Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0509m&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0509
Physics
2102 Corotating Streams, 2134 Interplanetary Magnetic Fields
Scientific paper
Observations of the magnetic field orientation in co-rotating rarefaction regions (CRRs) reveal that they are often significantly under-wound compared to the expected Parker spiral, sometimes being almost radial. In particular, CRRs sampled by the Ulysses and Pioneer spacecraft beyond 4 AU from the sun often show average field orientations deviating by more than 30° from the expected Archimedian spiral. These steady state structures last many days, with very little variance in the magnetic field magnitude or direction. The observations are explained by a model combining footpoint motion between fast to slow solar wind streams at the source surface, with the effects of velocity shear across coronal hole boundaries. Using reasonable values for the thickness of and the rate of footpoint transport across the coronal hole boundary, the model reproduces our observations. It also predicts that the magnetic field will evolve asymptotically to a fixed angle and not continue to become more tightly wound with distance.
Murphy Neil
Schwadron Nathan
Smith Edward
No associations
LandOfFree
Strongly Under-wound and Near-Radial Magnetic Fields in the Solar Wind does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Strongly Under-wound and Near-Radial Magnetic Fields in the Solar Wind, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Strongly Under-wound and Near-Radial Magnetic Fields in the Solar Wind will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1435831