Acceleration and loss of relativistic electrons during geomagnetic storms

By G. Reeves, K. L. McAdams, R. Friedel, T. P. O'Brien. 2003

804 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/3b355f155340f0d3c9e27637839c9a8e7af9e4ad

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

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

In Geophysics

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

Citations in the corpus

• Energetic electrons, 50 keV to 6 MeV, at geosynchronous orbit: Their responses to solar wind variations (2005, background): “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 geomagnetic storms spanning the 11…”
• Quantification of relativistic electron microburst losses during the GEM storms (2004, background): “[2] Essentially all magnetic storms substantially alter the electron radiation belts, and losses play a major role in that alteration [Reeves et al., 2003].”
• Outward radial diffusion driven by losses at magnetopause (2006, background): “For many storms, fluxes do not return to the original prestorm values, which indicates that nonadiabatic losses occur during storms [McAdams and Reeves, 2001; Onsager et al., 2002; Reeves et al., 2003; Green et al., 2004].”
• Timescale for MeV electron microburst loss during geomagnetic storms (2005, background): “A net increase in MeV electron flux can occur during the recovery of certain storms [Reeves et al., 2003], presumably when source processes dominate over weakened loss mechanisms.”
• Resonant scattering of plasma sheet electrons leading to diffuse auroral precipitation: 2. Evaluation for whistler mode chorus waves (2011, background): “There is considerable theoretical and observational evidence [e.g., Meredith et al., 2002; Reeves et al., 2003; Summers et al., 2002, 2004; Horne et al., 2005a, 2005b; Shprits et al., 2006a; Li et al., 2007; Thorne et al., 2007] that energy diffusion due to chorus is an essential candidate for 2 of…”
• Use of POES SEM-2 observations to examine radiation belt dynamics and energetic electron precipitation into the atmosphere (2010, background): “One of these concerns the physics of the radiation belts, and primarily the evolution of energetic electron fluxes during and after geomagnetic storms [e.g., Reeves et al., 2003].”
• Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “The primary impact of a fast stream appears to be the acceleration of additional energetic electrons in the radiation belts (e.g., Iles et al. 2002; Reeves et al. 2003; Jaynes et al. 2015; Kilpua et al. 2015).”
• Helium, Oxygen, Proton, and Electron (HOPE) Mass Spectrometer for the Radiation Belt Storm Probes Mission (2013, background): “Our ability to quantify these steps will ultimately shape our ability to predict, for example, whether a storm will increase or decrease radiation belt fluxes (Reeves et al. 2003).”
• 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].”