High-speed streams from coronal holes and the accelerating mechanism of the solar wind

Details High-speed streams from coronal holes and the accelerating mechanism of the solar wind High-speed streams from coronal holes and the accelerating mechanism of the solar wind

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982gapfd..19..311h&link_type=abstract

Geophysical and Astrophysical Fluid Dynamics, vol. 19, no. 3-4, 1982, p. 311-330.

Physics

Fluid Dynamics

4

Atmospheric Heating, Coronal Holes, Mach Number, Plasma Acceleration, Plasma Temperature, Solar Wind Velocity, Magnetic Field Configurations, Plasma Heating, Solar Magnetic Field, Temperature Distribution, Transonic Flow, Velocity Distribution

Scientific paper

The general Mach number equation is derived, and the influence of typical energy forms in the solar wind is analyzed in detail. It is shown that the accelerating process of the solar wind is influenced critically by the form of heating in the corona, and that the transonic mechanism is mainly the result of the adjustment of the variation of the cross-section of flowing tubes and the heat source term. The accelerating mechanism for both the high-speed stream from the coronal hole and the normal solar wind is similar. But the temperature is low in the lower level of the coronal hole and more heat energy supply in the outside is required, hence the high speed of the solar wind, while the case with the ordinary coronal region is just the opposite, and the velocity of the solar wind is therefore lower. The accelerating process for various typical parameters is calculated, and it is found that the high-speed stream may reach 800 km/sec.

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