The calibration of stellar convection theories

Details The calibration of stellar convection theories The calibration of stellar convection theories

Sep 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976mnras.176..589g&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 176, Sept. 1976, p. 589-607.

Astronomy and Astrophysics

Astronomy

88

Calibrating, Convective Heat Transfer, Stellar Models, Temperature Gradients, Adiabatic Conditions, Entropy, Gas Ionization, Luminous Intensity, Mixing Length Flow Theory, Prediction Analysis Techniques, Radiative Transfer, Stellar Evolution, Stellar Structure

Scientific paper

Any formula used to calculate the temperature gradient in a stellar convection zone must be calibrated, for example, by evolving 1-solar-mass stellar models to fit the present age, luminosity, and effective temperature of the sun. When this procedure is followed for various convection theories, including those of Opik (1950) and Boehm-Vitense (1958), the corresponding models become almost indistinguishable. In particular, they predict the same depth, around 150,000 km, for the solar convective zone.

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