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A deeper view of the CoRoT-9 planetary system A small non-zero eccentricity for CoRoT-9b likely generated by planet-planet scattering

A. S. Bonomo ; G. Hebrard ; S. N. Raymond ; F. Bouchy ; A. L. des Etangs ; P. Borde ; S. Aigrain ; J. M. Almenara ; R. Alonso ; J. Cabrera ; S. Csizmadia ; C. Damiani ; H. J. Deeg ; M. Deleuil ; R. F. Diaz ; A. Erikson ; Malcolm Fridlund (Institutionen för rymd-, geo- och miljövetenskap, Onsala rymdobservatorium) ; D. Gandolfi ; E. Guenther ; T. Guillot ; A. Hatzes ; A. Izidoro ; C. Lovis ; C. Moutou ; M. Ollivier ; M. Patzold ; H. Rauer ; D. Rouan ; A. Santerne ; J. Schneider
Astronomy & Astrophysics (1432-0746). Vol. 603 (2017), p. A43.
[Artikel, refereegranskad vetenskaplig]

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 (e = 0 : 133(-0.037)(+0.042)) 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 similar to 50 M-circle plus 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.

Nyckelord: planetary systems, techniques: radial velocities, techniques: photometric, stars: individual: CoRoT-9, Spin-Orbit Misalignments, Earth-Like Planets, Gas Giant Planets, Warm, Jupiters, Hot Jupiters, Super-Earths, Harps-N, Dynamical Instabilities, Terrestrial Planets, Sophie Velocimetry



Denna post skapades 2017-09-06. Senast ändrad 2017-09-14.
CPL Pubid: 251702

 

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