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Observations and Fokker-Planck Simulations of the L-Shell, Energy, and Pitch Angle Structure of Earth's Electron Radiation Belts During Quiet Times

Ripoll J. -., V. Loridan, M. H. Denton, G. Cunningham, G. Reeves, O. Santolik, J. Fennell, D. L. Turner, A. Y. Drozdov, J. S. Cervantes Villa, Y. Y. Shprits, S. A. Thaller, W. S. Kurth, C. A. Kletzing, M. G. Henderson, A. Y. Ukhorskiy, (2019), Observations and Fokker-Planck Simulations of the L-Shell, Energy, and Pitch Angle Structure of Earth’s Electron Radiation Belts During Quiet Times, J. of Geophys. Res. [Space Physics], 124, 1125-1142, doi:10.1029/2018JA026111

Abstract

Abstract The evolution of the radiation belts in L-shell (L), energy (E), and equatorial pitch angle (α0) is analyzed during the calm 11-day interval (4–15 March) following the 1 March 2013 storm. Magnetic Electron and Ion Spectrometer (MagEIS) observations from Van Allen Probes are interpreted alongside 1D and 3D Fokker-Planck simulations combined with consistent event-driven scattering modeling from whistler mode hiss waves. Three (L, E, α0) regions persist through 11 days of hiss wave scattering; the pitch angle-dependent inner belt core (L ~ ~5 and E~ < 100 keV), and a distinct pocket of electrons (L ~ [4.5, 5.5] and E ~ [0.7, 2] MeV). The pitch angle homogeneous outer belt is explained by the diffusion coefficients that are roughly constant for α0 ~ 100 keV, 3.5 < L < Lpp ~ 6. Thus, observed unidirectional flux decays can be used to estimate local pitch angle diffusion rates in that region. Top-hat distributions are computed and observed at L ~ 3–3.5 and E = 100–300 keV.

Authors (sorted by name)

Cervantes Villa Cunningham Denton Drozdov Fennell Henderson Kletzing Kurth Loridan Reeves Ripoll Santolik Shprits Thaller Turner Ukhorskiy

Journal / Conference

Journal Of Geophysical Research (Space Physics)

Bibtex

@article{doi:10.1029/2018JA026111,
author = {Ripoll, J.-F. and Loridan, V. and Denton, M. H. and Cunningham, G. and Reeves, G. and Santolik, O. and Fennell, J. and Turner, D. L. and Drozdov, A. Y. and Cervantes Villa, J. S. and Shprits, Y. Y. and Thaller, S. A. and Kurth, W. S. and Kletzing, C. A. and Henderson, M. G. and Ukhorskiy, A. Y.},
title = {Observations and Fokker-Planck Simulations of the L-Shell, Energy, and Pitch Angle Structure of Earth's Electron Radiation Belts During Quiet Times},
journal = {Journal of Geophysical Research: Space Physics},
volume = {124},
number = {2},
pages = {1125-1142},
keywords = {radiation belts, wave-particle interactions, electron lifetime, pitch angle diffusion coefficient, hiss waves},
doi = {10.1029/2018JA026111},
url = {https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/2018JA026111},
eprint = {https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2018JA026111},
abstract = {Abstract The evolution of the radiation belts in L-shell (L), energy (E), and equatorial pitch angle (α0) is analyzed during the calm 11-day interval (4–15 March) following the 1 March 2013 storm. Magnetic Electron and Ion Spectrometer (MagEIS) observations from Van Allen Probes are interpreted alongside 1D and 3D Fokker-Planck simulations combined with consistent event-driven scattering modeling from whistler mode hiss waves. Three (L, E, α0) regions persist through 11 days of hiss wave scattering; the pitch angle-dependent inner belt core (L ~  ~5 and E~ < 100 keV), and a distinct pocket of electrons (L ~ [4.5, 5.5] and E ~ [0.7, 2] MeV). The pitch angle homogeneous outer belt is explained by the diffusion coefficients that are roughly constant for α0 ~  100 keV, 3.5 < L < Lpp ~ 6. Thus, observed unidirectional flux decays can be used to estimate local pitch angle diffusion rates in that region. Top-hat distributions are computed and observed at L ~ 3–3.5 and E = 100–300 keV.},
year = {2019}
}