Electron acceleration in the Van Allen radiation belts by fast magnetosonic waves

By R. Horne, R. Thorne, S. Glauert, Nigel P. Meredith, D. Pokhotelov, O. Santolík. 2007

381 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/6d2e9b721f55e06363e688e1a76aa70be23dbe00

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In Astronomy and Astrophysics

1. R. Thorne
2. R. Horne
3. Nigel P. Meredith
4. Wen Li
5. Jacob Bortnik
6. S. Glauert
7. Y. Shprits
8. Binbin Ni

In Atmospheric Science

1. R. Thorne
2. Nigel P. Meredith
3. R. Horne
4. Jacob Bortnik
5. S. Glauert
6. I. Usoskin
7. G. Kovaltsov
8. E. Flückiger

Citations in the corpus

• Modeling radiation belt electron dynamics during GEM challenge intervals with the DREAM3D diffusion model (2013, background): “…interactions that violate the first adiabatic invariant [Horne and Thorne, 1998; Meredith et al., 2002; Horne et al., 2005], for example the heating from whistler mode chorus and magnetosonic waves [Temerin et al., 1994; Li et al., 1997; Summers et al., 1998; Horne et al., 2007; Liu et al., 2011].”
• Origin of energetic electron precipitation >30 keV into the atmosphere (2010, background): “…diffusion does not always extend into the loss cone, for example, magnetosonic waves, which can occur in the same frequency range as parallel propagating whistler mode waves, only scatter electrons at very large pitch angles and thus do not contribute to precipitation directly [Horne et al., 2007].”
• Statistical properties of plasmaspheric hiss derived from Van Allen Probes data and their effects on radiation belt electron dynamics (2015, background): “…with frequencies below the lower hybrid resonance frequency having wave normal angles (Figure 1g) larger than 80° and ellipticity (Figure 1f) between 0.2 and 0.2, since magnetosonic waves typically have wave normal angles close to ~90° and very low ellipticity near 0 [e.g., Horne et al., 2007].”
• Global simulation of magnetosonic wave instability in the storm time magnetosphere (2010, background): “[3] Equatorial MS waves can also influence radiation belts dynamics during active periods, leading to local electron acceleration from ∼10 keV up to a few MeV in the outer radiation belts [Horne et al., 2007].”
• Transit time scattering of energetic electrons due to equatorially confined magnetosonic waves (2010, methodology): “Both Figures 4a and 4b exhibit a broad maximum centered between ∼100 keV and 1 MeV, at a0 ∼ 50°–70°, with values of ∼10−5 s−1, that are primarily produced by the Landau resonance, and are comparable to the values obtained using quasilinear theory [Horne et al., 2007].”
• The Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) on RBSP (2013, methodology): “…for the local acceleration to relativistic energies during the recovery phase of a storm include cyclotron resonant interactions with VLF chorus in the low-density region just outside the plasmapause (Horne et al. 2005) and Landau resonance with equatorial magnetosonic waves (Horne et al. 2007).”
• Particle Dynamics in the Earth's Radiation Belts: Review of Current Research and Open Questions (2020, background): “11 of 48 angle diffusion concentrated around a narrow range of intermediate to high pitch angles at energies above 100 keV (e.g., Albert et al., 2016) and with some events responsible for particle acceleration (e.g., Horne et al., 2007).”
• Three‐dimensional electron radiation belt simulations using the BAS Radiation Belt Model with new diffusion models for chorus, plasmaspheric hiss, and lightning‐generated whistlers (2014, background): “For example, magnetosonic waves can accelerate electrons between ∼ 10 keV and a few MeV in the outer radiation belt on a timescale of 1–2 days for waves with intensities of the order 50,000 pT2 [Horne et al., 2007].”
• Electron losses from the radiation belts caused by EMIC waves (2014, background): “Magnetosonic waves may also lead to local acceleration and may particularly energize electrons with energies between 10 keV up to a few MeV in the outer radiation belt [Horne et al., 2007].”
• On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake revisited (2010, background): ““Local”acceleration processesthat have been studied include linear interaction with VLF whistlers [Summers et al., 1998] nonlinear whistler interactions [Omura et al., 2007], and interaction with other wave modes such as magneosonic waves [ Horne et al., 2007 ].While there is growingconsensus that l”