Kinetic Simulations of Type II Radio Burst Emission Processes

Details Kinetic Simulations of Type II Radio Burst Emission Processes Kinetic Simulations of Type II Radio Burst Emission Processes

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh53b2051g&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH53B-2051

Physics

Plasma Physics

[2101] Interplanetary Physics / Coronal Mass Ejections, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions, [7829] Space Plasma Physics / Kinetic Waves And Instabilities, [7868] Space Plasma Physics / Wave/Wave Interactions

Scientific paper

The fundamental emission process of Type II Radio Bursts has been under discussion for many decades. While analytic deliberations point to three wave interaction as the source for fundamental and harmonic radio emissions, sparse in-situ observational data and high computational demands for kinetic simulations have not allowed for a definite conclusion to be reached. A popular model puts the radio emission into the foreshock region of a coronal mass ejection's shock front, where shock drift acceleration can create eletrcon beam populations in the otherwise quiescent foreshock plasma. Beam-driven instabilities are then assumed to create waves, forming the starting point of three wave interaction processes. Using our kinetic particle-in-cell code, we have studied a number of emission scenarios based on electron beam populations in a CME foreshock, with focus on wave-interaction microphysics on kinetic scales. The self-consistent, fully kinetic simulations with completely physical mass-ratio show fundamental and harmonic emission of transverse electromagnetic waves and allow for detailled statistical analysis of all contributing wavemodes and their couplings.

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