A Note on the Onset of Helium Burning in Degenerate Cores

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Abstract
In a series of papers Schwarzschild et al. (1962, 1962 and 1964) have considered the onset of helium burning in partially degenerate cores, using the assumption that the degenerate part of the core is isothermal because electron conduction transports heat very efficiently. They therefore find that the helium flash begins at the centre, where the density is greatest. We shall show that if we include electron conduction both the temperature and the rate of helium burning may increase outwards from the centre in certain stars, depending on their zero-age composition, and we present some computational results supporting this, based on a simplified model. In particular, we show how the position of the point at which helium first burns can be estimated. It is suggested that the helium flash may be preceded by an explosion in a shell within the core, and in consequence the reaction products may float very rapidly to the surface.

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