On the source location of radiation belt relativistic electrons

By R. Selesnick, J. Bernard Blake. 2000

176 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/7f1b2122624bdcfa1c6fcec810a6a153e2c45146

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In Astronomy and Astrophysics

Citations in the corpus

Origin of energetic electron precipitation >30 keV into the atmosphere (2010, methodology): “The bow tie method is defined by Selesnick and Blake [2000] and”
Quantitative prediction of radiation belt electrons at geostationary orbit based on solar wind measurements (2001, background): “…at a given µ and J usually increases with increasing radial distance, the usual effect of radial diffusion is to increase the flux at smaller radial distances, by radially diffusing electrons from larger distances while preserving their first two adiabatic invariants [Selesnick and Blake, 2000].”
Acceleration mechanism responsible for the formation of the new radiation belt during the 2003 Halloween solar storm (2006, background): “Losses to themagnetopause during themain phase of a storm [Selesnick and Blake, 2000] may also contribute to net loss by creating inward gradients in phase space density which transport electrons outward.”
Event‐specific chorus wave and electron seed population models in DREAM3D using the Van Allen Probes (2014, background): “Given that the variability of radiation belt electrons is a delicate balance between various source and loss processes [Selesnick and Blake, 2000; Reeves et al., 2003; Tu et al., 2009], understanding the fast dropout and buildup of radiation belt electrons in this event is challenging even with the ”
Explaining sudden losses of outer radiation belt electrons during geomagnetic storms (2012, background): “Figure S4: NOAA-POES combined data for the 25 June 2008 storm and dropout studied by Loto’aniu et al. [2010]. The minimum magnetopause distance during this event was ~8.”
Resonant diffusion of radiation belt electrons by whistler‐mode chorus (2003, background): “…include the relatively long timescale for inward particle transport [Miyoshi et al., 2003], local peaks in the phase space density near L = 4 [Selesnick and Blake, 2000], flat topped pitch-angle distributions observed during acceleration events [Horne et al., 2003], and the energy dependence…”
Modeling radiation belt electron dynamics during GEM challenge intervals with the DREAM3D diffusion model (2013, background): “The variability of radiation belt electrons is controlled by the competition between source and loss processes [Selesnick and Blake, 2000; Reeves et al., 2003; Li, 2004; Fu et al., 2011].”
Earth's Van Allen Radiation Belts: From Discovery to the Van Allen Probes Era (2019, background): “A source term S, either at the outer boundary, corresponding to plasma sheet injections which provide a source population beyond geosynchronous orbit, or internal to represent localized gyroresonant heating, can be included on the right‐hand side of equation (1) (Selesnick & Blake, 2000).”
Energization of relativistic electrons in the presence of ULF power and mev microbursts: Evidence for dual ULF and VLF acceleration (2003, background): “Selesnick and Blake [2000] used a variety of magnetic field models to determine whether there was evidence for meaningful L structure in electron phase”