Gravonuclear Instabilities in Post-Horizontal-Branch Stars
Allen V. Sweigart (NASA/GSFC), John C. Lattanzio, James P. Gray, (Monash Univ.), Christopher A. Tout (Cambridge)

TL;DR
This paper examines the conditions under which gravonuclear instabilities occur in post-horizontal-branch stars, revealing that their appearance depends on the method used to suppress breathing pulses during stellar evolution modeling.
Contribution
It demonstrates that gravonuclear instabilities are artifacts of specific suppression techniques for breathing pulses, not intrinsic stellar phenomena.
Findings
Instabilities depend on how breathing pulses are suppressed.
Suppression method affects helium profile and shell stability.
Instabilities vanish when the helium shell broadens into an S-shape.
Abstract
We investigate the gravonuclear instabilities reported by Bono et al. (1997a,b) during the onset of helium-shell burning at the end of the horizontal-branch (HB) phase. These instabilities are characterized by relaxation oscillations within the helium shell which lead to loops in the evolutionary tracks. We find the occurrence of these instabilities depends critically on how the breathing pulses are suppressed near the end of the HB phase. If they are suppressed by omitting the gravitational energy term in the stellar structure equations, then the helium profile within the core at the end of the HB phase will contain a broad region of varying helium abundance. The helium-burning shell which forms in this region is too thick to be unstable, and gravonuclear instabilities do not occur. If, on the other hand, the breathing pulses are suppressed by prohibiting any increase in the central…
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Taxonomy
TopicsStellar, planetary, and galactic studies · Astrophysics and Star Formation Studies · Astronomy and Astrophysical Research
