2014/08/23 by Nikolaos Georgakarakos
Physics and Astronomy · #astro-ph.EP
paper · pdf · doi:10.1111/j.1365-2966.2005.09888.x
published as Monthly Notices of the Royal Astronomical Society, 2006, Volume 366, Issue 2, pp. 566-574 · This is a preprint of an article published in MNRAS in 2006. arXiv admin note: substantial text overlap with arXiv:0811.1146, arXiv:1408.5890, arXiv:1408.5462
arxiv created 2014/08/23 · arxiv updated 2014/08/28
In previous papers, we developed a technique for estimating the inner eccentricity in hierarchical triple systems, with the inner orbit being initially circular. We considered systems with well separated components and different initial setups (e.g. coplanar and non-coplanar orbits). However, the systems we examined had comparable masses. In the present paper, the validity of some of the formulae derived previously is tested by numerically integrating the full equations of motion for systems with smaller mass ratios (from 10-3 \hspace0.2cm to \hspace0.2cm 103, i.e. systems with Jupiter-sized bodies). There is also discussion about HD217107 and its planetary companions.