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The Evolution of Young Supernova Remnants

Published online by Cambridge University Press:  04 August 2017

A. C. Fabian ,
W. Brinkmann  and
G. C. Stewart
A. C. Fabian
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 OHA, UK
W. Brinkmann
Affiliation:
Max Planck Institut für Extraterrestrische Astrophysik, 8046 Garching bei München, F.D.R.
G. C. Stewart
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 OHA, UK

Extract

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Einstein X-ray observations of the young supernova remnants Cassiopeia A (Murray et al. 1980) and Tycho (Seward, Gorenstein and Tucker 1982) indicate that the swept-up mass does not much exceed that of the observed ejecta. The initial density distribution of the ejecta and surrounding material is then important in determining the X-ray structure and evolution. Some aspects of this behaviour have been dealt with in previous numerical (e.g. Gull 1973; Itoh 1977; Jones, Smith and Straka 1981) and analytical (e.g. Chevalier 1982a,b) studies. We present here results obtained from numerical models covering a wider range of initial conditions. In particular, we consider the effect of a constant stellar wind from the progenitor star on the expansion of the remnant. We have previously suggested that variable mass loss from SN1006 may explain its warm filled interior (Fabian, Stewart and Brinkmann 1982).

Type
I. Young Supernova Remnants
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 119 - 124
Copyright
Copyright © Reidel 1983 

References

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