Atmosphere and orbital stability of exosolar planets orbiting gamma Cephei

Details Atmosphere and orbital stability of exosolar planets orbiting gamma Cephei Atmosphere and orbital stability of exosolar planets orbiting gamma Cephei

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....12443l&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #12443

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The recently discovered Jupiter-like planet (m sin i= 1.76 M_jup) in the binary system γ Cephei moves in a so-called S-type orbit around its host-star with a distance of about 2.15 AU. It is the first planet that have been found in a close binary and is from the dynamical point of view a very stable configuration. Numerical computations in the range between 0.5 AU and 1.9 AU from the host-star show possible habitable zones, where other planets might exist. In this context we increased the mass of the fictitious planet up to 90 Earth-masses, for which we have found stability at a distance around 1 AU. By including the possibility that a planet orbits inside a habitable zone of γ Cephei, we study the atmospheric loss and atmospheric stability for such bodies by estimating the exospheric temperature and energy limited EUV driven atmospheric escape fluxes driven by EUV, based on the assumption of equilibrium between EUV heat input and downward heat transport by conduction. Further, we also show that data obtained by space based observations, like those expected from COROT and EDDINGTON, in combination with ground-based observations and studies on comparative planetology of planets in the solar system can be used for theto study of the atmospheric evolution and habitability of exosolar planets.

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