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. 2016 Sep 28;7:12883. doi: 10.1038/ncomms12883

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Copyright © 2016, The Author(s)

This work is licensed under a Creative Commons Attribution 4.0 International License. The images or other third party material in this article are included in the article's Creative Commons license, unless indicated otherwise in the credit line; if the material is not included under the Creative Commons license, users will need to obtain permission from the license holder to reproduce the material. To view a copy of this license, visit http://creativecommons.org/licenses/by/4.0/

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All panels show the flux of electrons at 85° equatorial pitch angle as a function of radial distance and day of January 2013. The output of numerical simulations accounting for radial transport and scattering by VLF waves but without EMIC wave scattering are shown for (a) 1.02 MeV and (b) 4.2 MeV electrons. The output of numerical simulations similar to the first row but now with additional scattering by EMIC waves are shown for (c) 1.02 MeV and (d) 4.2 MeV electrons. Observations of electron flux from the MagEIS and REPT instruments on the Van Allen Probes spacecraft are shown for (e) 1.02 MeV and (f) 4.2 MeV electrons. The white lines in e and f show the plasmapause location. Observations show an increase in electron flux at MeV energies (e) and a decrease at ultra-relativistic energies (f). The numerical simulations including EMIC waves successfully reproduce the evolution of both of these electron populations (c,d).