Spectra and Evolution of Exrasolar Planets

Details Spectra and Evolution of Exrasolar Planets Spectra and Evolution of Exrasolar Planets

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002sf2a.conf..573a&link_type=abstract

SF2A-2002: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 24-29, 2002, Eds.: F. Combes and D. Barret,

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We have used our general atmosphere code Phoenix to generate radiative equilibrium models of irradiated planets located near a dM6 and a G2 primary. The external radiation, as modeled also by Phoenix, was explicitly included in the solution of the radiative transfer equation. A cool (Teff = 500K) and a hot (Teff = 1000K) planet were modeled at various orbital separations from both the dM6 and the G2 primary. In all scenarios, we compared the effects of the irradiation in two cases: one where dust clouds form and remain suspended in the atmosphere and another where dust clouds form but settle out of the atmosphere. The atmospheric structure and emergent spectrum strongly depend on the presence or absence of dust clouds.

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