Low-mass evolution - Zero-age main sequence to asymptotic giant branch

Details Low-mass evolution - Zero-age main sequence to asymptotic giant branch Low-mass evolution - Zero-age main sequence to asymptotic giant branch

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...251..639d&link_type=abstract

Astrophysical Journal, Part 1, vol. 251, Dec. 15, 1981, p. 639-653. Research supported by the U.S. Department of Energy

Astronomy and Astrophysics

Astrophysics

22

Asymptotic Giant Branch Stars, Giant Stars, Horizontal Branch Stars, M Stars, Main Sequence Stars, Stellar Evolution, Stellar Mass, Asymptotic Methods, Hertzsprung-Russell Diagram, Nuclear Fusion, Red Giant Stars, Stellar Envelopes, Stellar Models

Scientific paper

A description is given of the hydrostatic evolution of a 0.6 solar mass stellar model from the zero-age main sequence to the asymptotic giant branch. A stability analysis for core and shell flashes is conducted, taking into account aspects of hydrostatic readjustment and the thermal response. Attention is also given to the core flash, the evolution to the horizontal branch, questions of horizontal branch evolution, and the asymptotic giant branch evolution. Since the red giant evolution reported is done without hydrogen shell shifting techniques, it may serve as a comparison case for those using them. Proper hydrogen shell structure can be verified with the aid of a presented graph which shows the variation of the hydrogen-burning shell structure with core mass. The hydrostatic decoupling of the core and envelope is seen to arise from the steep pressure decline in the region of the hydrogen shell.

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