Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...108..118l&link_type=abstract
Astronomy and Astrophysics, vol. 108, no. 1, Apr. 1982, p. 118-126.
Astronomy and Astrophysics
Astrophysics
11
B Stars, Helium, Mass To Light Ratios, Stellar Evolution, Stellar Models, Cores, Hertzsprung-Russell Diagram
Scientific paper
Numerical calculations are carried out for the evolution of a 1-solar-mass helium star with initial chemical composition (Y equals 0.979, z equals 0.021) from the helium zero-age main sequence to the phase at which it is past its maximum radius. The results are found to be consistent with those of previous studies. During the greater part of the helium shell burning phase, the star moves nearly horizontally toward the right in the HR diagram and achieves large radii. A convective envelope appears when the core mass reaches approximately 0.7 solar mass. The star then increases its luminosity much more rapidly and moves up along a red giant branch. Throughout the subsequent evolution, the nuclear burning shell is extremely close to the base of the convective envelope, but the two regions never overlap. It is noted that the very thin helium burning shell is always thermally stable and that no nonnegligible carbon burning is expected to occur. At the end of the computation, the star is moving toward the left in the HR diagram; it will gradually evolve into the white dwarf stage.
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