Patterns of convection in the evolution of massive stars

Details Patterns of convection in the evolution of massive stars Patterns of convection in the evolution of massive stars

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...199..166s&link_type=abstract

Astrophysical Journal, vol. 199, July 1, 1975, pt. 1, p. 166-172.

Astronomy and Astrophysics

Astrophysics

6

Convective Flow, Giant Stars, Nuclear Fusion, Stellar Evolution, Stellar Structure, Astronomical Models, Flow Geometry, Helium, Hydrogen, Stellar Envelopes, Stellar Mass

Scientific paper

Models for stars of 30 solar masses have been computed with an algorithm that assumes every point in the star to be radiative or fully convective. The ordinary Schwarzschild criterion is used, and semiconvection is not treated explicitly. In the resulting models, detached convective shells with superadiabatic inner boundaries appear instead of semiconvection. Since these boundaries travel inward by overshoot more rapidly than the core recedes, such detached convective zones would not persist in an actual star but would mix with the core. Inward of the detached convection, the hydrogen profile is insensitive to the treatment of convection if mass points are frequently redistributed in regions with a steep gradient of chemical composition. Treatment of overshoot will be necessary if radiative and convective zones are to represent semiconvection. During shell hydrogen burning, a convective region outside the nuclear burning shell and a semiconductive region farther outside will arise independent of overshoot. The N-14 + alpha reaction may precede triple-alpha ignition in the core in stars of 30 solar masses.

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