Thermal Instability in a Nuclear-Burning Shell of Stars

Details Thermal Instability in a Nuclear-Burning Shell of Stars Thermal Instability in a Nuclear-Burning Shell of Stars

Apr 1968

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1968pthph..39..957h&link_type=abstract

Progress of Theoretical Physics, Vol. 39, No. 4, pp. 957-984

Physics

18

Scientific paper

The criterion for instability that appears in a nuclear burning shell of stars and the evolution during the period of this instability are studied in general. It is shown without detailed numerical calculations that the temperature at the unstable shell increases until it reaches a certain maximum value, and afterward it decreases gradually. The maximum value of the temperature depends on the ratio of the radiation pressure to the total pressure of the nuclear burning shell at a stage when the instability begins. The evolution during the instability has been calculated in detail for four stellar configurations, including the stars with an unstable hydrogen-burning shell, an unstable helium-burning shell, an unstable carbon-burning shell and with an unstable hydrogen-burning shell which has been made by the accretion of a hydrogen-rich gas.

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