Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm11b1723y&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SM11B-1723
Physics
[2730] Magnetospheric Physics / Magnetosphere: Inner, [2774] Magnetospheric Physics / Radiation Belts
Scientific paper
We perform test particle simulations of energetic electrons interacting with whistler mode chorus emissions. Chorus waves propagate from the geomagnetic equator in both northward and southward directions along the dipole magnetic field. The rapidly increasing frequency and amplitude are determined by model chorus equations. We solve these equations for northward and southward propagating emissions. The source particles are assumed to be located uniformly along magnetic field line, and initial pitch angles at the magnetic equator are assumed to be 10 to 90 degrees. Particles are evenly distributed in gyro-phase, and are assumed to take the form of a delta function in energy and pitch angle. Following interaction with chorus emissions, the calculated distribution function assumes the form of a Green’s function. By repeating this process at different energies and pitch angles, we thereby obtain a numerical Green’s function as a function of energy and pitch angle. We determine the evolution of the distribution function by the interaction of chorus waves and electrons based on this Green’s function method. Through interaction with many chorus elements, which is simulated by the repeated convolution integrals with the numerical Green's function, the distribution function of the injected electrons in the lower energy rage (10keV - 100keV) quickly expands to the higher energy (> 1MeV) and higher pitch angles by the relativistic turning acceleration and the ultra-relativistic acceleration along with the effect of rising tone chorus emissions, resulting in a substantial flux of relativistic electron near the magnetic equator.
Hikishima Mitsuru
Omura Yuji
Summers Donald
Yoshikawa Makoto
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