Poster abstract details
Asteroseismic constraint on the mass of the planet orbiting the CoRoT Sun-like star HD 52265
L. Gizon, J. Ballot, C. Catala, T. Stahn, G. Vauclair, T. Appourchaux, M. Auvergne, A. Baglin, F. Baudin, O. Benomar, H. Bruntt, T.L. Campante, W.J. Chaplin, S. Deheuvels, N. Dolez, R.A. García, P. Gaulme, S. Mathur, E. Michel, B. Mosser, C. Régulo, I.W. Roxburgh, D. Salabert, R. Samadi, G.A. Verner, and the other members of the CoRoT Data Analysis Team
Abstract
The star HD52265 was chosen as a CoRoT prime target for asteroseismology because this Sun-like star hosts a planet, discovered in 2000 using radial velocity measurements (with a mass of 1.13 Jupiter mass divided by the sine of the angle between the line of sight and the normal to the orbital plane). Thanks to four months of CoRoT photometry, HD 52265 provides the best example of solar-like oscillations. The quality of the data is such that the angular velocity of the star and the inclination of the rotation axis can both be inferred from the rotationally-split modes of oscillation and their relative amplitudes. Assuming that the planet's orbital plane is normal to the stellar rotation axis, we find that the mass of the companion can be constrained with precision and that it is indeed a planet, not a brown dwarf.