Physics
Scientific paper
Apr 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976rspsa.348..511j&link_type=abstract
Royal Society (London), Proceedings, Series A, vol. 348, no. 1655, Apr. 6, 1976, p. 511-523.
Physics
2
Flow Distribution, Magnetohydrodynamic Flow, Mass Ratios, Solar Wind, Two Fluid Models, Viscous Flow, Asymptotic Methods, Conductive Heat Transfer, Plasma Dynamics, Prandtl Number, Shock Layers, Solar Corona, Steady Flow
Scientific paper
The classical two-fluid equations for the solar-wind flow field are analyzed in the limit of small mass ratio using a model of a steady spherically symmetric flow of a fully ionized neutral electron-proton plasma plus the continuum representation of viscous effects. The plasma is considered to be compressible, viscous, and heat conducting, with a constant Prandtl number and a viscosity proportional to some power (greater than unity) of temperature. The equations are written in dimensionless form, and the method of matched asymptotic expansions is applied to construct a solution which starts from the base of the corona and extends out to a diffuse shock layer at a distance of about 100 light years. Four asymptotic regions are found which match completely and describe the flow field from the corona to the shock layer. Both the structure and detail of the solution are shown to parallel the results for the one-fluid theory. It is noted that the method gives rise to slightly doubtful results in the shock-layer region and to an unphysical solution beyond that region.
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