The solar wind's return to a simple three-dimensional structure: Ulysses' second fast-latitude scan

Details The solar wind's return to a simple three-dimensional structure: Ulysses' second fast-latitude scan The solar wind's return to a simple three-dimensional structure: Ulysses' second fast-latitude scan

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh42c..03m&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH42C-03

Physics

2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536), 2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind

Scientific paper

Ulysses' first orbit, which occurred over the declining phase and through minimum of the solar activity cycle, revealed a regular and quite symmetric global solar wind structure, with fast, uniform solar wind from polar coronal holes at mid- and high-heliolatitudes. In contrast, Ulysses' second orbit exhibited a much more complex mixture of solar wind with both fast and slower flows from numerous smaller coronal holes, more frequent coronal mass ejections, active regions, and slow, dense, streamer belt type flows at all latitudes. Now, as Ulysses again reaches its highest northern latitudes in its second fast latitude scan, longer intervals of more uniform fast solar wind are being observed. These observations suggest that a reforming northern polar coronal hole is again beginning to provide the dominant fast, uniform solar wind observed ubiquitously at mid- and high-latitudes over the first orbit. Solar observations confirm the reformation of a large polar coronal hole. These observations in combination with our earlier results indicate that the highly structured high latitude solar wind may be only a short-lived phase around solar maximum with the large polar coronal hole flows dominant throughout the rest of the solar cycle.

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