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Instabilities Driven in Young Supernova Remnants by Electron Heat Conduction

Published online by Cambridge University Press:  12 April 2016

R. Bedogni  and
A. D’Ercole
R. Bedogni*
Affiliation:
Osservatorio Astronomico di Bologna, Italy
A. D’Ercole
Affiliation:
Osservatorio Astronomico di Bologna, Italy
*
* Present address: Minnesota Supercomputer Institute, Minneapolis, USA

Extract

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Adiabatic models of supernova remnants (SNRs) show very large temperature gradients. The effect of thermal conduction on the Sedov solution was studied by a number of authors (Solinger et al., 1979; Cox and Edgar, 1983; Cowie, 1977).

The observations show, however, that young SNRs such as SN 1006 (Hesser and van den Bergh, 1981) and SN 1572 (Strom, Goss and Shaver, 1982) are in an intermediate state between free expansion and the Sedov phase. In these cases stellar matter cannot be neglected. Following Chevalier (1982), the freely expanding ejecta of a Type I SNR can be modeled in such a way that the inner 4/7 of the mass have constant density and the outer 3/7 have a ρ∝r−7 profile (the "ramp"). The interaction of the ejecta with the uniform circumstellar medium (CSM) gives rise to a pair of shocks. As long as the reverse shock is within the r−7 part of the density profile, the interaction region is described by a self-similar solution (Chevalier, 1982). Such a solution holds for an adiabatic single fluid; the temperature gradient, however, is so large that it may give rise to a quite high heat flux.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 101: Supernova Remnants and the Interstellar Medium , 1988 , pp. 43 - 46
Copyright
Copyright © Cambridge University Press 1988

References

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