Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh32d..01g&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #SH32D-01
Physics
2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma
Scientific paper
Numerous examples when the heliospheric magnetic field is oriented nearly radial to the Sun for intervals of several hours or more have been reported in the literature. Occasionally the field in such events remains nearly radial for many hours. A very large fraction of radial field events occur at times when the solar wind flow speed is declining gradually. Here we propose that most radial field events in the solar wind result from temporally discontinuous drops in flow speed on field lines close to the Sun. The sudden drop in flow speed along an open field line may, but need not necessarily, be the result of an interchange reconnection of the open field line with a closed field line. In our idealized model a radially-directed magnetic field connects the different Archimedean spirals associated respectively with the faster and slower flows preceding and following the temporal flow speed discontinuity. With increasing heliocentric distance the radial extent of the event increases while the flow speed discontinuity that produces it evolves into a gradual flow speed decline.
Gosling Jack T.
Skoug Ruth M.
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