HR: 11:20h
AN: SM42A-05    [Abstracts]
TI: Hemispheric Asymmetries in the Dayside Aurora
AU: * Fillingim, M O
EM: matt@ssl.berkeley.edu
AF: University of California, Berkeley, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Spasojevic, M
AF: University of California, Berkeley, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Parks, G K
AF: University of California, Berkeley, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Immel, T J
AF: University of California, Berkeley, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Mende, S B
AF: University of California, Berkeley, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AB: Using global auroral images from Polar UVI in the southern hemisphere and IMAGE FUV in the north, we have analyzed the asymmetries in the dayside aurora for a five-month period. The observed asymmetries were related to the interplanetary magnetic field (IMF). Initial results suggest that the direction of the IMF plays a major role in influencing the asymmetrical behavior of the dayside aurora. When the IMF is southward and a significant dawnward component exists, there is an enhancement in the afternoon aurora in the northern hemisphere. If there is a significant duskward component to the IMF, then an enhancement in the afternoon aurora in the southern hemisphere is observed. Additionally, when the ratio of the magnitudes of the Y and Z components of the IMF are greater than about 2, distinct structure (i.e., a string of pearls configuration) is seen in the hemisphere with enhanced emission. These results are in general agreement with models and observations of the IMF influence on ionospheric convection. A strong Y component of the IMF can lead to a strong shear flow at the dayside convection reversal boundary. Strong flow shear can lead to strong field aligned currents (i.e., elelctron precipitation for upward current) in this same region. If the flow shear exceeds some threshold, an instability (e.g., a Kelvin-Helmholtz instability) can develop leading to discrete structures.
UR: http://sprg.ssl.berkeley.edu/matt/AGU04/
DE: 2704 Auroral phenomena (2407)
DE: 2736 Magnetosphere/ionosphere interactions
DE: 2760 Plasma convection
DE: 2772 Plasma waves and instabilities
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting