Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm33b..08p&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SM33B-08
Physics
[2740] Magnetospheric Physics / Magnetospheric Configuration And Dynamics, [2764] Magnetospheric Physics / Plasma Sheet, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [2788] Magnetospheric Physics / Magnetic Storms And Substorms
Scientific paper
The acceleration of ions of ionospheric and solar wind origin in the near-Earth magnetotail during geomagnetic storms caused by the impact of a coronal mass ejection (CME) and by corotating interaction regions (CIRs) and high-speed streams (HSS)were investigated in this study. For each of the storms examined, a global magnetohydrodynamic (MHD) simulation of the event was run using upstream solar wind and interplanetary magnetic field data. A large-scale kinetic (LSK) particle tracing calculation was then carried out for each event: ions originating from the solar wind and from the ionosphere were launched in the global, time-dependent electric and magnetic fields obtained from the MHD simulation of the event. Ion launches began 2 - 3 hours prior to storm onset and continued well into the main phase of CME-driven storms. For the CIR/HSS storm studied, ion launches began prior to the arrival of the density plug associated with the CIR, and continued into the HSS portion of the storm event. We examined the acceleration of ions in the near-Earth plasma sheet and ring current during the sudden storm commencement during CME-driven storms to the acceleration of ions during the more slowly evolving CIR-driven storms. To do so, we evaluated the effect of various solar wind drivers on ion velocity distribution functions computed throughout the near-Earth tail during each event. Where possible, our simulation results were compared with observations.
El-Alaoui Mostafa
Garg Saurabh
Peroomian Vahé
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