Volume 425, Number 1, October I 2004
|Page(s)||207 - 216|
|Section||Stellar structure and evolution|
|Published online||10 September 2004|
On the stability of thermonuclear shell sources in stars
Astronomical Institute, Utrecht University, Princetonplein 5, 3584 CC, Utrecht, The Netherlands e-mail: email@example.com
Accepted: 1 June 2004
We present a quantitative criterion for the thermal stability of thermonuclear shell sources. We find that the thermal stability of shell sources depends on exactly three factors: they are more stable when they are geometrically thicker, less degenerate and hotter. This confirms and unifies previously obtained results in terms of the geometry, temperature and density of the shell source, by a simplified but quantitative approach to the physics of shell nuclear burning. We present instability diagrams in the temperature-density plane for hydrogen and helium shell burning, which allow a simple evaluation of the stability conditions of such shell sources in stellar models. The performance of our stability criterion is demonstrated in various numerical models: in a 3 AGB star, in helium accreting CO white dwarfs, in a helium white dwarf which is covered by a thin hydrogen envelope, and in a 1.0 giant.
Key words: instabilities / nuclear reactions, nucleosynthesis, abundances / stars: interiors / stars: AGB and post-AGB / stars: white dwarfs
© ESO, 2004
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