Physics
Scientific paper
Apr 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...315..571d&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 315, April 15, 1987, p. 571-579.
Physics
47
Emission Spectra, Infrared Spectra, Stellar Physics, Stellar Spectrophotometry, Supernova Remnants, Interstellar Gas, Line Spectra, Milky Way Galaxy, Stellar Evolution, Synchrotron Radiation
Scientific paper
Infrared emission from the Cas A supernova remnant has been detected in the IRAS survey from 12 to 100 μm, greatly in excess of the extrapolated radio synchrotron continuum. A fraction of the infrared flux probably comes from line emission in knots of shocked, optical-line emitting gas that are dispersed throughout the supernova cavity. Most of the infrared emission is due to thermal radiation by dust. The total in-band infrared luminosity is ≡3100 L_sun;, assuming a source distance of 2.8 kpc. This emission can be most simply interpreted as radiation from a mixture of silicate and graphite dust particles which have been swept up by the expanding supernova blast wave and collisionally heated by the X-ray emitting gas. Alternatively, or in addition to the swept-up dust, stellar or supernova condensates, heated by the reverse shock that travels through the ejecta, may give rise to or contribute to the emission.
Dinerstein Harriet L.
Dwek Eli
Gillett Fred C.
Hauser Michael G.
Rice Walter L.
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