Further adventures of a thermally pulsing star

Details Further adventures of a thermally pulsing star Further adventures of a thermally pulsing star

Aug 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...208..165i&link_type=abstract

Astrophysical Journal, vol. 208, Aug. 15, 1976, pt. 1, p. 165-176.

Astronomy and Astrophysics

Astrophysics

161

Astrophysics, Carbon Stars, Stellar Models, Stellar Temperature, Variable Stars, Abundance, Chemical Composition, Convection, Nuclear Fusion, Oscillations, Stellar Mass, Thermal Instability

Scientific paper

Eight additional thermal pulses are calculated for a 7-solar-mass model star with a carbon-oxygen core of 0.95 to 0.096 solar mass. The successive increase in maximum helium burning luminosity from the 10th to the 18th pulse is calculated, along with the corresponding increase in the temperature at the base of the convective shell and in the amount of matter containing fresh carbon that is dredged up by the convective envelope. The mass of carbon-rich matter dredged up near the end of the 18th pulse is found to be more than one third of the mass through which the hydrogen-burning shell has advanced during the preceding interpulse phase. It is shown that failure of the outer edge of the convective shell to reach the hydrogen-helium interface may be attributed to an 'entropy barrier' set up through this interface during the interpulse phase and that radiation pressure is the dominant contributor to the magnitude of this barrier. Similarly, the dredging-up phenomenon can be interpreted in terms of widely different rates of entropy change on either side of the hydrogen-helium interface

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