Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...145..179l&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 145, no. 1, April 1985, p. 179-191. Sponsorship: Deutsche Forschungsgemeinscha
Astronomy and Astrophysics
Astrophysics
100
Convective Flow, Stellar Evolution, Stellar Mass, Stellar Models, Supermassive Stars, Turbulent Diffusion, Hertzsprung-Russell Diagram, Stellar Composition, Stellar Cores, Stellar Structure, Stellar Temperature, Time Dependence
Scientific paper
Evolutionary sequences at constant mass are presented for Pop I stars of 15 and 30 solar masses until the onset of core carbon burning. A time-dependent diffusion model based on a vibrational instability analysis is adopted in order to describe mixing of layers having a gradient of mean molecular weight (semiconvection). The fully-convective layers are determined according to the Ledoux criterion. For comparison, evolutionary sequences are also calculated for the same masses without assuming semiconvection but using the Schwarzschild criterion for convective instability. It is found that the vibrational instability does not establish the Schwarzschild-Haerm criterion for semiconvection during the fast phases of evolution, such as shell hydrogen burning. The modification of the chemical profile by semiconvection during this phase does strongly affect the evolutionary tracks in the H-R diagram during core helium burning. The results are discussed in comparison to earlier calculations of massive star evolution with and without inclusion of semiconvection.
El Eid Mounib F.
Fricke Klaus J.
Langer Norbert
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