Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh12a..04s&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SH12A-04
Physics
[2102] Interplanetary Physics / Corotating Streams, [2114] Interplanetary Physics / Energetic Particles, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [2169] Interplanetary Physics / Solar Wind Sources
Scientific paper
Where coronal hole fast wind runs into slow wind ahead, a compression region forms. The boundary between the compressed slow and fast wind is referred to as the stream interface (SI). Ideally, if the coronal source regions of slow and fast wind are distinct and stationary, and the interplanetary magnetic field (IMF) foot point locations are fixed, the SI is a discontinuous plasma boundary for both solar wind ions and 100eV-1keV suprathermal electrons which stream out from the sun through the ions along the IMF. In the ideal case, IMF lines do not cross the SI. However, field line crossing of the SI may result from IMF foot point motion during the time required for solar wind ions to travel from the sun to 1 AU. On January 29, 2005 ACE encountered a stream interface within a CIR at the leading edge of a coronal hole fast stream. A solar electron burst was observed from 11-15 UT at 0.5-1.3 keV energies. The burst was observed across the SI, indicating magnetic connection to the electron burst source region on both sides of the SI. This could indicate that the electron burst source region spanned a coronal hole boundary. A more likely alternative is that field lines on opposite sides of the SI at 1 AU were no longer connected to different sides of a coronal hole boundary. Instead, footpoint motion occurred during solar wind ion transit to 1 AU, so that field lines on both sides of the SI were connected to a single coronal electron burst source region.
McComas David John
Skoug Ruth M.
Steinberg John T.
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