Santerne, A.; Schneider, J.; Rauer, H.; Rouan, D.; Pätzold, M.; Ollivier, M.; Lovis, C.; Moutou, C.; Hatzes, A.; Izidoro, A.; Guillot, T.; Gandolfi, D.; Guenther, E.; Fridlund, M.; Erikson, A.; Díaz, R. F.; Deeg, H. J.; Deleuil, M.; Damiani, C.; Csizmadia, Sz.; Cabrera, J.; Almenara, J.-M.; Alonso, R.; Aigrain, S.; Bordé, P.; Lecavelier des Etangs, A.; Raymond, S. N.; Bouchy, F.; Bonomo, A. S.; Hébrard, G.
Bibliographical reference
Astronomy and Astrophysics, Volume 603, id.A43, 11 pp.
Description
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.
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