HR: 0800h
AN: SA21A-0286    [Abstracts]
TI: Cluster Observations of Pc 1-2 Waves and Associated Ion Distributions During the October and November 2003 Magnetic Storms
AU: * Engebretson, M J
EM: engebret@augsburg.edu
AF: Augsburg College, 2211 Riverside Ave, Minneapolis, MN 55454 United States
AU: Keiling, A
EM: keiling@ssl.berkeley.edu
AF: University of California, Berkeley, Space Science Laboratory, Berkeley, CA 94720 United States
AU: Fornacon, K -
EM: k-h.fornacon@tu-bs.de
AF: Institut fur Geophysik und Meteorologie, Technical University of Braunschweig, Braunschweig, D-83106 Germany
AU: Catell, C A
EM: cattell@belka.space.umn.edu
AF: University of Minnesota, School of Physics and Astronomy, Minneapolis, MN 55454 United States
AU: Johnson, J R
EM: jrj@pppl.gov
AF: Princeton University, Plasma Physics Laboratory, Princeton, NJ 08543 United States
AU: Posch, J L
EM: posch@augsburg.edu
AF: Augsburg College, 2211 Riverside Ave, Minneapolis, MN 55454 United States
AU: Glassmeier, K -
EM: kh.glassmeier@tu-bs.de
AF: Institut fur Geophysik und Meteorologie, Technical University of Braunschweig, Braunschweig, D-83106 Germany
AU: Parks, G K
EM: parks@ssl.berkeley.edu
AF: University of California, Berkeley, Space Science Laboratory, Berkeley, CA 94720 United States
AU: RŠme, H
EM: reme@cesr.fr
AF: Centre d'Etude Spatiale des Rayonnements, Centre National de la Recherche Scientifique, Toulouse, 31028 France
AB: Unusual wave activity in the Pc 1-2 frequency band (0.1-5 Hz) was observed by the Cluster spacecraft in association with the two large geomagnetic storms of late 2003. During the onset of the Halloween storm on October 29, 2003, intense broadband activity between ~0.1 and 0.6 Hz appeared at all 4 spacecraft on both sides of the magnetic equator at perigee (near 1400 UT and 08:45 MLT). Power was especially strong and more structured in frequency in the compressional component: a minimum in wave power was observed at 0.38 Hz, corresponding to the oxygen ion cyclotron frequency. Poynting vector calculations indicated that wave power was primarily directed radially outward rather than along the magnetic field. Narrowband purely compressional waves near 0.15 Hz appeared at higher dayside latitudes in the southern hemisphere. CIS ion spectrometer data during this pass revealed that O⁺ was the dominant energetic ion. During the recovery phase of the November storm, on November 22, 2003, predominantly transverse 1.8 Hz waves with peak-to-peak amplitude of 10 nT were observed by all four spacecraft near perigee at L = 4.4. During this more typical Pc 1 event, wave power was directed along B, toward the northern ionosphere. An unusually polarized 2.3 Hz emission (with power in the radial and compressional, but not azimuthal directions) was observed at L = 5.4-5.9, 10-15° south of the magnetic equator. We infer that this wave event may have been generated on lower L shells and propagated obliquely to Cluster's location. Consistent with other recent observations, anisotropic plasma sheet / ring current proton distributions appeared to be a necessary condition for occurrence of waves during both passes, but was not always a sufficient condition. The transverse waves of Nov. 22 occurred in regions which also contained greatly increased fluxes of cool ions (E < 1 keV). On both days Cluster observed features not previously reported, and we note that the purely compressional nature of the October 29 events was not anticipated in previous theoretical studies. The fact that these unusually polarized waves occurred in association with very intense geomagnetic storms suggests that they are likely to be extremely rare.
DE: 2720 Energetic particles: trapped
DE: 2730 Magnetosphere: inner
DE: 2752 MHD waves and instabilities (2149, 6050, 7836)
SC: SPA-Aeronomy [SA]
MN: Fall Meeting 2005