AdvisorHubbard, William B.
Committee ChairHubbard, William B.
MetadataShow full item record
PublisherThe University of Arizona.
RightsCopyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author.
AbstractWe present theoretical calculations for the evolution of highly-irradiated extrasolar giant planets. The value of the energy-limited escape rates are taken from Watson et al. (1981), Lammer et al. (2003) and Yelle (2004) which vary by two orders of magnitude. The lowest rate is from Watson et al., while the highest rate comes from Lammer et al., which predicts that all highly-irradiated planets are remnants of much larger planets. We find that for cases with lower mass loss rates, the tidal effects, such as the planet exceeding the Roche Lobe are more effective at removing mass than stellar radiation. We also compare our theories with observations to show observational evidence for mass loss.
Degree ProgramPlanetary Sciences