PHOENIX is a state-of-the-art model atmosphere code used to
model a variety of astrophysical atmopsheres. The code is
maintained by a large international, collaboration of
astronomers who work on stars, planets, brown dwarfs, white
dwarfs, super novae, novae, giants, stellar winds, AGNs,
etc.
The basic features of PHOENIX are:
- solves the 1-D plane-parallel or spherically symmetric
radiative transfer equation
- includes irradiation by a nearby companion
- includes atomic, molecular, and condensate (liquid and
solid) opacities
- includes many non-LTE species
- includes a parameterized cloud model appropriate for
brown dwarfs and giant planets
- capable of computing wind models for O stars and novae
- and much much more
