Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm53a1348t&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SM53A-1348
Physics
Plasma Physics
[2774] Magnetospheric Physics / Radiation Belts, [7836] Space Plasma Physics / Mhd Waves And Instabilities, [7859] Space Plasma Physics / Transport Processes, [7867] Space Plasma Physics / Wave/Particle Interactions
Scientific paper
We compare several scenarios of radial transport and energization in the radiation belts as electrons become drift-resonant with ultra-low-frequency (ULF) Pc4-Pc5 waves. For the initial setup we have used a simple compressed field profile with toroidally propagating waves. The accumulated potential over each electron drift orbit is significant if the orbit period is in the vicinity of the resonance with a wave, thus a radial transport may be experienced as a result. Since the first adiabatic invariant is conserved, the energy of the electron will shift as well. For individual toroidal modes, the overall energy shift of the electrons has a dependency on initial azimuthal distribution with highest effect at dusk and dawn sides, with some asymmetry. Poloidal modes produce a stronger effect, but we limit these waves to certain regions. In the presence of multiple modes and provided the Chirikov criterion is met, some electrons experience much larger change in energy. The effect is further examined after adding a third or more waves. Finally we present electron acceleration during historical intervals of ULF wave observations during the passage of geoeffective interplanetary structures such as high-speed streams and interplanetary coronal mass ejections. For those more complex events a Tsyganenko-96 model provides the magnetic field as it is driven with time-dependent interplanetary plasma key parameters.
Huang Chan Chun
Koepke Mark E.
Tornquist Mattias
Vassiliadis Dimitris
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