Abstract. Convective motions in the photosphere and sub-photosphere may be responsible for generating the magnetic fields that support long-lived quiescent solar prominences. The connection is explored here by solving a Dirichlet problem on a semi-infinite strip where the base of the strip is the photosphere, and the strip extends into a current free corona. Even though the convection is simulated only by a one-dimensional potential prescribed at the photosphere it is found that both Kippenhahn-Schlüter and Kuperus-Raadu type fields are possible.
Abstract. The solar convection zone may be a mechanism for generating the magnetic fields in the corona that create and thermally insulate quiescent prominences. This connection is examined here by numerically solving a diffusion equation with convection (below the photosphere) matched to Laplace's equation (modeling the current free corona above the photosphere). The types of fields formed resemble both Kippenhahn-Schlüter and KuperusRaadu configurations with feet that drop into supergranule boundaries.
Using the first Born approximation, properties of the scattering phase shift are investigated for waves that are scattered by a schematic representation of a large-scale "stellar potential," i.e., one for which the star itself is viewed as the potential inducing a phase shift in an incoming wave. In particular, the phase shift properties are examined as functions of the relative wavenumber (c~) and the azimuthal wavenumber (g), high g-values being of interest in helioseismology.
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