A cooling flow model after Mushotzky & Szymkowiak (``Cooling Flows in Clusters and Galaxies" ed. Fabian, 1988). This one uses the MEKA model for the individual temperature components and differs from cflow in setting the emissivity function to be the inverse of the cooling time. The model assumes H0=50 and q0=0. Abundance ratios are set by the abund command.