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Shell Flashes*

Published online by Cambridge University Press:  30 March 2016

I.-Juliana Sackmann
I.-Juliana Sackmann*
Affiliation:
W. K. Kellogg Radiation Laboratory, California Institute of Technology, Pasadena, California 91125, USA

Extract

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Shell flashes will be discussed here with regard to three different stages of evolution: 1. normal stars, 2. white dwarfs accreting H-rich matter and 3. neutron stars accreting matter.

A shell flash Is a thermal instability, a nuclear run-away process, occurring in any nuclear burning shell, as long as It is sufficiently thin in geometrical extent and sufficiently thick for a high enough heat capacity. (in contrast to the off-center helium shell flash, another kind of shell flash which occurs for degenerate matter, the shell flash discussed here does take place for an Ideal gas including radiation pressure and does not require degeneracy.) The first shell flash discovered was the helium shell flash, about 15 years ago, by Schwarzschild and Härm (1965); Hayashi, Hoshi, and Suglmoto (1965); and Weigert (1965, 1966).

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 445 - 448
Copyright
Copyright © Cambridge University Press 1980

Footnotes

*

Work supported in part by the National Science Foundation [PHY76-83685].

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