Substorm dependence of plasmaspheric hiss

By Nigel P. Meredith, R. Horne, R. Thorne, Danny Summers, R. R. Anderson. 2004

361 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/941812c54193a04a35b64541e130ca05244b821b

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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. S. Glauert

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. S. Glauert

Citations in the corpus

• Relativistic electron loss timescales in the slot region (2009, background): “Plasmaspheric hiss can persist during relatively quiet conditions, but the emission intensifies during magnetic storms or substorms [Smith et al., 1974; Thorne et al., 1974, 1977; Meredith et al., 2004 ].”
• Energetic outer zone electron loss timescalesduring low geomagnetic activity (2006, methodology): “Hiss intensities vary as a function of spatial location and magnetic activity [Meredith et al., 2004].”
• Modeling of outer radiation belt electrons by multidimensional diffusion process (2009, background): “Hiss often occurs in higher-density regions associated with the Earth’s plasmasphere and dayside plumes [ Meredith et al., 2004 ].”
• Particle Dynamics in the Earth's Radiation Belts: Review of Current Research and Open Questions (2020, background): “…mode hiss waves are the third main wave of the plasmasphere (e.g., Thorne et al., 1979), acting broadband from (~50 Hz to ~2 kHz) from L ~ 2 up to the plasmapause (Li et al., 2015; Meredith et al., 2004; Meredith, Horne, Clilverd, et al., 2006; Meredith et al., 2018; Tsurutani et al., 2015).”
• Modeling the evolution of chorus waves into plasmaspheric hiss (2011, background): “Although PH occurs at essentially all magnetic local times (MLT) and latitudes within the plasmasphere, there is nevertheless a pronounced MLT asymmetry in wave power, with dayside values being roughly an order of magnitude larger than those on the nightside [Meredith et al., 2004, 2006].”
• Modeling the propagation characteristics of chorus using CRRES suprathermal electron fluxes (2007, methodology): “…we adopt, based on a previous experimental study using data from the CRRES Plasma Wave Experiment, requires that the wave amplitude for frequencies in the range fce f 2 fce be greater than 0.0005 mVm 1 in order for the wave and particle data to be included in the survey [Meredith et al., 2004].”
• Origins of plasmaspheric hiss (2006, methodology): “Figure 7 shows the data organized by geomagnetic activity where AE* is the maximum value of the auroral electrojet index in the previous 3 hours [ Meredith et al., 2004 ].”
• Dynamic evolution of energetic outer zone electrons due to wave‐particle interactions during storms (2007, methodology): “The values are based on work by Horne et al. [2005], Meredith et al. [2004, 2006] , Loto’aniu et al. [2006], Sheeley et al. [2001], Spasojevic ´e t al.[2003], and Shprits et al. [2007].”
• Event‐specific chorus wave and electron seed population models in DREAM3D using the Van Allen Probes (2014, methodology): “For example, the global intensity distributions of chorus waves used in Tu et al. [2013] are statistically derived from the CRRES wave data, which are then binned in AE* (the mean value of AE over the previous 1 h) [Meredith et al., 2003, 2004].”
• Origin of energetic electron precipitation >30 keV into the atmosphere (2010, background): “[16] Meredith et al. [2004] show plasmaspheric hiss generally scatters electrons in the 20 keV to 2 MeV energy range, so hiss is a possible candidate.”
• A statistical look at plasmaspheric drainage plumes (2008, background): “Three candidate plasmaspheric waves that can 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., 2004; Summers et al., 2004], and electromagnetic ioncyclotron (EMIC) waves…”
• Outward radial diffusion driven by losses at magnetopause (2006, background): “Meredith et al. [2004] also demonstrated that the intensity of the hiss and consequently the rate of pitch angle scattering are correlated with the level of geomagnetic activity.”
• Electron scattering by whistler-mode ELF hiss in (2008, background): “Hiss is present over a broad region of the plasmasphere even during geomagnetically quiet periods and intensifies during storms or substorms [Smith et al., 1974; Thorne et al., 1974; Meredith et al., 2004].”
• Timescale for radiation belt electron acceleration by whistler mode chorus waves (2005, background): “Plasmaspheric hiss is mainly confined to within the high-density plasmapause, which is compressed during large geomagnetic disturbances [ Meredith et al., 2004 ].”