Convective shells and the core He-burning phase of massive stars

Details Convective shells and the core He-burning phase of massive stars Convective shells and the core He-burning phase of massive stars

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978ap%26ss..56..431c&link_type=abstract

Astrophysics and Space Science, vol. 56, no. 2, July 1978, p. 431-438. Research supported by the Consiglio Nazionale delle Rice

Astronomy and Astrophysics

Astrophysics

3

Convective Heat Transfer, Hertzsprung-Russell Diagram, Stellar Evolution, Helium, Main Sequence Stars, Stellar Mass

Scientific paper

In this paper we briefly discuss the effect of complete homogenization in the intermediate unstable layers of massive stars on the effective temperature of the core He-burning models. To this end, a 20 M0 star of Population I chemical composition (X = 0.700, Z = 0.020) has been allowed to evolve from the Main Sequence into the core He-exhaustion stage without taking into account semiconvective mixing. The results show that the models are systematically bluer than those computed with the same physical parameters but with the inclusion of semiconvection

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