Testing a hypothesis of the \nu Octantis planetary system
Abstract
We investigate the orbital stability of a putative Jovian planet in a compact binary \nu Octantis reported by Ramm et al. We re-analyzed published radial velocity data in terms of self-consistent Newtonian model and we found stable best-fit solutions that obey observational constraints. They correspond to retrograde orbits, in accord with an earlier hypothesis of Eberle & Cuntz, with apsidal lines anti-aligned with the apses of the binary. The best-fit solutions are confined to tiny stable regions of the phase space. These regions have a structure of the Arnold web formed by overlapping low-order mean motion resonances and their sub-resonances. The presence of a real planet is still questionable, because its formation would be hindered by strong dynamical perturbations. Our numerical study makes use of a new computational Message Passing Interface (MPI) framework MECHANIC developed to run massive numerical experiments on CPU clusters.
Keywords
Cite
@article{arxiv.1205.1341,
title = {Testing a hypothesis of the \nu Octantis planetary system},
author = {Krzysztof Gozdziewski and Mariusz Slonina and Cezary Migaszewski and Anna Rozenkiewicz},
journal= {arXiv preprint arXiv:1205.1341},
year = {2014}
}
Comments
12 pages, 12 figures, accepted to Monthly Notices of the RAS