A possible mechanism for generating high-velocity solar-wind streams

Details A possible mechanism for generating high-velocity solar-wind streams A possible mechanism for generating high-velocity solar-wind streams

Apr 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976sval....2...78k&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 2, Apr. 1976, p. 200-206.) Soviet Astronomy Letters, vol. 2, Mar.-Apr. 1976, p. 78-80.

Physics

1

Magnetohydrodynamics, Solar Physics, Solar Wind Velocity, Lines Of Force, Magnetic Field Configurations, Plasma Density, Solar Corona, Solar Magnetic Field

Scientific paper

Solar-wind properties are analyzed in the framework of a hydrodynamic approximation for radial and nonradial expansion in order to investigate the sources and formation conditions of high-speed streams. The results suggest that the sources of these streams are large-scale coronal regions with nonradially diverging, open magnetic-field lines. It is shown that large-scale nonradial expansion near the sun (within 1.3 to 3 solar radii) can simultaneously increase the velocity and decrease the density of the solar wind near earth's orbit, thus giving rise to the high-speed streams.

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