Evolution of energetic electron pitch angle distributions during storm time electron acceleration to megaelectronvolt energies

By R. Horne, Nigel P. Meredith, R. Thorne, D. Heynderickx, R. Iles, R. R. Anderson. 2003

153 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/244cf2e649b087c554b1ac825f95375410e8c8f4

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. Jacob Bortnik
7. Binbin Ni
8. S. Glauert

In Molecular Biology

1. R. Thorne
2. Wen Li
3. R. Horne
4. Y. Shprits
5. Nigel P. Meredith
6. Jacob Bortnik
7. S. Glauert
8. J. Fennell

Citations in the corpus

• 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].”
• Statistical analysis of relativistic electron energies for cyclotron resonance with EMIC waves observed on CRRES (2003, background): “…, 2001; Mathie and Mann , 2001; Meredith et al. , 2001, 2002a, 2002b, 2003; O’Brien et al. , 2001; Friedel et al. , 2002; Summers et al. , 2002; Horne et al. , 2003; Miyoshi et al. , 2003], due in part to the potentially serious hazard posed by enhanced fluxes of relativistic electrons to…”
• Dynamic evolution of energetic outer zone electrons due to wave‐particle interactions during storms (2007, background): “There has been considerable, recent effort directed toward understanding the processes responsible for storm time acceleration of relativistic electrons [e.g., Li et al., 1997; Elkington et al., 1999; Meredith et al., 2002, 2003b; O’Brien et al., 2001; Horne et al., 2003; Miyoshi et al., 2003].”
• Timescale for MeV electron microburst loss during geomagnetic storms (2005, background): “... the rate of energy diffusion maximizes for pitch angles well away from the loss cone [e.g., Horne et al., 2005], while the bounce-averaged pitch angle diffusion rates minimize near the loss cone (Figure 2). Theoretical modeling [Thorne et al., 2005] has shown that the combined effect of pitch an”
• Favored regions for chorus‐driven electron acceleration to relativistic energies in the Earth's outer radiation belt (2003, background): “…in support of this mechanism has come from the energy-dependence of the spectral hardening [Meredith et al., 2002b; Summers et al., 2002] and the energy-dependent flat-topped pitch angle distributions [Horne et al., 2003a] observed during the recovery phase of the October 9, 1990 magnetic storm.”
• Energization of relativistic electrons in the presence of ULF power and mev microbursts: Evidence for dual ULF and VLF acceleration (2003, methodology): “In this scenario, the chorus interaction described in the literature [e.g., Horne and Thorne, 1998; Summers et al., 1998, 2001; Summers and Ma, 2000a; Meredith et al., 2001, 2002a, 2002b; Horne et al., 2003] would result primarily in loss, rather than acceleration.”
• Substorm dependence of plasmaspheric hiss (2004, methodology): “Since the minimum resonant energy decreases with increasing L, the data here suggest that the outer boundary of the quiet time slot region should be found at progressively higher L values for decreasing energies, as previously observed [e.g., Lyons et al., 1972; Horne et al., 2003a].”
• Relativistic electron acceleration and precipitation during resonant interactions with whistler‐mode chorus (2003, background): “Existing bounce-average scattering codes [e.g., Lyons, 1974; Albert, 1999] are not able to treat resonant interactions between electrons and chorus emission in the low density limit, although local diffusion rates have recently been evaluated [Horne et al., 2003b].”
• A statistical look at plasmaspheric drainage plumes (2008, background): “pitch-angle scatter relativistic electrons are plasmaspheric hiss [Horne et al., 2003; Meredith et al., 2004], whistlermode chorus [Tsurutani and Smith, 1974, 1977; Smith et al.”
• Corotating solar wind streams and recurrent geomagnetic activity: A review (2006, unknown): “It is believed that the frequency ‘‘gap’’ is due to Landau absorption [Tsurutani and Smith, 1974; Coroniti et al., 1984; Lauben et al., 2002; see also Horne et al., 2003].”
• THEMIS analysis of observed equatorial electron distributions responsible for the chorus excitation (2010, background): “…understand the global distribution of chorus excitation and its effect on energetic radiation belt electrons [Meredith et al., 2001; Summers et al., 2002; Horne and Thorne, 2003; Horne et al., 2003b, 2005; Meredith et al., 2003; Albert, 2005; Li et al., 2007; Thorne et al., 2007; Li et al., 2009a].”
• Dynamics of the Earth’s Particle Radiation Environment (2009, background): “…magnetic activity outside the plasmasphere (Meredith et al. 2000, 2001, 2003a, 2003b, 2003c) in regions where the ratio of the electron plasma frequency to the electron gyrofrequency is low, which is the condition required for efficient electron diffusion to higher energies (Horne et al. 2003b).”
• Relativistic electron loss timescales in the slot region (2009, background): “Furthermore, as particles are transported from outside the plasmapause to lower L gyroresonant electron acceleration by chorus waves outside the plasmapause would contribute to an initial pitch angle distribution that is peaked near 90 [ Horne et al., 2003 ].”