A dynamical analysis of the 14 Her planetary system
K. Gozdziewski, C. Migaszewski, M. Konacki

TL;DR
This study uses dynamical analysis of radial velocity data to propose a stable configuration for the 14 Her planetary system, suggesting the presence of an additional giant planet within 13 AU with specific orbital characteristics.
Contribution
It provides the first dynamical constraints on the orbit of an additional planet in the 14 Her system, demonstrating long-term stability and possible orbital parameters.
Findings
Outer planet likely within 9-13 AU with moderate eccentricity
Stable configurations exist within a range of orbital parameters
Masses of planets depend on the system's inclination, approaching 10 Jupiter masses at lower inclinations
Abstract
Precision radial velocity (RV) measurements of the Sun-like dwarf 14 Herculis published by Naef et. al (2004), Butler et. al (2006) and Wittenmyer et al (2007) reveal a Jovian planet in a 1760 day orbit and a trend indicating the second distant object. On the grounds of dynamical considerations, we test a hypothesis that the trend can be explained by the presence of an additional giant planet. We derive dynamical limits to th orbital parameters of the putative outer Jovian companion in an orbit within ~13 AU. In this case, the mutual interactions between the Jovian planets are important for the long-term stability of the system. The best self-consistent and stable Newtonian fit to an edge-on configuration of Jovian planets has the outer planet in 9 AU orbit with a moderate eccentricity ~0.2 and confined to a zone spanned by the low-order mean motion resonances 5:1 and 6:1. This…
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