MHD moment equations for strong spherically symmetric magnetic fields - Application to solar wind expansion

Details MHD moment equations for strong spherically symmetric magnetic fields - Application to solar wind expansion MHD moment equations for strong spherically symmetric magnetic fields - Application to solar wind expansion

Jun 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....58..339f&link_type=abstract

Astronomy and Astrophysics, vol. 58, no. 3, June 1977, p. 339-344.

Astronomy and Astrophysics

Astrophysics

7

Anisotropic Media, Magnetic Fields, Magnetohydrodynamics, Particle Trajectories, Solar Wind, Astronomical Models, Continuity Equation, Differential Equations, Field Strength

Scientific paper

Magnetohydrodynamic moment equations for strong magnetic fields in a spherically symmetric geometry are derived using the method of integration along single particle trajectories rather than an expansion technique for the velocity distribution function. The behavior of an anisotropic plasma in a strong inhomogeneous magnetic field is then investigated, with special application to the radial expansion of the solar wind. Closure of the set of differential equations is accomplished by introducing anisotropic polytropic indices in order to simulate various forms of solar-wind heating. It is shown that temperature anisotropies where the perpendicular temperature component is greater than the parallel component, resulting from preferentially stronger heating of the perpendicular energy mode, can produce distinctly higher solar-wind bulk velocities at heliocentric distances between 2 and 100 solar radii, and also reduced temperature anisotropies at the orbit of earth.

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