Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh22a0847s&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH22A-0847
Physics
2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma, 2169 Solar Wind Sources, 2199 General Or Miscellaneous
Scientific paper
Large rotations observed in the interplanetary magnetic field (IMF) can be due to true field polarity reversals, i.e. crossings of the heliospheric current sheet. But very often they are instead encounters with fields that are locally folded back upon themselves. Within coronal hole-related high-speed streams, we find that folds can be readily distinguished from true polarity reversals by using the property of differential streaming between alpha particles and protons. The vector difference between the alpha particle velocity and the proton velocity lies parallel (or anti- parallel) to the magnetic field, but always points in the field-aligned direction away from the sun. Previously we presented a survey of folds within the uniform coronal hole-related high-speed solar wind sampled by Ulysses at solar minimum during the first Northern Polar pass. We found that all the folds examined showed correlation between the field turnings and variations in the solar wind velocity vector, indicative of propagating Alfvenic features. Here we present an extension of that survey to solar wind from isolated polar coronal holes seen by ACE and Ulysses at solar maximum. We report on the occurence of folded fields and polarity reversals near solar maximum, including how the observed frequency and duration of folded field intervals differ between flow from larger solar minimum polar coronal holes and smaller isolated solar maximum coronal holes.
Skoug Ruth M.
Steinberg John T.
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