Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ap%26ss.117...95e&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 117, no. 1, Dec. 1985, p. 95-109. Research supported by the Scientific and
Astronomy and Astrophysics
Astrophysics
6
Blue Stars, Main Sequence Stars, Stellar Evolution, Stellar Structure, Big Bang Cosmology, Helium, Hydrogen, Stellar Mass, Stellar Models
Scientific paper
Assuming the Big-Bang nucleosynthesis was responsible for the formation of helium, the evolution of first-generation intermediate-mass stars of 5, 7, and 9 solar masses with no metals have been studied from the threshold of stability through the stage of helium exhaustion in the cores of the stars. Hydrogen Main-Sequence positions are marked at effective temperatures higher than those of normal stars. The evolutionary tracks during the hydrogen-burning phase begin to be similar to those of normal stars when the CN-cycle reactions, which are controlled by the triple-alpha reactions, become operative for hydrogen depletion. Helium Main Sequence of Population III stars of intermediate mass occurs at the high effective temperature region of the H-R diagram, and stars stay as blue stars until the end of the core helium exhaustion phase. The total time elapsed is in the range of 3 x 10 to the 7th and 3 x 10 to the 8th yr. The stars with the initial masses of 5, 7, and 9 solar masses developed a moderately electron-degenerate, complete hydrogen-exhausted region with masses of 0.77, 1.06, and 1.42, respectively, in which the most abundant element is carbon.
Eryurt-Ezer Dilhan
Kiziloglu Nilgun
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