Parametric excitation of electrostatic whistler waves by electron plasma waves

Sharma, R. P.; Tripathi, Y. K.; Al‐Janabi, Abdulhadi; Boswell, Roderick

doi:10.1029/91ja02379

Cited by 13 publications

(3 citation statements)

References 29 publications

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“…These mechanisms can't explain the frequencies and oblique propagation seen in the STEREO data in Breneman et al or in this study. Several studies of correlated Langmuir waves and whistler-mode waves (Kennel et al, 1980;Kellogg et al,1992;Sharma et al, 1992;Ergun et al, 1998)have suggested that either both modes are destabilized by an electron bump-on-tail, or that they may be related by a three-wave decay.…”

Section: Introductionmentioning

confidence: 99%

Narrowband Large Amplitude Whistler-mode Waves in the Solar Wind and Their Association with Electrons: STEREO Waveform Capture Observations

Cattell

Short

Breneman

et al. 2020

ApJ

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Large amplitude (up to 70 mV m−1) whistler-mode waves at frequencies of ∼0.2–0.4 f ce (electron cyclotron frequency) are frequently observed in the solar wind. The waves are obliquely propagating at angles close to the resonance cone, resulting in significant electric fields parallel to the background magnetic field, enabling strong interactions with solar wind electrons. Very narrowband (sinusoidal waveforms) and less coherent waves (more irregular waveforms) occur, but do not have a bimodal distribution. Frequencies and/or propagation angles are distinctly different from whistler-mode waves usually observed in the solar wind, and amplitudes are 1–3 orders of magnitude larger. Waves occur most often in association with stream interaction regions, and are often “close-packed.” Wave occurrence as a function of normalized electron heat flux and beta is consistent with the whistler heat flux fan instability for both the narrowband coherent and the incoherent waves. The incoherent waves are associated with zero or near zero heat flux. This suggests that the less coherent waves may be more effective in regulating the electron heat flux, or that the scattering and energization of solar wind electrons by the narrowband waves results in broadening of the waves. The oblique propagation and large amplitudes of both the narrowband and less coherent whistlers enable resonant interactions with electrons over a broad energy range, and, unlike parallel whistlers, do not require that the electrons and waves counter-propagate. Therefore, they are much more effective in modifying solar wind electron distributions than parallel propagating waves.

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Section: Introductionmentioning

confidence: 99%

Narrowband Large Amplitude Whistler-mode Waves in the Solar Wind and Their Association with Electrons: STEREO Waveform Capture Observations

Cattell

Short

Breneman

et al. 2020

ApJ

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“…They propose that these multiple oblique Langmuir modes of different frequencies combine to produce the modulations. This mechanism has gained wide acceptance, and it is usually proposed that the multiple modes are generated through wave‐wave interactions such as decay of a parent Langmuir wave into an oblique Langmuir wave and a VLF wave that might or might not be observable [ Ergun et al , 1991; Sharma et al , 1992; Newman et al , 1994b; Stasiewicz et al , 1996; Bonnell et al , 1997; Lizunov et al , 2001; Khotyaintsev et al , 2001]. Ergun et al [1991] interpret VLF modulations of auroral Langmuir waves as evidence for a transverse modulational instability (MI) resonant with lower hybrid or ion Bernstein modes.…”

Section: Introductionmentioning

confidence: 99%

“… Lizunov et al [2001] present a full dynamical theory of parametric decay of Langmuir waves into oblique Langmuir and lower hybrid waves in the auroral ionospheric context; Umeda and Ito [2008] present simulations interpreted as decay into Langmuir and ion acoustic waves. Other papers discuss Langmuir wave decay into ion acoustic/lower hybrid/whistler waves in other environments such as solar wind and laboratory plasmas [e.g., Cairns and Melrose , 1985; Cairns and Robinson , 1992; Kellogg et al , 1992; Rizzato and Chian , 1992; Sharma et al , 1992]. In particular, it has been shown convincingly that three‐wave decay plays a role in turbulence in the Earth's foreshock [ Robinson and Cairns , 1995; Bale et al , 1996; Kellogg et al , 1999a, 1999b].…”

Section: Introductionmentioning

confidence: 99%

Electric field statistics and modulation characteristics of bursty Langmuir waves observed in the cusp

2010

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[1] HF wave receivers on the Twin Rockets to Investigate Cusp Electrodynamics (TRICE) detect numerous 20-250 ms duration Langmuir wave bursts. Investigation of 41 bursts at 967-984 km, where the gyrofrequency exceeds the plasma frequency, reveals a characteristic signature whereby the Langmuir wave bandwidth and highest frequency maximize at the center of the bursts, suggesting that bursts coincide with density enhancements. The Langmuir waveforms are modulated at frequencies up to 50 kHz, with significant modulation at frequencies <1 kHz about 10% of the time. Where amplitudes of the modulated waves pass through zero, the phase of the carrier wave shifts by 180°, consistent with a superposition of interfering waves. The corresponding wave spectrum has multiple <1 kHz bandwidth peaks separated by <1-50 kHz. For no averaging, the wave E field statistics, dominated by the carrier Langmuir wave, show an E +1 dependence at small E fields as expected for rectified sine waves. For moderate averaging, the statistics, dominated by the envelope field, show a spectral index of ≈ +2 at small E fields, consistent with numerical simulations of independent stochastically driven waves. The wave statistics, absence of VLF waves, lack of transition in the modulation occurrence as a function of frequency, and tendency of the spread spectrum to cut off at the ambient plasma frequency outside the density enhancement associated with the wave burst suggest that linear growth and mixing of Langmuir modes provides a more natural explanation of modulated Langmuir waves than do wave-wave processes previously proposed, at least for cusp waves encountered by TRICE.Citation: LaBelle, J., I. H. Cairns, and C. A. Kletzing (2010), Electric field statistics and modulation characteristics of bursty Langmuir waves observed in the cusp,

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Vortices near the wavy heliospheric current sheet

Drillia

Moussas

1996

Sol Phys

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We study the heliospheric current sheet structure during the 1979-1982 time period, which includes the sunspot maximum of solar cycle 21 and the 1980 reversal of the polar magnetic field of the Sun. We examine the evolution of the large-scale configuration of the heliospheric current sheet (HCS), as calculated by Hoeksema (1991), and its extent in heliographic latitude during this time period.We study the fine-scale characteristics of its structure near sector boundaries (SB) detected in the vicinity of the Earth, using interplanetary magnetic field and solar wind velocity data, as well as temperature measurements (mainly from IMP data). We observe small vortices (eddies) of the order of 0.2 to 0.4 AU in diameter, with time scales of several hours to days. Vortices appear frequently in the plasma near the so-called 'thick' sectors. The local orientation of the sector boundaries is distorted by the presence of vortices. The appearance of vortices is evident in the interplanetary magnetic field, plasma velocity, density, and temperature data.

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Parametric excitation of electrostatic whistler waves by electron plasma waves

Cited by 13 publications

References 29 publications

Narrowband Large Amplitude Whistler-mode Waves in the Solar Wind and Their Association with Electrons: STEREO Waveform Capture Observations

Narrowband Large Amplitude Whistler-mode Waves in the Solar Wind and Their Association with Electrons: STEREO Waveform Capture Observations

Electric field statistics and modulation characteristics of bursty Langmuir waves observed in the cusp

Vortices near the wavy heliospheric current sheet

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