2004A&A...427.1075P

Close-in extrasolar planets experience extreme tidal interactions with their host stars. This may lead to a reduction of the planetary radius and a spin-up of stellar rotation. Tidal interactions have been computed for a number of extrasolar planets in circular orbits within 0.06AU, namely for OGLE-TR-56b. We compare our range of the tidal dissipation value with two dissipation models from Sasselov (2003ApJ...596.1327S) and conclude that our choices are equivalent to these models. However, applied to the planet OGLE-TR-56b, we find in contrast to Sasselov (2003ApJ...596.1327S) that this planet will spiral-in toward the host star in a few billion years. We show that the average and maximum value of our range of dissipation are equivalent to the linear and quadratic dissipation models of Sasselov (2003ApJ...596.1327S). Due to limitations in the observational techniques, we do not see a possibility to distinguish between the two dissipation models as outlined by Sasselov (2003ApJ...596.1327S). OGLE-TR-56b may therefore not be well suited to serve as a test case for dissipation models. The probable existence of OGLE-TR-3b at 0.02AU and the discovery of OGLE-TR-113b at 0.023AU and OGLE-TR-132b at 0.03AU may also counter Sasselovs (2003ApJ...596.1327S) assumption of a pile-up stopping boundary at 0.04AU.