Relativistic cyclotron resonance condition as applied to Type II interplanetary radio emission

Details Relativistic cyclotron resonance condition as applied to Type II interplanetary radio emission Relativistic cyclotron resonance condition as applied to Type II interplanetary radio emission

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jgra..10902106f&link_type=abstract

Journal of Geophysical Research, Volume 109, Issue A2, CiteID A02106

Physics

Plasma Physics

2

Solar Physics, Astrophysics, And Astronomy: Radio Emissions, Space Plasma Physics: Radiation Processes, Space Plasma Physics: Wave/Particle Interactions, Space Plasma Physics: Waves And Instabilities, Space Plasma Physics: Shock Waves

Scientific paper

We demonstrate that energy from energetic electrons upstream of interplanetary (IP) shocks are able to couple directly to the o-mode radio branch via the relativistic cyclotron harmonic resonance interaction, thereby creating the Type II radiation observed from IP shocks. The conditions required for the electron/wave resonance are that the wave frequency, f, lies near the local plasma frequency, fp, and near (but not exactly at) the cyclotron harmonics, mfc, where m is the cyclotron harmonic number. We compare the details of this relativistic electron cyclotron harmonic theory with observations in a Type II source region, with good agreement in many areas including the prediction of ``Zeeman'' splitting of the Type II emission. Based on the character of the high-resolution emission spectrum, we can narrow the Type II source location to the IP shock foot region and place some general conditions on shock topology required for Type II emission.

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