Theoretical evolution of a hydrogen-helium star of 3M &sun; from the pre-Main Sequence to the core helium-exhaustion phase

Details Theoretical evolution of a hydrogen-helium star of 3M &sun; from the pre-Main Sequence to the core helium-exhaustion phase Theoretical evolution of a hydrogen-helium star of 3M &sun; from the pre-Main Sequence to the core helium-exhaustion phase

Sep 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972ap%26ss..18..226e&link_type=abstract

Astrophysics and Space Science, Volume 18, Issue 1, pp.226-245

Astronomy and Astrophysics

Astrophysics

13

Scientific paper

The evolution of a first-generation 3M &sun; star from the threshold of stability through the stage of helium exhaustion in the core has been studied. The total time elapsed is 4.174×108 yr and most of this time is spent in the blue-giant region of theH-R diagram. Hydrogen-burning near the Main Sequence occurs at a high central temperature via the proton-proton chain until the triplealpha reactions generate a small amount of C12 toward the end of the hydrogen-burning phase. The corresponding evolution time is longer than that of a normal population I star with the same mass. The ignition of the triple-alpha processes begins in a mildly degenerate, small convective core while the star still has a high surface temperature. Helium-burning in the core, coupled with hydrogenburning in the shell, occupies a period of about 1.8×107 yr, which is only one-third that of a normal star. The mass of the star interior to the hydrogen shell source has increased to a value of 0.50M &sun; near the end of core helium exhaustion. This region maintains an inhomogenous composition composed of helium, carbon and oxygen.

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