Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...133..264f&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 133, no. 2, April 1984, p. 264-284. Research supported by the Naturvetenskapli
Astronomy and Astrophysics
Astronomy
51
Compton Effect, Shock Waves, Stellar Envelopes, Supernovae, Ultraviolet Astronomy, X Ray Sources, Photoionization, Stellar Evolution, Stellar Luminosity, Stellar Spectra, Stellar Temperature, Stellar Winds
Scientific paper
The X-ray and UV emission from young Type II supernovae are discussed in relation to recent observations. There is now strong evidence that the supernova envelope expands out in the dense stellar wind of the supernova progenitor. This interaction results in one fast shock propagating into the stellar wind and one slow, propagating back into the dense stellar envelope. It is shown that during the first month these will cool rapidly, due to the strong radiation losses. The outer shock will emit the bulk of its energy as Comptonized EUV radiation, whereas the inner shock radiates mainly in X rays. The author concentrates on the physics of the UV shell and the reprocessing of the hard radiation from the shock wave into observable UV emission lines. Since both the total luminosity and spectral shape of the EUV and X-ray emission are crucial for the structure, these are first discussed. After this the author discusses the qualitative features of the UV shell and its time evolution using simplified analytical models. Exact comparison with the UV observations requires the solution of the coupled radiative transfer and statistical equations for different values of the important physical parameters; these calculations are described. The results of these and the sensitivity to the parameters used are then discussed and the main conclusions are summarized.
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