Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm42a..02w&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SM42A-02
Physics
2431 Ionosphere/Magnetosphere Interactions (2736), 2481 Topside Ionosphere, 2704 Auroral Phenomena (2407), 2784 Solar Wind/Magnetosphere Interactions
Scientific paper
The ionosphere is clearly a significant source of magnetospheric plasma [Chappell et al., 1987] since terrestrial ions have been discovered in the ring current [Johnson et al., 1977], the plasma sheet [Peterson et al., 1981], and the tail lobes [Eastman et al., 1984]. The escape of plasma from the ionosphere to the magnetosphere is a multi-step process that begins with upwelling of ionospheric plasma in the topside. Some distance above the topside, the heavier ions (O+, N+, N2+, O2+, NO+) gain escape energy by one or more of a multitude of wave-particle energization processes. Ionospheric upwelling does not always lead to plasma escape since it can be part of the normal "breathing" of the atmosphere as it responds to changes in the inputs of solar or magnetospheric energy. When upwelling does participate in ion outflow, it can control the flux of escaping ions by the rate at which it feeds thermal plasma to the higher altitude energization regions. In that regard, it is important to understand ionospheric upwelling that occurs in places where escaping ions are generated routinely such as the so-called cleft ion fountain [Lockwood et al., 1985; Valek et al., 2002] and the dayside auroral zone. Using ion driftmeter and RPA data from several DMSP satellites we demonstrate how topside plasma upflow on the dayside responds to variations in the solar wind. We have observed that the intensity of the upflow flux, the location of the upflow region, and the size of the upflow region are highly correlated with solar wind parameters such as the merging electric field and dynamic pressure.
Germany Glynn A.
Wilson Gordon Ray
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