Dynamics of a Probable Earth-mass Planet in the GJ 832 System

作者：Satyal S^*; Griffith J; Musielak Z E

来源：Astrophysical Journal, 2017, 845(2): 106.

DOI：10.3847/1538-4357/aa80e2

• planets and satellites: dynamical evolution and stability
• planets and satellites: individual (GJ 832b, GJ 832c)

The stability of planetary orbits around the GJ 832 star system, which contains inner (GJ 832c) and outer (GJ 832b) planets, is investigated numerically and a detailed phase-space analysis is performed. Special attention is given to the existence of stable orbits for a planet less than 15M(circle plus) that is injected between the inner and outer planets. Thus, numerical simulations are performed for three and four bodies in elliptical orbits (or circular for special cases) by using a large number of initial conditions that cover the selected phase-spaces of the planet's orbital parameters. The results presented in the phase-space maps for GJ 832c indicate the least deviation of eccentricity from its nominal value, which is then used to determine its inclination regime relative to the star-outer planet plane. Also, the injected planet is found to display stable orbital configurations for at least one billion years. Then, the radial velocity curves based on the signature from the Keplerian motion are generated for the injected planets with masses 1M(circle plus) to 15M(circle plus) in order to estimate their semimajor axes and mass limits. The synthetic RV signal suggests that an additional planet of mass <= 15M(circle plus) with a dynamically stable configuration may be residing between 0.25 and 2.0 au from the star. We have provided an estimated number of RV observations for the additional planet that is required for further observational verification.

• 出版日期2017-8-20