associated with the Sedov phase. Possibly related is the observation that the plasma in many MMSNRs is observed to be overionized [e.g., @Kawasaki_etal_2002; @Yamaguchi_etal_2009], indicating a rapid cooling phase [@Uchida_etal_2012; @Moriya_2012].

Nearly half of the known MMSNRs are observed to produce gamma-ray emission, presumably indicating the interaction between protons accelerated by the SNR (or re-accelerated cosmic rays) and molecular cloud material or dense post-shock regions of radiative shocks [@Uchiyama_etal_2010; @Lee_etal_2015].

Even well before many of these observations that characterized MMSNRs in detail, @White+Long_1991 [hereafter WL] put forward an analytical model that attempted to explain remnants with centrally peaked X-ray emission. WL included terms in the fluid equations describing evolution in spherical symmetry of a SNR that allowed for a continual injection of mass and momentum as the result of cloud evaporation. In this way they aimed to describe the evolution and emission distribution generated when a SN explodes in a cloudy medium and where thermal conduction evaporates the clouds that have been enveloped by the blastwave. We note that there was no term in the equations accounting for the transfer of energy within the hot gas by thermal conduction. We will discuss the ramifications of this further below.

Methods {#sec:meth}
