A cooling flow model after Mushotzky & Szymkowiak (``Cooling Flows in Clusters
and Galaxies," ed. Fabian, 1988). An index of zero for the power-law emissivity
function corresponds to emission measure weighted by the inverse of the cooling
time at that temperature. The model assumes 
and 
. The
abundance ratios are set by the abund command.
par1 = index for power-law emissivity functionpar2 = low temperature (keV)
par3 = high temperature (keV)
par4 = abundance relative Solar
par5 = redshift
K = Mass accretion rate (solar mass/yr)