derived from simulations to estimate how the the binary eccentricity affects the extent of the stability region. The presence of the secondary star affects the Planet Planet scattering outcomes causing a broadening of the final distribution in semimajor axis of the inner planet as some of the orbital energy of the planets is absorbed by the companion star. Repeated approaches to the secondary star causes also a significant reduction in the frequency of surviving two planet systems in particular for larger values of the inner planet semimajor axis. The formation of Kozai states with the companion star increases the number of planets which may be tidally circularized. To predict the possible final distribution of planets in binaries we have performed a large number of simulations where the initial semimajor axis of the inner planets is chosen randomly. For small values of the binary semimajor axis, the higher frequency of collision alter the final planet orbital distributions which, however, beyond 50 au appear to be scalable to wider binary separations.

Comments: Accepted for publication in MNRAS

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

Cite as: arXiv:2112.05012 [astro-ph.EP] (or arXiv:2112.05012v1 [astro-ph.EP] for this version)

Submission history

From: Francesco Marzari Dr. 

[v1] Thu, 9 Dec 2021 16:10:20 UTC (9,227 KB)

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