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We present Spitzer MIPS SED and IRS observations of 14 Galactic SupernovaRemnants previously identified in the GLIMPSE survey. We find evidence forSNR/molecular cloud interaction through detection of [OI] emission, ioniclines, and emission from molecular hydrogen. Through black-body fitting of theMIPS SEDs we find the large grains to be warm, 29-66 K. The dust emission ismodeled using the DUSTEM code and a three component dust model composed ofpopulations of big grains, very small grains, and polycyclic aromatichydrocarbons. We find the dust to be moderately heated, typically by 30-100times the interstellar radiation field. The source of the radiation is likelyhydrogen recombination, where the excitation of hydrogen occurred in the shockfront. The ratio of very small grains to big grains is found for most of themolecular interacting SNRs to be higher than that found in the plane of theMilky Way, typically by a factor of 2--3. We suggest that dust shattering isresponsible for the relative over-abundance of small grains, in agreement withprediction from dust destruction models. However, two of the SNRs are best fitwith a very low abundance of carbon grains to silicate grains and with a veryhigh radiation field. A likely reason for the low abundance of small carbongrains is sputtering. We find evidence for silicate emission at 20 $\mu$m intheir SEDs, indicating that they are young SNRs based on the strong radiationfield necessary to reproduce the observed SEDs.

Dust processing in Supernova Remnants: Spitzer MIPS SED and IRS Observations