Localization on the sun of regions from which quasi-steady high-speed solar-wind streams emanate

Details Localization on the sun of regions from which quasi-steady high-speed solar-wind streams emanate Localization on the sun of regions from which quasi-steady high-speed solar-wind streams emanate

Aug 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977azh....54..859k&link_type=abstract

Astronomicheskii Zhurnal, vol. 54, July-Aug. 1977, p. 859-869. In Russian.

Astronomy and Astrophysics

Astronomy

2

Magnetic Field Configurations, Radiation Sources, Solar Magnetic Field, Solar Wind, Astronomical Maps, Photosphere, Solar Corona, Solar Cycles, Solar Wind Velocity

Scientific paper

Properties of solar regions that constitute sources of quasi-steady high-speed solar-wind streams are analyzed. It is found that the high-speed streams are localized in coronal regions with open, nonradially divergent magnetic-field configurations. These regions are shown to be characterized by a low level of coronal emission and decreased density; as a rule, they adjoin coronal condensations. A model is presented which can explain some features of the velocity variations of high-speed streams over a solar activity cycle. The results obtained are taken as confirmation of the previous conclusion that active regions play a major role in producing high-speed solar-wind streams which affect geophysical activity. It is concluded that the magnetic-field geometry in the corona determines the sites where quasi-steady high-speed solar-wind streams are localized.

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