Evolution of “51 Pegasus b-like” planets
Observatoire de la Côte d'Azur, Laboratoire Cassini, CNRS UMR 6529, 06304 Nice Cedex 4, France
2 University of Arizona, Department of Planetary Sciences and Lunar and Planetary Lab, Tucson, AZ 85721 USA e-mail: firstname.lastname@example.org
Corresponding author: T. Guillot, email@example.com
Accepted: 7 November 2001
About one-quarter of the extrasolar giant planets discovered so far have orbital distances smaller than 0.1 AU. These “51 Peg b-like” planets can now be directly characterized, as shown by the planet transiting in front the star HD 209458. We review the processes that affect their evolution. We apply our work to the case of HD 209458b, whose radius has been recently measured. We argue that its radius can be reproduced only when the deep atmosphere is assumed to be unrealistically hot. When using more realistic atmospheric temperatures, an energy source appears to be missing in order to explain HD 209458b's large size. The most likely source of energy available is not in the planet's spin or orbit, but in the intense radiation received from the parent star. We show that the radius of HD 209458b can be reproduced if a small fraction (~) of the stellar flux is transformed into kinetic energy in the planetary atmosphere and subsequently converted to thermal energy by dynamical processes at pressures of tens of bars.
Key words: stars: individual: 51 Peg, HD 209458 / planets and satellites: general / stars: planetary systems
© ESO, 2002