This version includes the following added features:
(i) Inclusion of all elements up to Z=30. The atomic data for the energy level
structure of ions with 3 or more electrons for many of these are scaled
hydrogenic and so the associated line emission must be treated with caution.
(ii) Inclusion of two new input parameters: the radius exponent (radexp) and the
number of continuum energy bind (ncn2). These are described in the chapter on
input to xstar. (iii) Inclusion of the radiation scattered in resonance
lines as a column in the output fits file xout_spect1.fits. This is provided
in the same units of specific luminosity as the other columns. (iv) Use
of a new algorithm for the multilevel calculation which is considerably faster
and requires less storage. Hence smaller values of critf (even 0) can
be accomodated for many problems. (v) The input parameter critf now
refers to the fractional ion abundance (i.e. relative to the parent element)
rather than the absolute (i.e. relative to H) ion abundance.
(vi) Minor changes have been made to some of the output formats in the
ascii file xout_step.lis. (vii) The atomic data for dielectronic recombination has
been changed to incorporate the results from Badnell and coworkers
(http://amdpp.phys.strath.ac.uk/tamoc/DATA/RR/) in place
of the rates from [Aldrovandi and Pequignot 1973] and [Arnaud and Raymond 1992].
This has quantitative effects on many of the results from xstar. Notable is
the effect on the ionization balance of iron for ionization parameters
in the range 0
2, where the m-shell ions dominate, and where
the new rates are greater than the previous ones by large factors.