Anelastic Planetary Magnetohydrodynamics
A self-consistent anelastic planetary/satellite MHD system is optimally scaled. This scaling identifies key properties of MHD generators. Those are primarily located in thin (∼ r/R n ) buoyancy layers at the liquid core boundary. Here n = 1/3 at the onset of convection, n = 1/2 for the developed magneto-convection and R, which is defined via the preliminary Reference State of the planet/satellite, is about the ‘turbulent’ Reynolds or/and magnetic Reynolds number. Simple diffusion and heat equations together with non-inertia state for magnetic and velocity equations are proposed in order to solve the real 3D MHD problems in planet or satellite. Boussinesq and anelastic approaches are compared.
KeywordsRayleigh Number Outer Core Magnetic Reynolds Number Rigid Core Ekman Number
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- 1.Anufriev, A.P. and Cupal, I. (2001) Characteristic amplitudes in the solution of anelastic geodynamo model, Phys. Earth Planet. Inter., in printGoogle Scholar
- 4.Starchenko, S.V. (1999) Supercritical convection associated with ultra fast MHD rotation, JETP (Zh. Eksp. Teor. Fiz.), Vol. 115 (5), pp. 1708–1720Google Scholar