HR: 1340h
AN: SM23A-0478    [Abstracts]
TI: Correlation between Low Frequency AKR and Auroral Structures
AU: Pazamickas, K
EM: kbzap@msn.com
AF: St. Monica School, 109 Market St., Sunbury, PA 17801 United States
AU: * Green, J L
EM: James.Green@nasa.gov
AF: NASA Goddard Space Flight Center, Code 630, Greenbelt, MD 20771 United States
AU: Gallagher, D L
EM: dennis.gallagher@msfc.nasa.gov
AF: NASA Marshall Space Flight Center, Code SD50, Huntsville, AL 35812 United States
AU: Mende, S
EM: mende@ssl.berkeley.edu
AF: U. C. Berkeley, Space Sciences Laboratory, Berkeley, CA 94720 United States
AU: Frey, H U
EM: hfrey@ssl.berkeley.edu
AF: U. C. Berkeley, Space Sciences Laboratory, Berkeley, CA 94720 United States
AB: Auroral Kilometric Radiation (AKR), a radio emission with a broadband frequency range, has long been associated with auroral activity. Recently we have done a preliminary study of AKR related very low frequency events (hear after referred to as LF AKR) and their association to specific auroral structures. LF AKR events are characterized as a rapid extension of AKR related emissions to 30 kHz or lower in frequency for typically much less than 10 minutes. We have extended the previous study to include all instances of LF AKR events during the nearly 4 years of observations from the IMAGE spacecraft's Radio Plasma Imager (RPI) instrument. We will discuss the possibility of a correlation between low frequency AKR emissions and the bifurcation in the aurora by examining images of the auroral oval from the Far Ultraviolet (FUV) instrument on IMAGE. We will examine the relationship of LF AKR emissions events and other factors including dipole tilt, Dst and AE Index . Although we don't expect LF AKR to be the only factor in the bifurcated auroral structures, we do expect that this bifurcation will occur in every instance when LF AKR is observed. The unique character of LF AKR is a possible indicator of specific processes sometimes occurring during storm-time conditions, resulting from narrow field-aligned density cavities forming at a distance of perhaps 5-6 RE tailward from the Earth.
DE: 2712 Electric fields (2411)
DE: 2772 Plasma waves and instabilities
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting