HR: 0800h
AN: SH21B-0426    [Abstracts]
TI: Time-of-flight dispersed electrons at strong interplanetary shocks
AU: * Pulupa, M
EM: pulupa@ssl.berkeley.edu
AF: Space Sciences Laboratory University of California, Berkeley, 7 Gauss Way, Berkeley, CA 94720 United States
AU: * Pulupa, M
EM: pulupa@ssl.berkeley.edu
AF: Department of Physics University of California, Berkeley, 366 LeConte Hall, Berkeley, CA 94720 United States
AU: Bale, S D
EM: bale@ssl.berkeley.edu
AF: Space Sciences Laboratory University of California, Berkeley, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Bale, S D
EM: bale@ssl.berkeley.edu
AF: Department of Physics University of California, Berkeley, 366 LeConte Hall, Berkeley, CA 94720 United States
AB: Strong interplanetary shocks accelerate solar wind electrons to produce a foreshock region and, often, type II radio bursts. On upstream field lines, these electrons can be dispersed due to time-of-flight effects. We use data from instruments on the Wind spacecraft to study this effect at several strong IP shocks. At each shock, a velocity-dispersed electron beam is detected in the upstream region. We use the dispersion to calculate field line length to the shock source. The measurement of field line length indicates the existence and scale of structure on the shock front.
DE: 7513 Coronal mass ejections
DE: 7534 Radio emissions
DE: 2139 Interplanetary shocks
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting