Van Allen Probes Bibliography is from August 2012 through September 2021 Notice:

The effect of ULF compressional modes and field line resonances on relativistic electron dynamics
Author  Degeling, A.; Rankin, R.; Kabin, K.; Marchand, R.; Mann, I.R.; 
Keywords  Radial Transport 
Abstract  The adiabatic, driftresonant interaction between relativistic, equatorially mirroring electrons and a ULF compressional wave that couples to a field line resonance (FLR) is modelled. Investigations are focussed on the effect of azimuthal localisation in wave amplitude on the electron dynamics. The ULF wave fields on the equatorial plane (r , φ ) are modelled using a box model [Zhu, X., Kivelson, M.G., 1988. Analytic formulation and quantitative solutions of the coupled ULF wave problem. J. Geophys. Res. 93(A8), 8602\textendash8612], and azimuthal variations are introduced by adding a discrete spectrum of azimuthal modes. Electron trajectories are calculated using drift equations assuming constant magnetic moment M , and the evolution of the distribution function f(r,φ,M,t) from an assumed initial condition is calculated by assuming f remains constant along electron trajectories. The azimuthal variation in ULF wave structure is shown to have a profound effect on the electron dynamics once a threshold in azimuthal variation is exceeded. Electron energy changes occur that are significantly larger than the trapping width corresponding to the maximum wave amplitude. We show how this can be explained in terms of the overlap of multiple resonance islands, produced by the introduction of azimuthal amplitude variation. This anomalous energisation is characterised by performing parameter scans in the modulation amplitude ε and the wave electric field. A simple parametric model for the threshold is shown to give reasonable agreement with the threshold observed in the electron dynamics model. Above the threshold, the radial transport averaged over φ is shown to become diffusive in nature over a timescale of about 25 wave periods. The anomalous energisation described in this paper occurs over the first 15 wave periods, indicating the importance of convective transport in this process. 
Year of Publication  2007 
Journal  Planetary and Space Science 
Volume  55 
Number of Pages  731742 
Section  
Date Published  04/2007 
ISBN  
URL  http://www.sciencedirect.com/science/article/pii/S0032063306002893 
DOI  10.1016/j.pss.2006.04.039 