Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...244..678d&link_type=abstract
Astrophysical Journal, Part 1, vol. 244, Mar. 1, 1981, p. 678-694.
Astronomy and Astrophysics
Astrophysics
12
Convective Flow, Free Convection, Solar Atmosphere, Solar Rotation, Stellar Models, Angular Momentum, Angular Velocity, Centrifugal Force, Energy Dissipation, Perturbation Theory, Poisson Equation, Radiative Transfer, Stellar Envelopes, Transport Properties
Scientific paper
Numerical solutions are evaluated of the equations governing the large-scale motions of rotating stellar convection zones, as derived by Durney (1976) and Spruit (1977) (DS). With reference to the solar convection zone, these equations were solved by a perturbation method with the uniformly rotating convection zone as the unperturbed state (approximated by a polytrope). The calculations suggest that (1) large pole-equator differences in flux in the lower part of the convection zone are entirely compatible with negligible pole-equator differences in flux at the surface; (2) in realistic models of the rotating solar convection zone the energy carried by radiation should be included; and (3) in the lower part of the convection zone the solar convection velocities could differ substantially from those evaluated in the absence of rotation.
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