HR: 11:45h
AN: SM22A-06    [Abstracts]
TI: Observation of the Dayside Cusp With IMAGE, Cluster, and DMSP
AU: * Sharber, J R
EM: jsharber@swri.edu
AF: Southwest Research Institute, Space Science and Engineering Division, 6220 Culebra Road, San Antonio, TX 78238 United States
AU: Gurgiolo, C A
AF: Bitterroot Basic Research, 837 Westside Road, Hamilton, MT 59840 United States
AU: Mende, S B
AF: University of California, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Frey, H U
AF: University of California, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Burch, J L
AF: Southwest Research Institute, Space Science and Engineering Division, 6220 Culebra Road, San Antonio, TX 78238 United States
AU: Parks, G K
AF: University of California, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Cumnock, J A
AF: Royal Institute of Technology, Alfven Laboratory, Stockholm, SE-100 44 Sweden
AU: Cumnock, J A
AF: University of Texas at Dallas, Center for Space Sciences, P.O. Box 830688, Richardson, TX 75083 United States
AU: Keith, W R
AF: Goddard Space Flight Center, Code 692, Greenbelt, MD 20771 United States
AU: Reme, H
AF: Paul Sabatier University, CESR, 9 ave de Colonel Roche, Toulouse, F-31028 France
AU: Lewis, W S
AF: Southwest Research Institute, Space Science and Engineering Division, 6220 Culebra Road, San Antonio, TX 78238 United States
AU: Fazakerley, A N
AF: University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT United Kingdom
AB: The IMAGE, Cluster, and DMSP spacecraft are used to investigate the cusp during an extended interval of IMF north on March 20-21 of 2002. Continuous monitoring by the IMAGE Far Ultraviolet spectrographic imager within the ~5 hour interval shows the dayside IMF-north emission region or spot, transpolar arcs, and evidence of a small substorm. Within the study interval the Cluster and DMSP F-13 field lines map down to the dayside spot. We are thus able to make a direct comparison between the particle measurements at Cluster and the cusp FUV emissions as well as determine the convective flow patterns at low altitudes. We relate the cusp characteristics to the rest of the oval and subsequently to the magnetosphere. The appearance and fading of the transpolar arcs provide information on changes in the magnetospheric configuration, which are then related to changes in the solar wind plasma and field characteristics.
DE: 2700 MAGNETOSPHERIC PHYSICS
DE: 2704 Auroral phenomena (2407)
DE: 7800 SPACE PLASMA PHYSICS
SC: SPA-Magnetospheric Physics [SM]
MN: 2005 Joint Assembly