Rapid response of the plasmasphere to changes in the solar wind and IMF: Global plasmapause electric field measurements by IMAGE EUV, and simulation with the Rice MSM.

Details Rapid response of the plasmasphere to changes in the solar wind and IMF: Global plasmapause electric field measurements by IMAGE EUV, and simulation with the Rice MSM. Rapid response of the plasmasphere to changes in the solar wind and IMF: Global plasmapause electric field measurements by IMAGE EUV, and simulation with the Rice MSM.

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm41b..09g&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SM41B-09

Physics

2700 Magnetospheric Physics, 2712 Electric Fields (2411), 2730 Magnetosphere: Inner, 2760 Plasma Convection, 2768 Plasmasphere

Scientific paper

Images recorded by the extreme ultraviolet (EUV) instrument on the IMAGE satellite very often show a well-defined and identifiable plasmapause; dynamic changes in the shape and location of this plasmapause can be tracked by EUV with 10-minute time resolution. For some time, it has been established that the plasmapause moves in response to changes in the global magnetospheric convection field, which in turn is driven by solar wind dynamic pressure and interplanetary magnetic field (IMF) orientation. A handful of time histories recorded by EUV show the plasmapause moving radially inward or outward. Comparison of the EUV-observed plasmapause time development with IMF orientation in these cases shows that the plasmapause responds rapidly (within 25 to 30 minutes) to sudden changes in the IMF Bz polarity. A change to southward Bz enhances magnetospheric convection, causing visible inward motion of the nightside plasmapause. A change to northward Bz seems to trigger an overshielding condition, producing outward motion of the nightside plasmapause. In general the plasmapause motion (inward and outward) seems to be concentrated most strongly in the post-midnight sector, with a lesser concentration at pre-noon MLT. This spatial character is consistent with simulation results of the Rice Magnetospheric Specification Model (MSM). The overall picture, from both observation and simulation, is that the plasmapause location is very responsive to changes in the solar wind and IMF conditions.

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