Abstract
Kinematical hydromagnetic theory is used to study the magnetic fields produced by the action of two prescribed, steady two-dimensional velocity fields on initially weak, large-scale magnetic fields. In both flows, the magnetic field becomes concentrated along certain vertical planes. In an effort to approximate one aspect of solar photospheric flows, it has been assumed that the fluid motions occupy only a lower half-space, so that a horizontal plane of zero mass flux separates a lower region in motion from an upper one at rest. The magnetic field lines cross this boundary, so that the concentration of the field by the flow is opposed by the tendency of the field above the flow to spread. The other factor opposing the field concentration is the diffusive effect of finite conductivity. Both the time-dependent and eventual steady state magnetic fields are considered for various (large) values of the magnetic Reynolds number.
Published Version
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