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Supernova generated shock waves are responsible for most of the destructionof dust grains in the interstellar medium (ISM). Calculations of the dustdestruction timescale have so far been carried out using plane parallel steadyshocks, however that approximation breaks down when the destruction timescalebecomes longer than that for the evolution of the supernova remnant (SNR)shock. In this paper we present new calculations of grain destruction inevolving, radiative SNRs. To facilitate comparison with the previous study byJones et al. (1996), we adopt the same dust properties as in that paper. Wefind that the efficiencies of grain destruction are most divergent from thosefor a steady shock when the thermal history of a shocked gas parcel in the SNRdiffers significantly from that behind a steady shock. This occurs in shockswith velocities >~ 200 km/s for which the remnant is just beginning to goradiative. Assuming SNRs evolve in a warm phase dominated ISM, we find dustdestruction timescales are increased by a factor of ~2 compared to those ofJones et al. (1996), who assumed a hot gas dominated ISM. Recent estimates ofsupernova rates and ISM mass lead to another factor of ~3 increase in thedestruction timescales, resulting in a silicate grain destruction timescale of~2-3 Gyr. These increases, while not able resolve the problem of the discrepanttimescales for silicate grain destruction and creation, are an important steptowards understanding the origin, and evolution of dust in the ISM.

Destruction of Interstellar Dust in Evolving Supernova Remnant Shock Waves