Propagation characteristics of plasmaspheric hiss: Van Allen Probe observations and global empirical models

Yu, Jiahong; Li, L. Y.; Cao, Jinbin; Chen, Lunjin; Wang, Jun; Yang, Junying

doi:10.1002/2016ja023372

Cited by 51 publications

(95 citation statements)

References 37 publications

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“…The wave normal angle (WNA) and polarization ellipticity (Figures c–d) derived from the singular value decomposition (SVD) method (Santolík et al, ) indicate that these emissions are nearly perpendicularly propagating and linearly polarized. These wave properties confirm that the amplified emissions are magnetosonic waves (Yu J et al, ).…”

Section: Observations Of Low‐frequency Ms Wavessupporting

confidence: 78%

“…Magnetosonic (MS) waves, also known as equatorial noise, are predominantly observed near the magnetic equator at frequencies between the proton cyclotron frequency ( f cp ) and the lower hybrid resonance frequency ( f LHR ) both inside and outside the plasmasphere (Russell et al, ; Perraut et al, ; Santolík et al, ; Meredith et al, ; Fu HS et al, ; Posch et al, ; Li LY et al, , b; Yuan ZG et al, ; Liu X et al, ; Liu B et al, ). These waves are mostly linearly polarized; they propagate nearly perpendicular to the background magnetic field (Zhima et al, ; Yu J et al, ; Su ZP et al, ), and they are believed to be excited by proton ring distributions (Horne et al, ; Chen LJ et al, , ; Liu KJ et al, ; Xiao FL et al, ). Recently, MS waves have caught much attention because, by resonating with particles, they play a crucial role in radiation belt dynamics.…”

Section: Introductionmentioning

confidence: 99%

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Ring current proton scattering by low-frequency magnetosonic waves

Wang

Cui

2019

Earth and Planetary Physics

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Magnetosonic (MS) waves are believed to have the ability to affect the dynamics of ring current protons both inside and outside the plasmasphere. However, previous studies have focused primarily on the effect of high‐frequency MS waves (f > 20 Hz) on ring current protons. In this study, we investigate interactions between ring current protons and low‐frequency MS waves (< 20 Hz) inside the plasmasphere. We find that low‐frequency MS waves can effectively accelerate < 20 keV ring current protons on time scales from several hours to a day, and their scattering efficiency is comparable to that due to high‐frequency MS waves (>20 Hz), from which we infer that omitting the effect of low‐frequency MS waves will considerably underestimate proton depletion at middle pitch angles and proton enhancement at large pitch angles. Therefore, ring current proton modeling should take into account the effects of both low‐ and high‐frequency MS waves.

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Section: Observations Of Low‐frequency Ms Wavessupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

Ring current proton scattering by low-frequency magnetosonic waves

Wang

Cui

2019

Earth and Planetary Physics

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“…The PP position ( L pp ) is roughly marked out by the red vertical line in Figures c–h. Inside the plasmasphere ( L < L pp ), there is plasmaspheric hiss whose frequency ( f ) is above the lower hybrid resonance frequency ( f LHR ) (Li et al, ; Yu et al, , ). However, the power spectral density of electric field from the high‐frequency receiver indicates that there is no electrostatic electron cyclotron harmonic waves inside the plasmapause ( L < L pp ).…”

Section: Van Allen Probe Observations and Numerical Validationmentioning

confidence: 99%

The Rapid Responses of Magnetosonic Waves to the Compression and Expansion of Earth's Magnetosphere

Liu

et al. 2017

Geophysical Research Letters

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Under different solar wind dynamic pressures, we observed the magnetosonic (MS) wave amplification and attenuation associated with the compression and expansion of the Earth's magnetosphere. By analyzing the wave and particle variations recorded by the twin Van Allen Probes, we found that the magnetospheric compression or expansion can alter the keV proton phase space density distribution in velocity space and thus affects the MS wave intensity in upper band (f > 50 Hz) in the dawnside magnetosphere (magnetic local time ~ 4.0–7.9 and L ~ 5.7–3.0). During the magnetospheric compression period, the reduction of the 0.1 to 2 keV protons and the enhancement of the 3 to 7 keV protons form a positive phase space density gradient in their velocity space (i.e., the proton ring distribution), and meanwhile, the upper band MS waves are significantly amplified in the proton ring distribution region. During the subsequent magnetospheric expansion period, the enhancement of the 0.1 to 2 keV protons and the reduction of the protons above 3 keV produce a negative phase space density gradient in their velocity space, and meanwhile, the upper band MS waves are rapidly damped. These observations demonstrate that the intensity of the upper band MS waves in the dawnside magnetosphere is highly variable during the change in solar wind pressure.

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“…Falkowski et al () studying dayside sector plasmaspheric hiss found that the waves were associated with both substorms and solar wind pressure pulses (for solar wind pressure effects, see also Gail & Inan, ; Kokubun, ; Shinbori et al, ; Tsurutani et al, , ; Remya et al, ; Yue et al, ). The substorm‐dependent scenario is that substorm‐injected electrons gradient drift from their midnight sector injection to the dayside magnetosphere, generate chorus there (Meredith et al, ; Tsurutani & Smith, , ), and the waves then propagate into the plasmasphere (Bortnik et al, ; Bortnik, Li, et al, ; Bortnik, Thorne, et al, ; Breneman et al, ; L. Chen et al, ; Li et al, ; Li, Chen, et al, ; Santolik, ; Santolik & Chum, ; Thorne et al, , ; Tsurutani et al, ).…”

Section: Introductionmentioning

confidence: 99%

Plasmaspheric Hiss: Coherent and Intense

et al. 2018

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Low frequency (LF) ~22 Hz to 200 Hz plasmaspheric hiss was studied using a year of Polar plasma wave data occurring during solar cycle minimum. The waves are found to be most intense in the noon and early dusk sectors. When only the most intense LF (ILF) hiss was examined, they are found to be substorm dependent and most prominent in the noon sector. The noon sector ILF waves were also determined to be independent of solar wind ram pressure. The ILF hiss intensity is independent of magnetic latitude. ILF hiss is found to be highly coherent in nature. ILF hiss propagates at all angles relative to the ambient magnetic field. Circular, elliptical, and linear/highly elliptically polarized hiss have been detected, with elliptical polarization the dominant characteristic. A case of linear polarized ILF hiss that occurred deep in the plasmasphere during geomagnetic quiet was noted. The waveforms and polarizations of ILF hiss are similar to those of intense high frequency hiss. We propose the hypothesis that ~10–100 keV substorm injected electrons gradient drift to dayside minimum B pockets close to the magnetopause to generate LF chorus. The closeness of this chorus to low altitude entry points into the plasmasphere will minimize wave damping and allow intense noon‐sector ILF hiss. The coherency of ILF hiss leads the authors to predict energetic electron precipitation into the mid latitude ionosphere and the electron slot formation during substorms. Several means of testing the above hypotheses are discussed.

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Propagation characteristics of plasmaspheric hiss: Van Allen Probe observations and global empirical models

Cited by 51 publications

References 37 publications

Ring current proton scattering by low-frequency magnetosonic waves

Ring current proton scattering by low-frequency magnetosonic waves

The Rapid Responses of Magnetosonic Waves to the Compression and Expansion of Earth's Magnetosphere

Plasmaspheric Hiss: Coherent and Intense

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