Physics
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh34a..04s&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SH34A-04
Physics
2102 Corotating Streams, 2109 Discontinuities, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma
Scientific paper
Recent studies have shown that, in selected cases, the heliospheric magnetic field is much more radial than the standard Parker spiral in the rarefactions of co-rotation interaction regions (CIRs). This reveals that open field footpoints at the Sun move through the coronal hole boundary, which causes magnetic field lines to be connected and stretched across the fast-slow wind transition. Here we include footpoint motion at the Sun in a magneto-hydrodynamic (MHD) model to describe the formation and evolution of a CIR out to 5 AU. We compare results with Ulysses observations in CIR rarefactions. In comprehensive observations of CIRs observed by Ulysses from 1992 through 1997, we find that the more radial field, the "sheared sub-Parker spiral", is almost always present in CIR rarefactions. These observations show striking evidence for both systematic footpoint motions strongly consistent with differential rotation, and random footpoint motions, consistent with interchange reconnection that continually reconfigures the open magnetic field. Thus, we reveal the sheared sub-Parker spiral of the inner heliospheric magnetic field, and discuss its broad implications for the origin of solar wind, the nature of coronal holes, and the magnetic structure of the heliosphere.
McComas David John
Schwadron Nathan A.
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