Terrestrial Planet Formation in Binary Star Systems

Abstract

A binary star system is the most common result of the star formation process, and binary companions can disrupt both the formation of terrestrial planets and their long term prospects for stability. We present results from a large set of numerical simulations of the final stages of terrestrial planet formation - from Moon- to Mars-sized planetary embryos to planets - in main-sequence binary star systems. We examine planetary accretion around both stars ('P-type' circumbinary orbits) or individual stars ('S-type' orbits) in binary systems, including terrestrial planet formation around each star in Alpha Centauri AB, the closest binary star system to the Sun. For comparison, we also simulate planetary growth from the same initial disk placed in the Sun-Jupiter-Saturn system and also around the Sun with neither giant planets nor a stellar companion perturbing the system. Our simulations show that giant and stellar companions not only truncate the disk, but hasten the accretion process by stirring up the planetary embryos to higher eccentricities and inclinations. Terrestrial planets similar to those in our Solar System formed around individual stars in simulations with the binary periastron (closest approach) greater than about 5 AU. Terrestrial planet growth within circumbinary disks was uninhibited around inner binary star systems with binary apastrons (maximum separation) less than ~0.2 AU. Results from our simulations can be scaled for different stellar and disk parameters. Approximately 50 - 60% of binary star systems - from contact binaries to separations of nearly a parsec - satisfy these constraints. Given that the galaxy contains more than 100 billion star systems, a large number of systems remain habitable based on the dynamic considerations of this research.