A deeper view of the CoRoT-9 planetary system. A small non-zero eccentricity for CoRoT-9b likely generated by planet-planet scattering
Journal
Date Issued
2017
Author(s)
•
Hébrard, G.
•
Raymond, S. N.
•
Bouchy, F.
•
Lecavelier des Etangs, A.
•
Bordé, P.
•
Aigrain, S.
•
Almenara, J. -M.
•
Alonso, R.
•
Cabrera, J.
•
Csizmadia, Sz.
•
Damiani, C.
•
Deeg, H. J.
•
Deleuil, M.
•
Díaz, R. F.
•
Erikson, A.
•
Fridlund, M.
•
Gandolfi, D.
•
Guenther, E.
•
Guillot, T.
•
Hatzes, A.
•
Izidoro, A.
•
Lovis, C.
•
Moutou, C.
•
Ollivier, M.
•
Pätzold, M.
•
Rauer, H.
•
Rouan, D.
•
Santerne, A.
•
Schneider, J.
Abstract
CoRoT-9b is one of the rare long-period (P = 95.3 days) transiting giant planets with a measured mass known to date. We present a new analysis of the CoRoT-9 system based on five years of radial-velocity (RV) monitoring with HARPS and three new space-based transits observed with CoRoT and Spitzer. Combining our new data with already published measurements we redetermine the CoRoT-9 system parameters and find good agreement with the published values. We uncover a higher significance for the small but non-zero eccentricity of CoRoT-9b () and find no evidence for additional planets in the system. We use simulations of planet-planet scattering to show that the eccentricity of CoRoT-9b may have been generated by an instability in which a 50 M⊕ planet was ejected from the system. This scattering would not have produced a spin-orbit misalignment, so we predict that the CoRoT-9b orbit should lie within a few degrees of the initial plane of the protoplanetary disk. As a consequence, any significant stellar obliquity would indicate that the disk was primordially tilted.
Volume
603
Start page
A43
Issn Identifier
0004-6361
Ads BibCode
2017A&A...603A..43B
Rights
open.access
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