In this example we model an H II region with parameters corresponding to the first of the Lexington benchmarks (see appendix C). In this case we give only the prompted values. This illustrates the use of a blackbody spectrum, with temperature given in keV, and non-solar abundances.
unix > xstar xstar version 2.1 covering fraction (0.:1.) [1.] temperature (/10**4K) (0.:1.e4) [100.] 1. constant pressure switch (1=yes, 0=no) (0:1) [0] pressure (dyne/cm**2) (0.:1.) [0.03] density (cm**-3) (0.:1.e18) [1.E+12] 1.e+2 spectrum type?[pow] bbody radiation temperature or alpha?[-1.] 0.004 luminosity (/10**38 erg/s) (0.:1.e10) [1.] column density (cm**-2) (0.:1.e25) [1.E23] log(ionization parameter) (erg cm/s) (-10.:+10.) [2.] 5. hydrogen abundance (0.:100.) [1.] helium abundance (0.:100.) [1.] carbon abundance (0.:100.) [1.]0.6215 nitrogen abundance (0.:100.) [1.] 0.429 oxygen abundance (0.:100.) [1.] 0.445 neon abundance (0.:100.) [1.] 0.417 magnesium abundance (0.:100.) [1.] 0. silicon abundance (0.:100.) [1.] 0. sulfur abundance (0.:100.) [1.] 0.421 argon abundance (0.:100.) [1.] 0. calcium abundance (0.:100.) [1.] 0. iron abundance (0.:100.) [1.] 0. nickel abundance (0.:100.) [1.] 0. model name[xstar Default] H II region