=======

WL created their models for SNR evolution in a cloudy medium starting from the usual set of equations for hydrodynamics under the assumption of spherical symmetry but with added terms to account for the effects of cloud evaporation on the mass, momentum and energy in the remnant. Though they included a term for mass injection into the intercloud medium as a result of thermal conduction, as mentioned above, they did not explicitly include thermal conduction. For our numerical hydrodynamical calculations presented here we employ the code FLASH [@Fryxell_etal_2000; @Fryxell_etal_2010 <http://flash.uchicago.edu/site/flashcode/>] without any extra terms added to account for mass loss from clouds since they are unnecessary in multiple dimensions as long as the physics is correctly modeled. An essential aspect of the modeling is the inclusion of thermal conduction, which is accurately and efficiently included via the `Diffuse` module included in version 4.3 of FLASH. We discuss the details of our use of this module in the appendix. The initial conditions for our cloudy medium runs include an initial distribution of clouds in space with varying sizes. The cloud size distribution and density were not important for WL as long as the fundamental assumptions of their calculations were not 