Meridional flow in the solar wind in the presence of latitudinally dependent boundary conditions

Details Meridional flow in the solar wind in the presence of latitudinally dependent boundary conditions Meridional flow in the solar wind in the presence of latitudinally dependent boundary conditions

Nov 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...45..255n&link_type=abstract

Solar Physics, vol. 45, Nov. 1975, p. 255-266.

Physics

6

Boundary Conditions, Magnetohydrodynamic Flow, Meridional Flow, Perturbation Theory, Solar Wind, Asymptotic Methods, Boundary Value Problems, Magnetic Field Configurations, Radial Velocity

Scientific paper

The influence of latitudinally dependent boundary conditions on the large-radius values of meridional flow in the distant solar wind is examined through a double-perturbation expansion of the magnetohydrodynamic equations. A general result is derived for the meridional velocity which allows arbitrary specification of radial velocity, radial magnetic field, and mass flux as a function of colatitude at some coronal reference surface. Three specific examples are treated, including the model of Pneuman and Kopp (1971). The latter example indicates that there may be flow toward the equator at large radii, as opposed to the pure equatorial divergence of internally generated motion due to a flow which is latitudinally uniform at the reference radius. A solar-cycle effect most probably averages the boundary conditions so that only the equatorial divergence from an average spherically symmetric corona is seen in comet-tail observations. This may also explain the off-and-on-again nature of the meridional gradient in the radial velocity of the solar wind as seen in radio scintillation observations.

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