Reconstruction of Chorus Type Whistler Waves Distribution in the Radiation Belts and Inner Magnetosphere Using Ray Tracing

Details Reconstruction of Chorus Type Whistler Waves Distribution in the Radiation Belts and Inner Magnetosphere Using Ray Tracing Reconstruction of Chorus Type Whistler Waves Distribution in the Radiation Belts and Inner Magnetosphere Using Ray Tracing

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm41b2022b&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM41B-2022

Physics

[2774] Magnetospheric Physics / Radiation Belts

Scientific paper

The quasi-monochromatic whistler wave packets are supposed to be formed in the vicinity of the magnetic equator and are frequently observed for example by Cluster spacecraft. The objective of our study is a reconstruction of realistic distribution of chorus emissions in radiation belts and in inner magnetosphere. To achieve this aim the data from the electric and magnetic field measurements onboard Cluster satellite are used to determine the major characteristics of the chorus signal around the equator region, namely, its averaged wave vector, wave vector distribution, Poynting flux and polarization. Then the propagation of such a wave packet is modeled using ray tracing technique. We developed the original code which employs K. Rönnmark's WHAMP to obtain hot plasma dispersion function values along the wave packet trajectory. The observed (real) whistler wave distributions at the equator are first fitted to reproduce the observed waveform using Cluster observations (initial conditions) and then these rays are propagated numerically through the inner magnetosphere in the frame of the WKB approximation. The density distribution of the magnetospheric particles is taken from the Gallagher et al. package that is provided by the authors and distributed as free software. Ray tracing allows one to reconstruct the properties of waves such as electric and magnetic fields, and the width of the wavepacket in k-space along the propagation path. The calculations take into account realistic effects of the spreading of the signal due to propagation in the inhomogeneous and anisotropic magnetized plasma, the dependence of signal propagation characteristics upon initial conditions, etc. Our calculations make possible to follow the wave packets and calculate their properties in the desired regions, e.g. the regions where an efficient wave-particle interaction is expected to occur. We present here the comparison between the distributions obtained with the statistical data sets of wave intensity based also on Cluster observations during several years.

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