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

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Fischera,  J.
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

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Tuffs,  R. J.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Völk,  H. J.
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

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Citation

Fischera, J., Tuffs, R. J., & Völk, H. J. (2002). Infrared emission towards SN 1987A, 11 years after outburst: Properties of the circumstellar dust. Astronomy & Astrophysics, 395(1), 189-200. Retrieved from http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2002A%26A..395.189F&db_key=AST&high=3fd59969ac20031.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0011-8278-4
Abstract
Detailed models are presented for the late epoch mid infrared (MIR) emission from collisionally heated grains in the shocked circumstellar gas around SN 1987A. Thermal dust emission from a region of moderate density interior to the thick inner ring seen with the Hubble Space Telescope (HST) is found to be a natural explanation for the MIR spectral energy distribution measured by ISOCAM. The MIR-spectrum can be reproduced by a mixture of silicate-iron or silicate-graphite grains or by a composition of pure graphite grains. A composition of pure iron grains on the other hand can be excluded and a pure silicate composition does not seem to be very likely. The dust-to-gas ratio in the interaction zone is similar to0.01%, an order of magnitude lower than estimates for dust abundances in the winds of red supergiant (RSG) stars in the LMC. This low dust abundance can be accounted for by a combination of evaporation through the UV-flash from the supernova outburst and subsequent sputtering in the shocked gas. For this explanation to hold, dust in the pre-supernova circumstellar medium (CSM) would have to have been predominantly composed of grains other than graphite, with a maximum size smaller than similar to0.1 mum.