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Detailed models are presented for the late epoch mid infrared (MIR) emissionfrom collisionally heated grains in the shocked circumstellar gas around SN1987A. Thermal dust emission from a region of moderate density interior to thethick inner ring seen with the Hubble Space Telescope (HST) is found to be anatural explanation for the MIR spectral energy distribution measured byISOCAM. The MIR-spectrum can be reproduced by a mixture of silicate-iron orsilicate-graphite grains or by a composition of pure graphite grains. Acomposition of pure iron grains on the other hand can be excluded and a puresilicate composition does not seem to be very likely. The dust-to-gas ratio inthe interaction zone is ~0.01%, an order of magnitude lower than estimates fordust abundances in the winds of red supergiant (RSG) stars in the LMC. This lowdust abundance can be accounted for by a combination of evaporation through theUV-flash from the supernova outburst and subsequent sputtering in the shockedgas. For this explanation to hold, dust in the pre-supernova circumstellarmedium (CSM) would have to have been predominantly composed of grains otherthan graphite, with a maximum size smaller than ~0.1 microns

Infrared emission towards SN 1987A, 11 years after outburst: Properties of the circumstellar dust