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Astron. Astrophys. 357, 1051-1055 (2000)


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Three types of solar wind flow

N.A. Lotova 1, V.N. Obridko 1 and K.V. Vladimirskii 2

1 Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, 142092 Troitsk, Russia
2 Lebedev Physical Institute, 117924 Moscow, Russia

Received 18 March 1999 / Accepted 13 January 2000

Abstract

The origin of the large-scale stream structure of the solar wind flow was studied using an experimental approach. Radio astronomy data obtained in 1997 were compared with SOHO optical observations of the solar corona and magnetic structures derived from the J.Wilcox Observatory Zeeman data. A correlative relation was obtained between the position of the transonic region of the solar wind and magnetic field strength at the solar corona level. This relation falls into three branches corresponding to three types of the magnetic field structure: an open type with the field lines going in the interplanetary space, closed loop-like type and intermediate type including both configurations of field lines. The high-speed streams originate above the open configurations, while closed and intermediate configurations produce low-speed solar wind.

Key words: Sun: corona – Sun: magnetic fields – Sun: solar wind

Send offprint requests to: N.A. Lotova

© European Southern Observatory (ESO) 2000

Online publication: June 5, 2000

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