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The code below implements a simple stellar atmosphere model. It assumes a one-dimensional slab in hydrostatic and local thermodynamic equilibrium with gray rosseland mean opacities. Still, it can be useful as a quick diagnostic of a stellar atmosphere, or for checking the effects of a piece of local physics (e.g.,ionization).
sun's temperature structure |
sun's ionization structure |
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atmos.f plus six include files: atmos.dek implno.dek const.dek network.dek vector_eos.dek vector_kap.dek |
You'll need the eosfxt equation of state and the kapfxt opacity routine.