Numerical simulations of stellar convective dynamos. I - The model and method

Details Numerical simulations of stellar convective dynamos. I - The model and method Numerical simulations of stellar convective dynamos. I - The model and method

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984jcoph..55..461g&link_type=abstract

Journal of Computational Physics (ISSN 0021-9991), vol. 55, Sept. 1984, p. 461-484. Sponsorship: Science and Engineering Researc

Statistics

Computation

234

Chebyshev Approximation, Computerized Simulation, Crank-Nicholson Method, Dynamo Theory, Stellar Magnetic Fields, Stellar Models, Boussinesq Approximation, Convection, Coriolis Effect, Differential Equations, Magnetohydrodynamics, Solar Rotation, Spherical Harmonics

Scientific paper

Many studies of stellar convection involve models which employ the Boussinesq approximation for which there is no basic density stratification. It is pointed out, however, that stellar convection zones have large density stratifications. The use of the Boussinesq approximation produces, therefore, serious limitation. The current investigation is concerned with a model which represents a multimode, nonlinear, dynamic dynamo within the anelastic approximation. The model includes the effects of rotation, spherical geometry, density stratification, and penetration into a subadiabatic region. It is hoped to obtain a better understanding of global convection and magnetic field generation in stars by analyzing, with good spatial and temporal resolution, the physics responsible for the considered phenomena. Attention is given to the stellar model, details regarding the numerical method, and preliminary solutions.

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