Detection of co-orbital planets by combining transit and radial-velocity measurements
Publisher DOI
Abstract
Co-orbital planets have not yet been discovered, although they constitute a frequent by-product of planetary formation and evolution models. This lack may be due to observational biases, since the main detection methods are unable to spot co-orbital companions when they are small or near the Lagrangian equilibrium points. However, for a system with one known transiting planet (with mass m1), we can detect a co-orbital companion (with mass m2) by combining the time of mid-transit with the radial-velocity data of the star. Here, we propose a simple method that allows the detection of co-orbital companions, valid for eccentric orbits, that relies on a single parameter α, which is proportional to the mass ratio m2/m1. Therefore, when α is statistically different from zero, we have a strong candidate to harbour a co-orbital companion. We also discuss the relevance of false positives generated by different planetary configurations.
Date Issued
2017-03
Publication Type
Article
Language(s)
en
Author(s)
Robutel, P. | |
Correia, A. C. M. | |
Lillo-Box, J. |
Journal
Astronomy & Astrophysics
Publisher
EDP Sciences
ISSN
0004-6361
1432-0746
Access(Rights)
restricted