Evolution of helium rich stars with hydrogen burning

Details Evolution of helium rich stars with hydrogen burning Evolution of helium rich stars with hydrogen burning

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975a%26a....45..335r&link_type=abstract

Astronomy and Astrophysics, vol. 45, no. 2, Dec. 1975, p. 335-341.

Astronomy and Astrophysics

Astrophysics

11

Helium, Hertzsprung-Russell Diagram, Hydrogen, Nuclear Fusion, Stellar Evolution, Astronomical Models, Stellar Luminosity, Stellar Mass, Stellar Structure

Scientific paper

Evolutionary tracks of stars with an initial chemical composition X 0.100, Y 0.8790, Z 0.021 are calculated for solar masses of 0.35, 0.66, 1.00, 2.00, and 5.00, and with X 0.302, Y 0.677, Z 0.021 for solar masses of 1.00, 3.00, and 5.00. The evolution is followed from hydrogen to helium burning, and to carbon burning when the occasion arises. The evolution data are presented and compared with normal Population I-stars. The helium rich stars show higher effective temperatures, much higher luminosities and therefore shorter time scales. They are situated in regions of the HR-diagram where observed helium stars are found.

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