Nonlinear electron magnetohydrodynamics physics. IV. Whistler instabilities

Urrutia, J. M.; Stenzel, R. L.; Strohmaier, K. D.

doi:10.1063/1.2934680

Cited by 12 publications

(4 citation statements)

References 46 publications

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“…These are only a few of the numerous other studies. For more literature, the readers can refer to the simulation work by Biskamp (Biskamp et al 1996) and others, including Shukla (1978), Shukla et al (2001), Cho & Lazarian (2004), Galtier (2008), Urrutia, Stenzel & Strohmaier (2008), Saito et al (2008), Bengt & Shukla (2008), Shaikh (2009), Shaikh & Shukla (2009) and numerous references therein.…”

Section: Introductionmentioning

confidence: 99%

Whistler wave cascades in solar wind plasma

Shaikh

2009

Monthly Notices of the Royal Astronomical Society

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Non-linear, three-dimensional, time-dependent fluid simulations of whistler wave turbulence are performed to investigate role of whistler waves in solar wind plasma turbulence in which characteristic turbulent fluctuations are characterized typically by the frequency and lengthscales that are, respectively, bigger than ion gyrofrequency and smaller than ion gyroradius. The electron inertial length is an intrinsic length-scale in whistler wave turbulence that distinguishably divides the high-frequency solar wind turbulent spectra into scales smaller and bigger than the electron inertial length. Our simulations find that the dispersive whistler modes evolve entirely differently in the two regimes. While the dispersive whistler wave effects are stronger in the large-scale regime, they do not influence the spectral cascades which are describable by a Kolmogorov-like k −7/3 spectrum. By contrast, the small-scale turbulent fluctuations exhibit a Navier-Stokes-like evolution where characteristic turbulent eddies exhibit a typical k −5/3 hydrodynamic turbulent spectrum. By virtue of equipartition between the wave velocity and magnetic fields, we quantify the role of whistler waves in the solar wind plasma fluctuations.

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Section: Introductionmentioning

confidence: 99%

Whistler wave cascades in solar wind plasma

Shaikh

2009

Monthly Notices of the Royal Astronomical Society

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“…These give rise to secondary whistler waves emerging from whistler spheromaks that are described in a separate companion paper. 10 Large amplitude whistler modes are not only of intrinsic interest in nonlinear wave physics but are also relevant to the understanding of strong turbulence and heating. This is thought to occur in plasmas with weak mean magnetic fields; for example, magnetic reconnection geometries, 11,12 laserproduced plasmas, 2 and certain space plasmas.…”

Section: Introductionmentioning

confidence: 99%

Nonlinear electron magnetohydrodynamics physics. II. Wave propagation and wave-wave interactions

2008

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The propagation of low-frequency whistler modes with wave magnetic field exceeding the ambient field is investigated experimentally. Such nonlinear waves are excited with magnetic loop antennas whose axial field is aligned with the background magnetic field and greatly exceeds its strength. The oscillatory antenna field excites propagating wave packets with field topologies alternating between whistler spheromaks and mirrors. The propagation speed of spheromaks is observed to decrease with amplitude while that of mirrors increases with amplitude. The field distribution varies with amplitude: Spheromaks contract axially while mirrors spread out compared to linear whistlers. Consequently, the peak magnetic field and current densities in spheromaks exceed that of mirrors. Wave-wave interactions of nonlinear whistler modes is also studied. Counterpropagating spheromaks collide inelastically and form a stationary field-reversed configuration. The radius of the toroidal current ring depends on current and can be larger than that of the loop antenna. A tilted field-reversed configuration precesses in the direction of the electron drift. The free magnetic energy is dissipated in the plasma volume and converted into electron heat.

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“…The oscillations are extracted by smoothing the original waveform and displaying the difference. The oscillations are a nonlinear phenomenon which occur only at large coil currents [15]. They peak when the light has a minimum and hence are not created by fast electrons.…”

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confidence: 99%

Field-Reversed Configurations in an Unmagnetized Plasma

2008

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An oscillating magnetic field is applied with a loop antenna to an unmagnetized plasma. At small amplitudes the field is evanescent. At large amplitudes the field magnetizes the electrons, which allows deeper field penetration in the whistler modes. Field-reversed configurations are formed at each half cycle. Electrons are energized. Transient whistler instabilities produce high-frequency oscillations in the magnetized plasma volume.

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Nonlinear electron magnetohydrodynamics physics. IV. Whistler instabilities

Cited by 12 publications

References 46 publications

Whistler wave cascades in solar wind plasma

Whistler wave cascades in solar wind plasma

Nonlinear electron magnetohydrodynamics physics. II. Wave propagation and wave-wave interactions

Field-Reversed Configurations in an Unmagnetized Plasma

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