Highlights of Stellar Modeling with PHOENIX

PHOENIX (see Hauschildt & Baron, 1999, and references therein) is a generalized, stellar model atmosphere code for treating both static and moving atmospheres. The goal of PHOENIX is to be both as general as possible so that essentially all astrophysical objects can be modeled with a single code, and to make as few approximations as possible. Approximations are inevitable (particularly in atomic data where laboratory values for most quantities are unknown); however, the agreement of synthetic spectra with observations across a broad class of astrophysical objects is a very good consistency check. We have modeled Planets/BDs (Barman et al., 2002; Allard et al., 2001; Schweitzer et al., 2001, 2002), Cool Stars (Hauschildt et al., 1999; Hauschildt et al., 1999), Hot Stars (βCMa, ǫCMa, Deneb Aufdenberg et al., 1998, 1999, 2002), α-Lyra, Novae (Hauschildt et al., 1997b; Schwarz et al., 1997), and all types of superovae (SNe Ia, Ib/c, IIP, IIb Baron et al., 1995; Lentz et al., 2001a; Baron et al., 1999; Mitchell et al., 2002).