Computer Science – Numerical Analysis
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...167..239x&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 167, Oct. 1986, p. 239-246.
Computer Science
Numerical Analysis
66
Convection, Stellar Evolution, Stellar Mass, Stellar Structure, Main Sequence Stars, Numerical Analysis, Schwarzschild Metric, Stellar Luminosity, Temperature Gradients
Scientific paper
The evolution of stars with masses 60, 30, 15, and 7 solar masses in the core H-burning phase is calculated using a complete nonlocal theory of convection. The convective overshooting is studied. The so-called semiconvection difficulties introduced by a local treatment of convection are removed automatically. The overshooting distance is about 4 sq rt c(1)c(2) times the pressure scale. The fractional mass of the overshooting zone increases as the mass of star decreases. The overshooting in a star with mass 7 solar masses is not essentially different from that for stars with masses larger than 9 solar masses; so the dividing ridge at 9 solar masses where semiconvection should appear is not verified. The temperature gradient in the penetrative convection zone is nearer the Schwarzschild criterion than Ledoux's. The theoretical evolutionary tracks run at higher luminosities and the main sequence band is wider than the traditional ones.
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