Orbital Stability of Circumstellar Planets in Binary Systems
Abstract
Planets that orbit only one of the stars in stellar binary systems (i.e., circumstellar) are dynamically constrained to a limited range of orbital parameters, and understanding conditions on their stability is thus of great importance in exoplanet searches. We perform ∼700 million Nbody simulations to identify how stability regions depend on properties of the binary, as well as the starting planetary inclination and mean longitude relative to the binary orbit. Moreover, we provide grid interpolation maps and lookup tables for the community to use our results. Through Monte Carlo methods, we determine that planets with a semimajor axis a_{p} ≲ 8% of the binary semimajor axis a_{bin} will likely be stable, given the known distribution of binary star parameters. This estimate varies in the LidovKozai regime or for retrograde orbits to 4% or 10% of a_{bin}, respectively. Our method to quickly determine the circumstellar stability limit is important for interpreting observations of binaries using direct imaging with the James Webb Space Telescope, photometry with the Transiting Exoplanet Survey Satellite, or even astrometry with Gaia.
 Publication:

The Astronomical Journal
 Pub Date:
 March 2020
 DOI:
 10.3847/15383881/ab64fa
 arXiv:
 arXiv:1912.11019
 Bibcode:
 2020AJ....159...80Q
 Keywords:

 1184;
 695;
 490;
 498;
 154;
 Astrophysics  Earth and Planetary Astrophysics;
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 28 pages, 10 figures, 6 tables