Non-spherical flow of matter in the solar wind

Details Non-spherical flow of matter in the solar wind Non-spherical flow of matter in the solar wind

Dec 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ang....32..373s&link_type=abstract

Annales de Geophysique, vol. 32, Oct.-Dec. 1976, p. 373-380.

Physics

Axisymmetric Flow, Magnetohydrodynamic Flow, Solar Flux, Solar Wind, Electron Gas, Hydrodynamic Equations, Radial Flow, Solar Electrons, Solar Protons, Solar Rotation, Steady Flow

Scientific paper

Deflections of solar wind flux from the radial direction are studied in a three-dimensional case. Hydrodynamic equations with magnetic field are solved by the perturbation method assuming flow stationary and axially symmetrical. Two polytropic formulae were used instead of the energy equation, one for electron gas and one for proton gas in the solar wind. The influence of the sun's rotation on the flow, mainly in a meridional direction is studied. When the azimuthal and meridional velocities are of the same order the flows in these directions are independent and the influence of rotation on the flow negligible. Significant coupling between azimuthal and meridional motions for different boundary conditions on the sun is analyzed. A method of computing the meridional flow for arbitrary differentially but slowly rotating stars is given.

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