High-speed streams of the stationary solar wind and the possible mechanism by which they are generated

The velocities of the stationary extra-ecliptic solar wind are analyzed depending on the heliolatitudes, heliocentric distances, and solar activity. An analysis has been performed using the direct measurements of the solar plasma flux velocities onboard Ulysses and the simultaneous ground-based IPS...

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Bibliographic Details
Published in:Geomagnetism and Aeronomy 2010-04, Vol.50 (2), p.153-159
Main Authors: Mogilevskii, E. I., Nikol’skaya, K. I.
Format: Article
Language:English
Subjects:
Astrophysics
Earth and Environmental Science
Earth Sciences
Geophysics/Geodesy
Magnetic fields
Plasma physics
Radiation
Solar activity
Sun
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Summary:The velocities of the stationary extra-ecliptic solar wind are analyzed depending on the heliolatitudes, heliocentric distances, and solar activity. An analysis has been performed using the direct measurements of the solar plasma flux velocities onboard Ulysses and the simultaneous ground-based IPS observations. The arguments for the hypothesis that primary high-speed ( V ∼ 900 km/s) flows exist at the corona bottom and are directly related to the photosphere and solar magnetic fields are presented. The possible mechanism by which high-speed streams are generated is generally considered.
ISSN:0016-7932
1555-645X
0016-7940
DOI:10.1134/S0016793210020027