Physics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh51a..07j&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SH51A-07
Physics
2100 Interplanetary Physics, 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks, 2164 Solar Wind Plasma, 7513 Coronal Mass Ejections
Scientific paper
The total perpendicular pressure (thermal plus magnetic) has a very characteristic pattern at the interface between fast and slow streams. The total pressure rises to a maximum at the interface and then decline. This pattern may include sudden changes in pressure at forward and/or reverse shocks. A necessary condition is that the solar wind speed increases through the enhanced pressure region. This aids in the positive identification of the stream interaction. Usually, there are abrupt changes in the plasma properties at the peak in the pressure profile signifying the interface between the two distinct solar wind source regions. The height of the pressure maximum indicates the strength of the interaction. This strength often falls in a narrow range over an extended period of time. Shocks or shock-like jumps in pressure are surprisingly frequent, appearing in about 30 percent of the stream interactions in 1997.
Gosling Jack T.
Jian Li
Luhmann Janet G.
Russell Christopher T.
No associations
LandOfFree
Using Total Perpendicular Pressure to Diagnose Stream Interactions 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 Using Total Perpendicular Pressure to Diagnose Stream Interactions, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Using Total Perpendicular Pressure to Diagnose Stream Interactions will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1694116