Energetic outer zone electron loss timescalesduring low geomagnetic activity
By Nigel P. Meredith, R. Horne, S. Glauert, R. Thorne, Danny Summers, J. Albert, R. R. Anderson. 2006
214 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Geophysics
View Paper: https://www.semanticscholar.org/paper/72db5cc75ac43756aa13dd95ce222153f828ba3c
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Citations in the corpus
- Resonant scattering of outer zone relativistic electrons by multiband EMIC waves and resultant electron loss time scales (2015, unknown): “D pure pitch angle diffusion simulations [e.g.,Meredith et al., 2006; Thorne et al., 2013; Ni et al., 2013, 2014a, 2014b] by numerically solving the equation ∂f ∂t ¼ 1 T αeq sin 2αeq ∂ ∂αeq T αeq sin 2αeq Dααh i ∂f∂αeq ; (7) NI ET AL.”
- Dynamic evolution of energetic outer zone electrons due to wave‐particle interactions during storms (2007, methodology): “The values are based on work by Horne et al. [2005], Meredith et al. [2004, 2006] , Loto’aniu et al. [2006], Sheeley et al. [2001], Spasojevic ´e t al.[2003], and Shprits et al. [2007].”
- Origins of plasmaspheric hiss (2006, background): “[38] In a recent study Meredith et al. [2006] measured the loss rates of 0.214–1.09 MeV electrons between 3 < L <5 during quiet magnetic conditions.”
- Electron losses from the radiation belts caused by EMIC waves (2014, background): “Furthermore, resonant wave-particle interactions with plasmaspheric hiss contribute to electron loss in the outer radiation belt [Summers et al., 2007; Meredith et al., 2006].”
- Survey of upper band chorus and ECH waves: Implications for the diffuse aurora (2009, background): “This emission is largely responsible for the formation of the slot region [e.g., Lyons and Thorne, 1973;Meredith et al., 2007, 2009], and the quiet time decay of radiation belt electrons in the inner region of the outer radiation belt [Meredith et al., 2006; Summers et al., 2007; Lam et al., 2007].”
- Statistical properties of plasmaspheric hiss derived from Van Allen Probes data and their effects on radiation belt electron dynamics (2015, methodology): “The dash-dotted magenta line shows the previously frequently used Gaussian frequency distribution [e.g., Meredith et al., 2006; Summers et al., 2007; Thorne et al., 2013; Ni et al., 2013, 2014], which is expressed in terms of exp f fmΔf 2h i with the wave frequency corresponding to the maximum wave…”
- Space Weather: Terrestrial Perspective (2007, background): “Recent research results have emphasized how effectively all these seemingly distinct populations and their dynamics are coupled together (Meredith et al., 2006).”
- Earth's Van Allen Radiation Belts: From Discovery to the Van Allen Probes Era (2019, background): “…in controlling radiation belt electron dynamics inside the plasmasphere by causing electron precipitation into the upper atmosphere through pitch angle scattering (Li, Ma, et al., 2015; Lyons & Thorne, 1973; Ma, Li, et al., 2016a; Meredith et al., 2007, 2006; Ni et al., 2013; Thorne et al., 2013b).”
- Timescales for radiation belt electron acceleration and loss due to resonant wave-particle interactions: 1. Theory (2007, background): “EMIC waves and plasmaspheric hiss can also contribute to the scattering loss of radiation belt electrons [Summers and Thorne, 2003; Albert, 2003; Summers et al., 2005; Meredith et al., 2006].”
- Global model of lower band and upper band chorus from multiple satellite observations (2012, background): “…is itself responsible for the formation of the slot region between the inner and outer radiation belts [Lyons and Thorne, 1973; Meredith et al., 2007, 2009] and the quiet time decay of energetic electrons in the outer radiation belt [Meredith et al., 2006a; Summers et al., 2007; Lam et al., 2007].”
- Dynamics of the Earth’s Particle Radiation Environment (2009, background): “The location of the proton belt varies with energy, with the peak flux of >50 MeV protons near L = 1.3, while the flux at lower energies peaks at more outward L shells.”
- Slot region electron loss timescales due to plasmaspheric hiss and lightning‐generated whistlers (2007, methodology): “…days at 1 MeV (Figure 8), consistent with observations and previous estimates using the374 PADIE code with CRRES measurements of plasmaspheric hiss [Meredith et al., 2006a].375 At lower energies, 200 keV, the loss timescales can be faster than a day at L = 4.0 but376 rise to 5 days at L = 3.5…”