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3D Models of Exoplanet Atmospheres

Published online by Cambridge University Press:  23 April 2012

Ian Dobbs-Dixon
Ian Dobbs-Dixon*
Affiliation:
Department of Astronomy, University of WashingtonBox 351580, Seattle, WA 98195Sagan Postdoctoral Fellow email: [email protected]
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Abstract

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Dynamical models of strongly irradiated gas-giant atmospheres exhibit a range of behavior, the nature of which depends on both the adopted parameters and the adopted numerical model. Discerning the correct choice of physical parameters and modeling philosophy can be difficult. Here, I present a series of wavelength-dependent transmission spectra for the giant planet HD209458b based on 3D radiative hydrodynamical models for a range of kinematic viscosities. While flow patterns and temperature distributions can vary significantly, disk-averaged phase curves mask much of this information. Transmission spectra, on the other hand, probe the day-night transition where advective contributions dominate and differences are often most pronounced. Transmission spectra illustrate noticeable changes, especially when comparing the differences between transmission spectra of eastern and western hemispheres, as might be seen during ingress and egress.

Keywords

hydrodynamicsradiative transfertechniques: spectroscopiceclipses
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 533 - 538
Copyright
Copyright © International Astronomical Union 2012

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