While it will generally be the responsibility of the individual investigator
to carry the analysis from the calibrated data to the physical characteristics
of the observed coronal gas, we anticipate providing standard versions of
commonly needed model codes. In particular, the UVCS project will provide
a documented code which predicts the intensities and line profiles of the
strongest lines (Ly
and the O VI, Mg X and Si XII doublets, and [Fe XII])
given the density, velocity, effective temperature and electron
temperature distributions along the line of sight. It will also provide a
code for inverting K-corona intensities to determine the electron column density.
Many of these codes were used
for previous programs, particularly the SAO/HAO rocket coronagraph program
and SPARTAN-201 ( e.g.,
Kohl { et al. 1980; Kohl and Withbroe 1982; Withbroe { et al. 1982,
1985, 1986; Noci { et al. 1987; Esser and Withbroe 1989;
Strachan 1990; Strachan { et al. 1993). They will be extended, updated and documented.