The initial Uranus model will be provided by my advisor Mark Marley.
His work is the first attempt at a self-consistent
radiative-convective model for the atmosphere since that of Appleby in
1986. His is also the first to use Voyager data as boundary
conditions. The model is based upon one derived for the atmosphere of
Titan (McKay 1989). There are 42 plane-parallel layers spaced equally
in log P from 2.5 
bars to 20 bars. In its present state the
model is essentially one-dimensional, but I will expand it into
greater dimension by adding a meridional component and taking
center-to-limb variations into account.
Calculations take place in the thermal infrared over 56
spectral intervals in the thermal IR between 5.7 
and 0.33
and 36 intervals in the reflected solar spectrum from 0.275
to 4.22 
. These bandpasses will be modified to meet those of the
filters use in the observational phase of the project. An atmospheric
model is allowed to relax to radiative equilibrium until the net flux
across each layer is zero. Layers with lapse rates greater than the
adiabatic condition are deemed to be convective. The equation of
radiative transfer is then solved for in each band until radiative
equilibrium is reached.