On core mass-luminosity relations for shell helium burning stages of stellar evolution

Details On core mass-luminosity relations for shell helium burning stages of stellar evolution On core mass-luminosity relations for shell helium burning stages of stellar evolution

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...233..589h&link_type=abstract

Astrophysical Journal, Part 1, vol. 233, Oct. 15, 1979, p. 589-595.

Astronomy and Astrophysics

Astrophysics

16

Helium Hydrogen Atmospheres, Main Sequence Stars, Stellar Evolution, Stellar Luminosity, Stellar Mass, Graphs (Charts), Stellar Atmospheres, Stellar Models

Scientific paper

The evolution of a number of medium-mass (2, 3, 3.7, 4, 5, and 6 solar masses) stars is followed from the hydrogen main sequence to the stage of double shell burning. It is found that a core mass-luminosity relation similar to that obtained by Paczynski (1970) for the double-shell-burning stage exists for the stage where the helium-burning shell is advancing outward but has not yet reached the hydrogen-helium interface; i.e., just before the formation of the double shell structure. Reasons why the stellar luminosity does not depend on any of the parameters of the overlying envelope are considered.

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