Exoclimes_Conference_booklet1

OH, H2, CO, CO2, CH4, NH3, MgO, MgSiO3, Mg2SiO4, Al2O3, etc. We compare our results with
available polarimetric and photometric measurements for hot Jupiters.
Testing radiative transfer schemes for use in global circulation models of hot
Jupiters!
David Skålid!Amundsen — University of Exeter!
Several studies which have used adapted Global Circulation Models (GCMs) to interpret
observations of hot Jupiters have now been published. Almost all of these studies involve
simplified dynamical (e.g shallow water or primitive equations) and radiative transfer
schemes (temperature forcing, grey or band-averaged absorption coefficients). We are
adapting the UK Met Office GCM, the Unified Model, which solves the full 3D compressible
Euler equations and includes a frequency dependent radiative transfer scheme (invoking
the two-stream approximation and correlated-k method) for the study of hot Jupiters.
We will discuss the adaptation of the radiative transfer scheme and the tests we have
performed to verify its accuracy. By comparing to more accurate discrete-ordinate line-byline
calculations we will demonstrate that this scheme yields fairly accurate fluxes and
heating rates overall. In some cases, however, there are significant deviations, and we find
the use of band-averaged absorption coefficients to be very inaccurate. Lastly, I will
present some of the first results we have obtained after recoupling the dynamical core and
radiative transfer schemes.
An Open Source Python Thermochemical Equilibrium Abundances Code!
Jasmina Blecic — University of Central Florida
We present a Thermochemical Equilibrium Abundances code (TEA) that calculates the
equilibrium abundances of the molecular species present at a given temperature and
pressure in a planetary atmosphere. There are two approaches to calculating
thermochemical equilibrium: by using equilibrium constants and reaction rates or by
minimizing the free energy of the system. Although chemical equilibrium can be calculated
almost trivially for several reactions present in the system, as the number of reactions
increases, the number of equilibrium-constant relations becomes difficult to solve
simultaneously. An advantage of the free-energy-minimization method is that each
species present in the system can be treated independently, without specifying
complicated sets of reactions. Therefore, just a limited set of equations needs to be
solved. TEA is based on the Gibbs-free-energy minimization calculation, originally
developed by White et al. (1958) and Eriksson (1971). The code is written entirely in
Python and is available to the scientific community under an open-source license.
VSTAR Models of a Hot Jupiter
Kimberly Bott -- University of New South Wales
Past analysis of HD 189733b's atmosphere has been a cause for some debate, with
conflicting findings regarding polarized light, carbon dioxide and sodium abundances and
the presence of a high altitude haze. I will present our model of HD 189733b's atmosphere
using VSTAR (Versatile Software for Transfer of Atmospheric Radiation), a robust, line-byline,
multiple scattering radiative transfer solution in a modular program, utilitizing its own
chemical equilibrium model. Since the effective temperature of the planet is expected to be
approximately 1100K, newly available high-temperature spectral line lists were used. The
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