Evolution of Relativistic Electron Ring Distribution Associated with Cyclotron Maser Instability

Details Evolution of Relativistic Electron Ring Distribution Associated with Cyclotron Maser Instability Evolution of Relativistic Electron Ring Distribution Associated with Cyclotron Maser Instability

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm13b2056l&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM13B-2056

Physics

Plasma Physics

[7829] Space Plasma Physics / Kinetic Waves And Instabilities, [7839] Space Plasma Physics / Nonlinear Phenomena, [7845] Space Plasma Physics / Particle Acceleration, [7867] Space Plasma Physics / Wave/Particle Interactions

Scientific paper

We carried out a series of simulations to study the cyclotron maser instability (CMI) with the initial condition that a population of tenuous energetic electrons with a pure ring distribution is present in a magnetized background plasma. In this report, relativistic cases are discussed with the initial ring kinetic energy ranging from 50 to 500keV, and the ratio of electron plasma to electron cyclotron frequency, α=ωpe/Ωce, ranges from 0.2 to 1. In the simulation, the Z or X mode with θB=90 or the Z mode with θB=0 is the dominant mode, where θB is a wave propagation angle with respect to ambient magnetic field. The amplification of wave modes highly depends on not only the value of α, but also the initial kinetic energy ɛ. For example, in cases with α=0.2 and ɛ=50-500keV, the first harmonic Z (Z1) mode with θB=90 is dominant; in the case with α=0.33 and ɛ=500keV, the Z1 mode with θB=0 is dominant; in the case with α=1.0 and ɛ=100keV, the second harmonic X (X2) mode with θB=90 is dominant. The amplification of the X or Z mode with θB=90 decreases the perpendicular energy of most ring electrons, and the excitation of Z mode with θB=0 diffuses the initial ring distribution leading to an X-like pattern in momentum space. Although only a fraction of the ring electrons can be accelerated/heated to the high-energy tail of the X-like distribution, as the distribution evolves, electron energy in the high-energy tail can reach double of the initial kinetic energy within two thousand cyclotron periods and even 4 times of the initial kinetic energy in 5000-10000 cyclotron periods. A comparison between 1D and 2D results is presented. A preliminary theory is developed as well.

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