Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm42d..02c&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #SM42D-02
Physics
2704 Auroral Phenomena (2407), 2724 Magnetopause, Cusp, And Boundary Layers, 2736 Magnetosphere/Ionosphere Interactions, 2407 Auroral Ionosphere (2704), 2431 Ionosphere/Magnetosphere Interactions (2736)
Scientific paper
Magnetic reconnection plays an important role in transferring solar wind mass, momentum, and energy into the magnetosphere. The merging site and rate depend on the solar wind and IMF condition. Magnetosheath plasmas precipitate into the ionosphere on magnetic field lines that become open as a result of the magnetic merging. Plasmas boundaries associated with the open/closed field line boundary as in the subsolar merging or the high-latitude boundary between the intense solar wind plasma and polar rain as in the lobe merging provide information regarding the location and size of merging line for various IMF conditions. Because of their scale and long duration of coverage, global images of auroral emissions produced by energetic protons in the cusp and its vicinity are particularly useful in determining the above plasma boundaries. We will utilize proton aurora images from IMAGE/FUV and ionosphere flows from SuperDARN radar network to estimate plasma boundaries at the ionosphere and map these boundaries to the magnetopause to estimate the size and location of merging line. For each solar wind and IMF condition, a range of estimates will be discussed.
Avanov Levon
Chang Sandy
Frey Harald U.
Gallagher Dennis L.
Greenwald Ray A.
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