Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ap%26ss..79..265e&link_type=abstract
Astrophysics and Space Science, vol. 79, no. 2, Oct. 1981, p. 265-287. Research supported by the Scientific and Technical Resea
Astronomy and Astrophysics
Astrophysics
6
Astrophysics, Energy Sources, Stellar Evolution, Stellar Models, Burning Time, Helium, Hertzsprung-Russell Diagram, Hydrogen, Main Sequence Stars
Scientific paper
The theoretical evolution of a first-generation star of 3 solar masses after the core helium-exhaustion phase has been investigated. The star displays the character of a double shell burning model. Shell hydrogen-burning produces energy mostly by the p-p chain reaction. The CN-cycle reaction is only operating in the inner edge regions where a sufficient amount of carbon is formed by the 3-alpha-reactions. Hence, the shell burning time of the star is longer than that of normal stars, thus lengthening the total evolutionary lifetime of the first-generation stars. Prior to carbon-burning phase, the mass of the complete hydrogen-exhausted region is 1.14 solar masses and that of the complete helium-exhausted region is 0.83 solar mass. A carbon-oxygen core of about 0.87 solar mass has developed within the star in which the ratio of carbon to oxygen is about 0.85, but decreases down to a value of 0.50 near the boundary of the core.
No associations
LandOfFree
Advanced evolutionary phase of a first-generation star does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Advanced evolutionary phase of a first-generation star, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Advanced evolutionary phase of a first-generation star will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1468344