The role of inhomogeneous heat transport and anisotropic momentum exchange in the dynamics of stellar convection zones - Application to models of the sun's differential rotation

Details The role of inhomogeneous heat transport and anisotropic momentum exchange in the dynamics of stellar convection zones - Application to models of the sun's differential rotation The role of inhomogeneous heat transport and anisotropic momentum exchange in the dynamics of stellar convection zones - Application to models of the sun's differential rotation

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...156...22p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 156, no. 1-2, Feb. 1986, p. 22-32.

Physics

19

Heat Transfer, Solar Rotation, Stellar Physics, Anisotropy, Convection, Momentum Transfer, Stellar Models

Scientific paper

We propose mean field models of the Sun's differential rotation which fully include the mixing-length formalism, ionization and inertial terms due to rotation. We assume that differential rotation can be generated by two distinct mechanisms: (i) latitude-dependent heat transport, HT, modelled through the perturbation of the mixing-length; (ii) anisotropy of viscosity, AV, modelled through a special form of the viscous tensor. in the former case the perturbation parameter ɛ represents the strength of the rotation-convection interaction process, in the latter case ɛ represents the deviation from isotropy of the viscous momentum exchange. In both cases ɛ is determined by comparison of the calculations with the observed differential rotation. We test the response of the models to changes of the input parameters, as the depth of the convection zone, the kinematic viscosity, and the boundary conditions imposed at the lower edge of the convection zone. One of the most interesting results is that the AV mechanism is more effective than the HT mechanism, especially for deep convection zones. Furthermore, all the AV models require a small scale horizontal momentum exchange more effective than the vertical one to reproduce the observed differential rotation. The influence of rotation on the latitude- dependent energy transport depends strongly on the choice of the lower boundary conditions. When the lower boundary conditions are imposed in the radiative layers immediately below the convection zone, the models become independent of the choice of the lower boundary conditions. There is a general good agreement of the models with the observable quantities. Also, our internal rotation curve is compatible with that deduced from the analysis of the rotational splittings of 5 min oscillation modes.

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