Relativistic electron pitch-angle scattering by electromagnetic ion cyclotron waves during geomagnetic storms

By Danny Summers, R. Thorne. 2003

713 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/75041817047ac52a6af01f7e87d349b1b659f037

How researchers see this paper

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In Astronomy and Astrophysics

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

Citations in the corpus

• Timescales for radiation belt electron acceleration and loss due to resonant wave‐particle interactions: 2. Evaluation for VLF chorus, ELF hiss, and electromagnetic ion cyclotron waves (2007, background): “scattering and precipitation loss can occur over many drift orbits, namely several hours, because EMIC wave amplitudes typically exceed the level for strong diffusion scattering [Summers et al., 1998; Summers and Thorne, 2003].”
• On the storm‐time evolution of relativistic electron phase space density in Earth's outer radiation belt (2013, background): “…chorus [e.g., Horne and Thorne, 2003; O’Brien et al., 2004; Bortnik and Thorne, 2007], whistler waves originating from lightning and ground-based VLF transmitters [e.g., Abel and Thorne, 1998a; 1998b], and electromagnetic ion cyclotron (EMIC) waves [e.g., Summers and Thorne, 2003; Albert, 2003].”
• Electron scattering by whistler-mode ELF hiss in (2008, background): “Scattering by EMIC waves along the duskside plasmasphere can induce precipitation loss of MeV electrons on timescales of several hours to a day [Lorentzen et al., 2000; Summers and Thorne, 2003; Meredith et al., 2003b; Summers et al., 2007b].”
• Substorm dependence of plasmaspheric hiss (2004, background): “Recent theoretical and experimental work has shown that EMIC waves may indeed play an important role in the loss of relativistic electrons during enhanced geomagnetic activity [Lorentzen et al., 2000; Albert, 2003; Meredith et al., 2003b; Summers and Thorne, 2003 ].”
• Nonlinear interaction of radiation belt electrons with electromagnetic ion cyclotron waves (2009, methodology): “The particles were started at the equator with E = 2 MeV, a0 = 15 , and a uniform spread in initial phase, f0.”
• The dual role of ELF/VLF chorus waves in the acceleration and precipitation of radiation belt electrons (2007, background): “Thus, chorus is believed to play an important role as a loss process during the main phase of storms, comparable to other loss processes which also act on the timescale of a day, such as combined scattering by plasmaspheric hiss and EMIC waves (Albert, 2003; Summers and Thorne, 2003) as well as radi”
• Calculation of pitch angle and energy diffusion coefficients with the PADIE code (2005, methodology): “density approximation, which simplifies the calculation considerably [e.g., Lyons et al., 1972; Albert, 1999, 2003; Summers and Thorne, 2003 ].”
• Energetic outer zone electron loss timescalesduring low geomagnetic activity (2006, background): “Farther out, but remaining inside the plasmapause, resonant interactions with both plasmaspheric hiss and electromagnetic ion cyclotron (EMIC) waves are believed to dominate [Thorne et al., 1973; Lyons et al., 1972; Albert, 1994; Summers and Thorne, 2003; Summers, 2005].”
• Outward radial diffusion driven by losses at magnetopause (2006, background): “For the same events as described in section 2, HEO observations show that all channels, (including E > 0.13 and E > 0.23 MeV) are depleted down to L = 4 during the main phases of the strong storms.”
• THEMIS analysis of observed equatorial electron distributions responsible for the chorus excitation (2010, background): “drift time is several hours [Chen and Schulz, 2001a, 2001b], which is considerably larger than the timescale ( Summers and Thorne, 2003 ].”
• A statistical look at plasmaspheric drainage plumes (2008, background): “cyclotron (EMIC) waves [Summers and Thorne, 2003; Meredith et al., 2003].”
• Timescale for radiation belt electron acceleration by whistler mode chorus waves (2005, background): “Electron losses due to EMIC waves can be significant [ Summers and Thorne, 2003; Albert, 2003], but they are generally confined to electron energies greater than � 1 MeV [Meredith et al., 2003b].”
• Precipitation of radiation belt electrons by EMIC waves, observed from ground and space (2008, methodology): “Awave spectrum with a wave power peak and band width obtained from observation (Figure 2), and a typical EMIC wave amplitude of 1 nT, were assumed [Summers and Thorne, 2003; Albert, 2003].”
• Space Weather Effects in the Earth’s Radiation Belts (2018, background): “Finally, EMIC waves are known to interact strongly with highly energetic electrons in the MeV range, particularly during active storm times (Albert 2003; Summers and Thorne 2003).”
• Effect of EMIC waves on relativistic and ultrarelativistic electron populations: Ground‐based and Van Allen Probes observations (2014, background): “…energy of relativistic electrons interacting with EMIC waves is very sensitive to the ratio of local plasma density to the magnetic field strength and, in the cold multi-ion plasma approximation, to the proximity of the wave frequency to ion gyrofrequencies [e.g., Summers and Thorne, 2003].”
• Differences between CME‐driven storms and CIR‐driven storms (2006, background): “…17 A07S08 the magnetosphere that are thought to be important for the physics of storms, such as whistler-mode chorus [Villalon and Burke, 1995; Smith et al., 2004], electromagnetic ion cyclotron waves [Jordanova et al., 1998; Summers and Thorne, 2003], and plasmaspheric hiss [Horne et al., 2003].”