In this example we model a quasar broad line cloud. In this case we give only the prompted values. This illustrates the use of constant pressure and a power law spectrum, with spectral index input in energy units.
unix > xstar xstar version 2.2 covering fraction (0.:1.) [1.] 0. temperature (/10**4K) (0.:1.e4) [100.] 1. constant pressure switch (1=yes, 0=no) (0:1) [0] 1 pressure (dyne/cm**2) (0.:1.) [0.03] density (cm**-3) (0.:1.e18) [1.E+12] 1.e+10 spectrum type?[pow] pow radiation temperature or alpha?[-1.] -0.9 luminosity (/10**38 erg/s) (0.:1.e10) [1.] 1.e+8 column density (cm**-2) (0.:1.e25) [1.E23] log(ionization parameter) (erg cm/s) (-10.:+10.) [2.] 0.2 hydrogen abundance (0.:100.) [1.] helium abundance (0.:100.) [1.] carbon abundance (0.:100.) [1.] nitrogen abundance (0.:100.) [1.] oxygen abundance (0.:100.) [1.] neon abundance (0.:100.) [1.] magnesium abundance (0.:100.) [1.] silicon abundance (0.:100.) [1.] sulfur abundance (0.:100.) [1.] argon abundance (0.:100.) [1.] calcium abundance (0.:100.) [1.] iron abundance (0.:100.) [1.] nickel abundance (0.:100.) [1.] model name[xstar Default] quasar BLR cloud