Quantitative prediction of radiation belt electrons at geostationary orbit based on solar wind measurements

By Xinlin Li, M. Temerin, D. N. Baker, G. Reeves, D. Larson. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Space Weather Effects in the Earth’s Radiation Belts (2018, methodology): “Li (2001), using a model based on the radial diffusion equation, quantitatively predicted the electron fluxes at GEO based on solar wind velocity and IMF properties.”
Radial diffusion and MHD particle simulations of relativistic electron transport by ULF waves in the september 1998 storm (2006, methodology): “calculations using semiempirical diffusion coefficients can successfully model MeVelectron fluxes at synchronous orbit [Li et al., 2001].”
A new model for the prediction of Dst on the basis of the solar wind (2002, methodology): “This model has already been applied [Li et al., 2001b] to describe the seasonal variation of magnetic activity as measured byDst.”
Three-dimensional simulations of outer radiation belt electron dynamics including cross-diffusion terms (2010, background): “... as the result of cyclotron wave‐particle interactions [Horne and Thorne, 1998; Summers et al., 1998, 2004, 2007a, 2007b; Roth et al., 1999; Summers and Ma, 2000; Horne et al., 2003a, 2005; L. Li et al., 2005; Iles et al., 2006; Xiao et al., 2006, 2007b, 2009a; Su et al., 2009b], together with in”
Energetic electrons, 50 keV to 6 MeV, at geosynchronous orbit: Their responses to solar wind variations (2005, background): “, Figure 1 of Li et al., 2001b]. A recent statistical study [Reeves et al., 2003] shows that about half of magnetic storms increased the fluxes of relativistic electrons, one quarter decreased the fluxes, and one quarter produced little or no change in the fluxes for 276 moderate and intense geomagn”
THEMIS observations of long‐lived regions of large‐amplitude whistler waves in the inner magnetosphere (2008, background): “Several acceleration mechanisms are known, including impulsive changes in the large-scale magnetic field configuration [Li et al., 2001], drift-resonant interaction with Ultra-Low Frequency (ULF) waves [Elkington et al., 2003; Mann et al., 2004] and Doppler-shifted cyclotronresonant interactions…”
On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake revisited (2010, background): “A notable exception is Li et al. [2005], who studied cross correlation between geosynchronous electron fluxes at different energies as well as the correlation between electron fluxes and solar wind velocity (lagged and unlagged).”
Long term measurements of radiation belts by SAMPEX and their variations (2001, background): “These recurrent high speed solar wind streams are efficient in driving recurrent magnetic storms and enhancing radiation belt electrons [e.g., Baker et al., 2001].”
Modeling of outer radiation belt electrons by multidimensional diffusion process (2009, background): “enhanced ULF waves [Li et al., 1999; Brautigam and Albert, 2000; Li and Temerin, 2001; Li et al., 2001; Li, 2004; Barker et al., 2005; Sarris et al., 2006].”
Relativistic electrons in the outer radiation belt: Differentiating between acceleration mechanisms (2004, background): “…orbit which we refer to as external source acceleration mechanisms [e.g., Elkington et al., 1999; Hudson et al., 2000; Kim et al., 2000; Li et al., 2001; Elkington et al., 2003] and in situ acceleration at L < 6.6 by wave particle interactions, referred to here as internal source…”
The global atmospheric electric circuit and its effects on cloud microphysics (2008, methodology): “…electrons precipitating from the quasitrapped radiation belts in the magnetosphere can dominate over that due to GCR. Measurements of the flux at orbital altitudes, which determines the precipitating flux, with data on its variability in time and latitude have been made by Li et al (2001a, 2001b).”
Calculation of pitch angle and energy diffusion coefficients with the PADIE code (2005, background): “Since increases in the energetic electron flux are related to damage and loss of satellites [e.g., Baker et al., 1998; Baker, 2001] and can change atmospheric chemistry leading to ozone destruction [Thorne, 1977; Callis et al., 1998], it is important to understand the physical processes involved so ”
Radiation Belt Environment model: Application to space weather nowcasting (2008, methodology): “One simple approach is based on a standard radial diffusion equation with diffusion coefficients driven by the solar wind conditions or geomagnetic activity [Li et al., 2001; Albert et al., 2001].”