Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....62....9w&link_type=abstract
Astronomy and Astrophysics, vol. 62, no. 1-2, Jan. 1978, p. 9-12.
Astronomy and Astrophysics
Astrophysics
2
Galactic Evolution, Stellar Evolution, Stellar Mass, Hydrogen, Populations, Stellar Envelopes, Stellar Models, Subdwarf Stars, Unsteady Flow
Scientific paper
The evolution and stability of low- and intermediate-mass models of very metal-poor stars are calculated. Evolutionary tracks are plotted to the point of minimum surface radius during core helium burning for 3.25- and 4.0-solar-mass models with (X, Z) of (0.739, 0.0001); a previous evolutionary sequence for a 2.5-solar-mass model is extended to the blue end of its blue loop. It is found that the models evolve significantly faster than Population I stars of the same mass and ignite core helium before reaching the red-giant branch. The 3.25- and 4.0-solar-mass models are shown to remain pulsationally stable in the fundamental radial mode during hydrogen burning, but a 0.55-solar-mass model is determined to be unstable to pulsation in the same mode during central hydrogen burning. The possibility is considered that an initial generation of stars of primordial composition (Population III) preceded the Population II.
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