Time-of-flight dispersed electrons at strong interplanetary shocks

Details Time-of-flight dispersed electrons at strong interplanetary shocks Time-of-flight dispersed electrons at strong interplanetary shocks

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh21b0426p&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH21B-0426

Physics

7513 Coronal Mass Ejections, 7534 Radio Emissions, 2139 Interplanetary Shocks

Scientific paper

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.

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