Mathematics – Logic
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm11c..07b&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SM11C-07
Mathematics
Logic
2723 Magnetic Reconnection (7526, 7835), 2744 Magnetotail, 2760 Plasma Convection (2463), 2776 Polar Cap Phenomena, 2784 Solar Wind/Magnetosphere Interactions
Scientific paper
Magnetic reconnection at the dayside magnetopause is the main process by which mass, energy, and momentum from the solar wind enter the terrestrial magnetosphere. Magnetic reconnection at the nightside energizes magnetotail plasma and closes the lobe open flux, thus completing the cycle that initiates and sustains magnetospheric convection. Understanding the drivers of reconnection and convection in the magnetosphere is one of the primary goals of magnetospheric physics. It has long been recognized that the Interplanetary Magnetic Field (IMF) is the most influential factor in initiation of reconnection and convection in the magnetosphere. Recent evidence has shown that the solar wind dynamic pressure plays also an important role in enhancing both dayside and nightside reconnection, and driving enhanced ionospheric convection. Super Dual Auroral Radar Network (SuperDARN) observations show that solar wind pressure fronts induce significantly enhanced ionospheric convection in the dayside ionosphere. In parallel, Defense Meteorological Satellite Program (DMSP) precipitating particle measurements and POLAR Ultra-Violet Imager (UVI) images have demonstrated that sudden solar wind pressure increases also significantly affect the size of the polar cap. The polar cap is observed to shrink after an increase in solar wind pressure, especially on the nightside, suggesting an enhancement of magnetotail reconnection. MHD models of the interaction of the magnetosphere with solar wind pressure fronts have managed to reproduce the enhancement of dayside reconnection, but have failed so far to account for the observed closing of the polar cap on the nightside and the suggested magnetotail reconnection increase. We use SuperDARN observations of ionospheric convection within both the dayside and nightside polar ionosphere, including near the magnetic separatrix, to evaluate the relative strengths of the observed dayside and nightside reconnection enhancements after an abrupt increase in solar wind dynamic pressure. We show that enhancements of both dayside and nightside convection occur after an increase in pressure, suggesting an increased reconnection rate on both sides of the ionosphere. We discuss these results in terms of a competition between dayside and nightside reconnection in the determination of the size of the polar cap and possibly their effect on the transpolar potential.
Anderson Philip C.
Boudouridis Athanasios
Lummerzheim Dirk
Lyons Larry R.
Ruohoniemi Michael J.
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