Three Types of Flows in the Structure of the Solar Wind

Details Three Types of Flows in the Structure of the Solar Wind Three Types of Flows in the Structure of the Solar Wind

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002arep...46..339l&link_type=abstract

Astronomy Reports, Volume 46, Issue 4, April 2002, pp. 339-345

Astronomy and Astrophysics

Astronomy

1

Scientific paper

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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