Two-dimensional magnetohydrodynamic equilibria in the solar corona. II

Details Two-dimensional magnetohydrodynamic equilibria in the solar corona. II Two-dimensional magnetohydrodynamic equilibria in the solar corona. II

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992chjss..12..178l&link_type=abstract

Chinese Journal of Space Science (ISSN 0254-6124), vol. 12, no. 3, p. 178-184.

Computer Science

Sound

Plasma Equilibrium, Radial Flow, Solar Corona, Solar Wind Velocity, Flow Velocity, Gravitational Fields, Two Dimensional Flow

Scientific paper

Based on a combination of analytical and numerical methods, 2D MHD equilibria in the nonuniform gravitational field for the solar corona are discussed. The critical points are carefully treated. The large-scale magnetic structure of the corona, which include the closed-field region, the neutral sheet, and the open-field region are obtained. The closed-field region and the neutral sheet constitute a coronal streamer. At high and low latitudes, the radial flow velocity of plasma exceeds the local sound and local Alfvenic velocities beyond several solar radii. The velocity of solar wind reaches 400 km/s at 1 AU.

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