Solar Wind Density Propagation and Magnetospheric Response

Details Solar Wind Density Propagation and Magnetospheric Response Solar Wind Density Propagation and Magnetospheric Response

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm41a2003j&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM41A-2003

Physics

[2164] Interplanetary Physics / Solar Wind Plasma, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [7924] Space Weather / Forecasting

Scientific paper

Solar wind pressure changes produce a characteristic increase or decrease in Bz on the dayside magnetosphere. This response can be used to study the propagation of variations observed at an upstream satellite to the Earth. We use this relationship to determine the characteristic orientation of planar fronts. This result is roughly consistent with one-half the average Parker spiral angle. However, it is not strongly dependent on solar wind velocity. As well, there is a distinct population of different orientations associated with ortho-spiral IMF configurations.

Affiliated with

Also associated with

No associations

Rating

Solar Wind Density Propagation and Magnetospheric Response 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 Solar Wind Density Propagation and Magnetospheric Response, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Solar Wind Density Propagation and Magnetospheric Response will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1891000