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Three types of flows in the structure of the solar wind

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Abstract

An experimental study of the source and formation of large-scale streams in the solar wind is presented. Radio-astronomical data from 1998 are compared with optical SOHO observations and solar coronal magnetic fields calculated from Zeeman data obtained at the Wilcox Observatory. A correlation between the geometry of the solar-wind transition region and the strength of coronal magnetic fields is revealed. For the moderate heliolatitudes studied, this correlation divides into three branches corresponding to three types of coronal magnetic-field structures: open structures with field lines escaping into interplanetary space, closed structures with loop-like field lines, and intermediate structures including both open and closed configurations. High-speed streams of solar wind originate in regions with open magnetic structures. These structures are connected with the lateral lobes of streamers at moderate heliolatitudes. Low-speed flows originate above closed magnetic structures, typical of the main bodies of streamers. The lowest-speed solar-wind flows are not associated with coronal streamer structures, and originate in coronal regions with intermediate magnetic configurations simultaneously containing open and closed field lines. In these regions, the white-light corona becomes an extended and amorphous area with high luminosity, which stratifies into a radial structure with narrow stripes at higher resolution.

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Authors and Affiliations

  1. Institute of Terrestrial Magnetism, Ionosphere and Radio Propagationt, Troitsk, Moscow Region, 142190, Russia

    N. A. Lotova, V. N. Obridko & K. V. Vladimirskii

  2. Lebedev Physical Institute, Leninskii pr. 53, Moscow, 117924, Russia

    N. A. Lotova, V. N. Obridko & K. V. Vladimirskii

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  1. N. A. Lotova
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  2. V. N. Obridko
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  3. K. V. Vladimirskii
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__________

Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \) Zhurnal, Vol. 79, No. 4, 2002, pp. 377–384.

Original Russian Text Copyright © 2002 by Lotova, Obridko, Vladimirski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \).

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Lotova, N.A., Obridko, V.N. & Vladimirskii, K.V. Three types of flows in the structure of the solar wind. Astron. Rep. 46, 339–345 (2002). https://doi.org/10.1134/1.1471398

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