  X-ray grating observations have revealed great detail in the spectra of Novae
in the Super Soft Source (SSS) phase. Notable features in the SSS spectra are
blue-shifted absorption lines, P-Cygni line profiles, and the absence of strong
ionization edges, all of which are indicators of an expanding atmosphere.
  We present, and make publicly available, a set of 672 wind-type (WT)
synthetic spectra, obtained from the expanding NLTE SSS models introduced in
Van Rossum 2010 with the PHOENIX stellar atmosphere code. The set presented in
this paper is limited to solar abundances with the aim to focus on the basic
model parameters and their effect on the spectra, providing the basis upon
which abundance effects can be studied using a much bigger non-solar set in the
next paper in this series.
  We fit the WT spectra to the five grating spectra taken in the SSS phase of
nova V4743 Sgr 2003 as an example application of the WT models. Within the
limits of solar abundances we demonstrate that the following parameters are
constrained by the data (in order of decreasing accuracy): column density N_H,
bolometric luminosity L_bol, effective temperature T_eff, white dwarf radius R,
wind asymptotic velocity v_inf, and the mass-loss rate M_dot. The models are
also sensitive to the assumed white dwarf mass M_wd but the effect on the
spectra can largely be compensated by the other model parameters. The WT
spectra with solar abundances fit the data better than abundance optimized
hydro-static models.

High Energy Astrophysical Phenomena;Solar and Stellar Astrophysics