HR: 0800h
AN: SM31B-0454    [Abstracts]
TI: Multi-Instrument Observations of Pc 3-4 Pulsations at Cusp Latitudes in Svalbard, Norway
AU: * Lu, F
EM: lu@augsburg.edu
AF: Augsburg College, Department of Physics 2211 Riverside Ave, St. Paul, MN 55454, United States
AU: Engebretson, M
EM: engebret@augsburg.edu
AF: Augsburg College, Department of Physics 2211 Riverside Ave, St. Paul, MN 55454, United States
AU: Lessard, M
EM: marc.lessard@unh.edu
AF: University of New Hampshire, Space Science Center and Department of Physics 417 Morse Hall, Durham, NH 03824, United States
AU: Kim, H
EM: hyomin.kim@unh.edu
AF: University of New Hampshire, Space Science Center and Department of Physics 417 Morse Hall, Durham, NH 03824, United States
AU: Wright, D
EM: Darren.Wright@ion.le.ac.uk
AF: University of Leicester, Radio and Space Plasma Physics Group Department of Physics & Astronomy University Road Leicester, LE1 7RH, UK, Leicester, LE1 7RH, United Kingdom
AB: It has been generally accepted that Pc 3-4 pulsations (~ 10-100 mHz) originate in the ion foreshock upstream of the bow shock due to the interaction between reflected ions and the solar wind, but it is not clear how these waves propagate to the high-latitude ionosphere. Many early studies noted increased power in the vicinity of the dayside cusp. In this study, we compared signal power at Pc 3-4 frequencies from searchcoil magnetometers at three closely-spaced stations on Svalbard: Ny Alesund (76.31o Magnetic Latitude), Longyearbyen (75.26o Magnetic Latitude) and Hornsund (74.24o Magnetic Latitude). Data from the SuperDARN Finland HF radar and DMSP satellites were used to accurately locate the cusp latitudes. We found several events where magnetometers showed strong, narrow-band Pc 3-4 signals, while during the same period the SuperDARN radar saw a clear-edged cusp and a DMSP satellite passing overhead observed the typical cusp signature. We found that often the wave packets were localized and linearly polorized. Also most of the time, the signals were strongest equatorward of the cusp, consistent not with entry via the cusp proper but along field lines equatorward of the cusp which map to the boundary layer or outer magnetosphere.
DE: 2706 Cusp
DE: 2716 Energetic particles: precipitating
DE: 2728 Magnetosheath
DE: 2736 Magnetosphere/ionosphere interactions (2431)
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting