Magneto-convection in sunspot penumbrae

Details Magneto-convection in sunspot penumbrae Magneto-convection in sunspot penumbrae

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..151...29t&link_type=abstract

Solar Physics, vol. 151, no. 1, p. 29-40

Astronomy and Astrophysics

Astronomy

1

Landau-Ginzburg Equations, Magnetic Diffusion, Solar Convection (Astronomy), Sunspots, Chandrasekhar Equation, Magnetic Disturbances, Nonlinear Equations, Penumbras, Prandtl Number, Solar Magnetic Field, Thermal Diffusion

Scientific paper

Finite amplitude convection in the presence of a horizontal magnetic field has been investigated in a region where thermal diffusivity (kappa) is less than magnetic diffusivity (eta) and when kappa/eta is greater than 1, Q is less than or equal to Qc, where Qc = ((1 + sigma1) (pi2 + qc2)2)/(qc2(sigma2 - sigma1)), Q is the Chandrasekhar number, sigma1 the Prandtl number, sigma2 the magnetic PrandH number, and qc the critical wave number at the onset of stationary convection. We have derived a nonlinear time-dependent Landau-Ginzburg equation near the onset of supercritical stationary convection and a nonlinear, second-order equation at the Takens-Bogdanov bifurcation. We have obtained steady-state solutions of these equations, which describe the nonlinear behavior near the onset of stationary convection.

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