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

TL;DR

This study investigates the stability and potential existence of a sub-Earth mass planet between the known planets in the GJ 832 system using numerical simulations and radial velocity analysis.

Contribution

It provides a detailed phase-space analysis and stability assessment for a hypothetical planet in GJ 832, suggesting possible stable orbits and observational signatures.

Findings

A stable orbit for a planet up to 15 Earth masses exists between 0.25-2.0 AU.

The injected planet can remain stable for at least one billion years.

Radial velocity signals indicate potential detectability of such a planet with current methods.

Abstract

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. A special emphasis is given to the existence of stable orbits for a planet less than 15M$_\oplus$ which 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 displays 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$_\oplus$ to 15M$_\oplus$ in order to estimate their semimajor axes and mass-limit. The synthetic RV signal suggests that an additional planet of mass $\le$ 15M$_\oplus$ with dynamically stable configuration may be residing between 0.25 - 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.