On the continuum theory of the one-fluid solar wind for small Prandtl number

Details On the continuum theory of the one-fluid solar wind for small Prandtl number On the continuum theory of the one-fluid solar wind for small Prandtl number

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976rspsa.348..129j&link_type=abstract

Royal Society (London), Proceedings, Series A, vol. 348, no. 1652, Feb. 10, 1976, p. 129-142.

Astronomy and Astrophysics

Astrophysics

Continuum Flow, Gas Expansion, Gravitational Effects, Magnetohydrodynamic Flow, Prandtl Number, Solar Wind, Astrophysics, Asymptotic Methods, Compressible Fluids, Flow Distribution, Flow Theory, Subsonic Flow, Supersonic Flow, Thermal Conductivity, Viscous Fluids

Scientific paper

The continuum theory for a single-species gas expanding into a vacuum (or near vacuum) is considered. The gas is under the influence of a gravitational field centered on the sun. For small Prandtl number, the method of matched asymptotic expansions is used to construct a solution describing the complete flow field from the surface of the sun to infinity. The first two regions correspond to those found by Roberts and Soward (1972) for large thermal conductivity; the next involves the viscous terms, and in the fourth the viscous terms dominate. From the fourth region it is shown that either the flow remains supersonic but terminates at a finite point, or the flow becomes subsonic through a diffuse shock layer and approaches a nonzero pressure at infinity. The existence of a subsonic/supersonic transition together with a known pressure at infinity can uniquely determine the complete solution. However, to correspond with typical results near the sun and at the earth's orbit the pressure at infinity is found to be very much larger than that generally accepted.

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