Planet-planet scattering in presence of a companion star

TL;DR

This study investigates how a companion star influences planet-planet scattering, revealing that it broadens orbital distributions, reduces system stability, and affects planet formation processes in binary star systems.

Contribution

It provides empirical formulas and simulation results showing the impact of a secondary star on planetary system stability and orbital evolution, extending understanding of planet dynamics in binaries.

Findings

Secondary star broadens the orbital distribution of inner planets.

Presence of the companion reduces the frequency of stable two-planet systems.

Binary eccentricity influences the extent of the stability region.

Abstract

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.