http://arxiv.org/abs/1509.00659
Helium burning in the convective cores of horizontal branch and `red clump’ stars appears to involve a process of `ingestion’ of unburnt helium into the core, the physics of which has not been identified yet. I show here that a limiting factor controlling the growth is the buoyancy of helium entering the denser C+O core. It yields a growth rate which scales directly with the convective luminosity of the core, and agrees with constraints on core size from current asteroseismology.
H. Spruit
Thu, 3 Sep 15
29/58
Comments: Accepted for publication in A&A
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