Solar wind electron beams and type II and III radio emission

Details Solar wind electron beams and type II and III radio emission Solar wind electron beams and type II and III radio emission

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21d..06b&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH21D-06

Physics

2114 Energetic Particles, Heliospheric (7514), 2139 Interplanetary Shocks, 2159 Plasma Waves And Turbulence

Scientific paper

Type II and III radio emission are generated by the plasma emission process in the solar wind and are signatures of energetic electron beams. Strong CME-driven IP shocks often accelerate electrons into a foreshock region upstream of the shock. This foreshock is also the source of the type II radio emission associated to fast CMEs. The electrons become time-of-flight dispersed along the bundle of magnetic field lines just tangent to the shock surface and the velocity dispersion observed on these field lines can be used to estimate the distance back to the shock front. Combined with the propagation of the shock in the solar wind, this technique can be used to remotely sample the shock front and, often, discern macroscopic structure. We present several examples of velocity dispersed electrons and plasma waves originating at CME-driven shock observed by instruments on Wind.

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