Substorm dependence of chorus amplitudes: Implications for the acceleration of electrons to relativistic energies

By Nigel P. Meredith, R. Horne, R. R. Anderson. 2001

510 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/592d9b2811852e6356d4468d8535b4cc48942497

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. Binbin Ni
6. Wen Li
7. Danny Summers
8. Jacob Bortnik

Citations in the corpus

• Bounce‐averaged diffusion coefficients for field‐aligned chorus waves (2006, methodology): “The variations of the wave confinement is taken according to the statistical study of Meredith et al. [2001] .”
• Diffuse auroral electron scattering by electron cyclotron harmonic and whistler mode waves during an isolated substorm (2003, background): “Statistical analysis of upper band chorus taken from the CRRES spacecraft over a year or so show that chorus amplitudes in the 2100– 0600 MLT sector, which is the MLT sector of this event, have the strongest amplitudes within about 5 degrees of the magnetic equator [Meredith et al., 2001].”
• Substorm dependence of plasmaspheric hiss (2004, methodology): “[18] To determine a threshold criterion for ECH waves, we initially inspected the data for orbits 63 to 163 shown in Plate 2 of Meredith et al. [2001] .”
• Global model of lower band and upper band chorus from multiple satellite observations (2012, methodology): “In particular, the gap in the coverage in the region 4 L* 6 for 0800–1200 MLT in global wave models derived from CRRES data [e.g., Meredith et al., 2001, 2003] is filled in, primarily with data from Double Star TC1 and THEMIS.”
• Theory and simulation of the generation of whistler‐mode chorus (2008, unknown): “There have been extensive observations of magnetospheric chorus waves [e.g., see Helliwell, 1965; Tsurutani and Smith, 1974; Burtis and Helliwell, 1976; Anderson and Kurth, 1989; Sazhin and Hayakawa, 1992; Lauben et al., 1998; Meredith et al., 2001; Santolik et al., 2003, 2004, 2005; Kasahara et a”
• Origins of plasmaspheric hiss (2006, background): “[12] Whistler mode chorus waves, which are observed in the low-density region outside of the plasmapause, can fall into the frequency range between 0.1 and 5 kHz [e.g., Meredith et al., 2001 ].”
• Computer simulation of chorus wave generation in the Earth's inner magnetosphere (2007, background): “Results of in situ observation have revealed that whistler-mode chorus emissions [Tsurutani and Smith, 1974] are observed in the dawn side of the Earth’s magnetosphere [Tsurutani and Smith, 1977; Meredith et al., 2001; Kasahara et al., 2005].”
• Statistics of whistler mode waves in the outer radiation belt: Cluster STAFF‐SA measurements (2013, background): “The obtained spatial distributions are consistent with the earlier plasmaspheric hiss observations aboard DE-1 [André et al., 2002; Green et al., 2005] and aboard CRRES [Meredith et al., 2004], and lower band chorus statistics from CRRES [Meredith et al., 2001], THEMIS [Cully et al., 2008; Li et al.”
• Dynamics of the Earth’s Particle Radiation Environment (2009, methodology): “Second, chorus wave power increases with 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…”
• THEMIS observations of long‐lived regions of large‐amplitude whistler waves in the inner magnetosphere (2008, result): “is several mV/m, consistent with previous results [Meredith et al., 2001].”
• Electron losses from the radiation belts caused by EMIC waves (2014, background): “Chorus waves tend to be most significant outside the plasmapause on the dawnside during active conditions [Meredith et al., 2001, 2012; Li et al., 2011].”
• Resonant diffusion of radiation belt electrons by whistler‐mode chorus (2003, background): “5 mV m 1 between L = 3–7 [Meredith et al., 2001] which corresponds (assuming propagation along the magnetic field) to a wave magnetic field amplitude between 0.”
• 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, methodology): “8 jWej, where jWej is the electron gyrofrequency [Tsurutani and Smith, 1974, 1977;Koons and Roeder, 1990;Meredith et al., 2001; Santolik et al., 2003, 2004].”
• Resonant scattering of plasma sheet electrons by whistler‐mode chorus: Contribution to diffuse auroral precipitation (2008, methodology): “08; qlc = 0, quc = 40 , qm = 0, qw = 23 ; BW = 50 pT [Meredith et al., 2001].”