On shallow convective envelopes

Details On shallow convective envelopes On shallow convective envelopes

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...201..183d&link_type=abstract

Astrophysical Journal, vol. 201, Oct. 1, 1975, pt. 1, p. 183-189.

Astronomy and Astrophysics

Astrophysics

5

Astronomical Models, Convection Currents, Convective Flow, Finite Difference Theory, Stellar Envelopes, Adiabatic Conditions, Computer Techniques, Mixing Length Flow Theory, Numerical Integration, Perturbation Theory, Pressure Effects, Stellar Atmospheres, Stellar Structure

Scientific paper

The finite difference method has been used to integrate the three-dimensional partial differential equations of mass, momentum, and energy conservation describing the convective motions of stellar envelopes. The method is applied specifically to a shallow convective envelope with extensive convective motion only in the second helium ionization zone. The size of the convective cells, the growth rate of convective motion, the pressure perturbations, and the effects of nonadiabaticity are discussed. A comparison is made with standard mixing length theory.

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