Double shell burning phase of intermediate mass population III stars

Details Double shell burning phase of intermediate mass population III stars Double shell burning phase of intermediate mass population III stars

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ap%26ss.147..343k&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 147, no. 2, Aug. 1988, p. 343-354.

Astronomy and Astrophysics

Astrophysics

2

Stellar Composition, Stellar Envelopes, Stellar Mass, Galactic Evolution, Interstellar Matter, Stellar Evolution

Scientific paper

The evolution of population III intermediate mass stars of 5, 7, and 9 solar masses has been studied after the core He-exhaustion phase. There are two energy producing regions within the stars; one is the H-burning shell and the other is the He-burning shell. During the double shell burning phase, the evolution does not proceed on the asymptotic giant branch and the second dredge-up does not appear; hence, there is no change in the surface composition of the stars. The final state of these stars is important in modeling galactic evolution.

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