The Underlying Direction of the Heliospheric Magnetic Field at Solar Maximum

Details The Underlying Direction of the Heliospheric Magnetic Field at Solar Maximum The Underlying Direction of the Heliospheric Magnetic Field at Solar Maximum

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0503f&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0503

Physics

2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536), 2169 Sources Of The Solar Wind, 7524 Magnetic Fields

Scientific paper

When Ulysses traversed the south polar regions of the heliosphere during solar maximum in late 2000 the distribution of magnetic field lines about the direction predicted by the Parker spiral model was very much broader than observed at similar latitudes under solar minimum conditions. Large deviations of up to 90 degrees were much more common. The reasons for this behaviour appear to be associated with the presence of the heliospheric current sheet in the high latitude regions. In this paper we extend this study to the north polar regions traversed by Ulysses during 2001 where a fast solar wind stream from the north polar coronal hole had become re-established. We compare the distributions of the magnetic field direction obtained at this time with those obtained at the south pole at solar maximum and those obtained at both poles at solar minimum when fast solar wind was routinely present in these regions. We find that the highly disturbed field direction distributions are unique to the south polar regions dominated by slow and intermediate speed solar wind streams near solar maximum.

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