A criterion for the maximum extent of flash-driven convection

Statistics – Computation

Scientific paper

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Convective Flow, Helium, Stellar Structure, Hydrogen, Long Term Effects, Stellar Evolution, Stellar Luminosity, Stellar Models

Scientific paper

Numerical experiments using a model of a 3-solar-mass star are performed to determine the physical process which limits the extent of convection during a helium flash and which seems to prohibit the convection zone from reaching the hydrogen shell. It is proposed that the maximum extent of convection is achieved when the time for radiative diffusion from the outer edge of the convection zone to the radiative region just above the hydrogen shell is shorter than the growth time of the instability. It is also suggested that this criterion should lead to quenching of the flash, since the star can then respond rapidly to entropy fluctuations in the helium shell. Computations of shell flashes with artificially altered rates of hydrogen and helium burning are found to indicate that the proposed criterion is correct. It is noted that in one calculation, an extremely violent flash resulted in contact between the convection zone and the hydrogen shell, which is not excluded by the present criterion.

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