Volume 581, September 2015
|Number of page(s)||14|
|Section||Planets and planetary systems|
|Published online||22 September 2015|
Detectability of quasi-circular co-orbital planets. Application to the radial velocity technique
ASD, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC,
77 Av. Denfert-Rochereau,
2 CIDMA, Departamento de Física, Universidade de Aveiro, Campus de Santiago, 3810-193 Aveiro, Portugal
Received: 24 March 2015
Accepted: 8 June 2015
Several celestial bodies in co-orbital configurations exist in the solar system. However, co-orbital exoplanets have not yet been discovered. This lack may result from a degeneracy between the signal induced by co-orbital planets and other orbital configurations. Here we determine a criterion for the detectability of quasi-circular co-orbital planets and develop a demodulation method to bring out their signature from the observational data. We show that the precision required to identify a pair of co-orbital planets depends only on the libration amplitude and on the planet’s mass ratio. We apply our method to synthetic radial velocity data, and show that for tadpole orbits we are able to determine the inclination of the system to the line of sight. Our method is also valid for planets detected through the transit and astrometry techniques.
Key words: planets and satellites: detection / planets and satellites: dynamical evolution and stability / celestial mechanics
© ESO, 2015
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