Evolution of helium stars - A self-consistent determination of the boundary of a helium burning convective core

Details Evolution of helium stars - A self-consistent determination of the boundary of a helium burning convective core Evolution of helium stars - A self-consistent determination of the boundary of a helium burning convective core

Mar 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....47..231s&link_type=abstract

Astronomy and Astrophysics, vol. 47, no. 2, Mar. 1976, p. 231-241. Research supported by the Nederlandse Organisatie voor Zuive

Astronomy and Astrophysics

Astrophysics

19

Convective Flow, Core Flow, Helium, Iterative Solution, Stellar Evolution, Stellar Mass, Abundance, Linearization, Numerical Stability, Stellar Envelopes, Stellar Structure

Scientific paper

A generalization of the Henyey scheme is given that introduces the mass of the convective core and the density at the outer edge of the convective-core boundary as unknowns which have to be solved for simultaneously with the other unknowns. This boundary is determined in a physically self-consistent way for expanding as well as contracting cores, i.e., during the Henyey iterative cycle, its position becomes consistent with the overall physical structure of the star, including the run of the chemical abundances throughout the star. The evolution of helium stars (X = 0, Z = 0.03) is followed up to (nondegenerate) carbon ignition for 2.5, 3, 4, and 8 solar masses. The calculations show a rather large increase in mass of the convective cores during core helium burning. Evolutionary calculations for a 2-solar-mass helium star show that the critical mass for which carbon is ignited nondegenerately lies near 2 solar masses (corresponding to a C/O core of 0.99 solar mass). The 2-solar-mass helium star is the only one for which the radius strongly expands after core helium burning.

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