The modelling of latitudinal gradients in the solar wind in the outer solar system

Details The modelling of latitudinal gradients in the solar wind in the outer solar system The modelling of latitudinal gradients in the solar wind in the outer solar system

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985asee.nasa.....n&link_type=abstract

In Alabama Univ. Res. Rept.: 1984 NASA/ASEE Summer Faculty Fellowship Program (NASA-CR-171317) 22p (SEE N85-22210 12-80)

Physics

Axisymmetric Flow, Meridional Flow, Radial Flow, Stellar Magnetic Fields, Stellar Winds, Latitude, Magnetic Flux, Radial Velocity

Scientific paper

A steady, axisymmetric, quasi-radial, global model is developed for thermally driven stellar winds with embedded magnetic fields. The asymptotic, linear results are presented for 0(1) latitudinal variations in the radial magnetic field, mass-loss rate, and radial velocity of the wind. The MHD equations are solved for the latitudinal dependence of the rotational velocity and magnetic field. They are driven by the meridional flows that develop naturally from internal magnetic stresses. Most flows open flux tubes in the stars equatorial plane, redistributing mass and magnetic flux as a function of stellar latitude. The plasma spins up to conserve angular momentum in fields and plasma.

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