Dispersion relation analysis of solar wind turbulence

Narita, Yasuhito; Gary, S. Peter; Saito, Shinji; Glaßmeier, Karl‐Heinz; Motschmann, U.

doi:10.1029/2010gl046588

Cited by 106 publications

(116 citation statements)

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“…The transition range around ion scales is also characterized by magnetic fluctuations with quasi-perpendicular wave-vectors k ⊥ > k and a plasma frame frequency close to zero (Sahraoui et al 2010;Narita et al 2011;Roberts et al 2013). Sahraoui et al (2010) interpret these observations as KAW turbulence, although Narita et al (2011) found no clear dispersion relation.…”

Section: Turbulence Around Ion Scalesmentioning

confidence: 88%

“…Sahraoui et al (2010) interpret these observations as KAW turbulence, although Narita et al (2011) found no clear dispersion relation. Magnetic fluctuations with nearly zero frequency and k ⊥ k can also be due to non-propagative coherent structures like current sheets (Veltri et al 2005;Greco et al 2010;Perri et al 2012), shocks (Salem 2000;Veltri et al 2005;Mangeney et al 2001), current filaments (Rezeau et al 1993), or Alfvén vortices propagating with a very slow phase speed ∼ 0.1V A in the plasma frame (Petviashvili and Pokhotelov 1992;Alexandrova 2008).…”

Section: Turbulence Around Ion Scalesmentioning

confidence: 96%

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Solar Wind Turbulence and the Role of Ion Instabilities

et al. 2013

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Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In addition to the presence of magnetic field, the differences with neutral fluid isotropic turbulence are: (i) weakness of collisional dissipation and (ii) presence of several characteristic space and time scales. In this paper we discuss observational properties of solar wind turbulence in a large range from the MHD to the electron scales. At MHD scales, within the inertial range, turbulence cascade of magnetic fluctuations develops mostly in the plane perpendicular to the mean field, with the Kolmogorov scaling k −5/3 ⊥ for the perpendicular cascade and k −2 for the parallel one. Solar wind turbulence is compressible in nature: density fluctuations at MHD scales have the Kolmogorov spectrum. Velocity fluctuations do not follow magnetic field ones: their spectrum is a power-law with a −3/2 spectral index. Probability distribution functions of different plasma parameters are not Gaussian, indicating presence of intermittency. At the moment there is no global model taking into account all these observed properties of the inertial range. At ion scales, turbulent spectra have a break, compressibility increases and the density fluctuation spectrum has a local flattening. Around ion scales, magnetic spectra are variable and ion instabilities occur as a function of the local plasma parameters. Between ion and electron scales, a small scale turbulent cascade seems to be established. It is characterized by a well defined power-law spectrum in magnetic and density fluctuations with a spectral index close to −2.8. Approaching electron scales, the fluctuations are no more self-similar: an exponential cut-off is usually observed (for time intervals without quasi-parallel whistlers) indicating an onset of dissipation. The small scale inertial range between ion and electron scales and the electron dissipation range can be together described by ∼ k −α ⊥ exp(−k ⊥ d ), with α 8/3 and the dissipation scale d close to the electron Larmor radius d ρ e . The nature of this small scale cascade and a possible dissipation mechanism are still under debate.

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Section: Turbulence Around Ion Scalesmentioning

confidence: 88%

Section: Turbulence Around Ion Scalesmentioning

confidence: 96%

Solar Wind Turbulence and the Role of Ion Instabilities

et al. 2013

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“…Other studies, including those employing the multi-spacecraft k-filtering technique [68,69], have also found that the quasi-perpendicular wavevectors remain energetically dominant in the dissipation range [67,[70][71][72][73][74][75], as in the inertial range. In k-filtering, multi-spacecraft observations (e.g.…”

Section: (A) Review Of Observationsmentioning

confidence: 99%

“…Although this is consistent with linear Maxwell-Vlasov dispersion relations for very oblique KAWs (θ kB 0 = cos(k ·B 0 ) ≈ 88 • ), with such strong obliquities of the ks the results can also be interpreted as indicating the presence of relatively energetic quasi-two-dimensional turbulence. Indeed, Narita et al [71,72,76,77] use essentially the same multi-spacecraft technique, over similar wavenumber ranges, and state that they find no evidence of a linear dispersion relation. They favour an explanation in terms of well-developed strong quasi-two-dimensional turbulence.…”

Section: (A) Review Of Observationsmentioning

confidence: 99%

Anisotropy in solar wind plasma turbulence

Oughton

Matthaeus

Wan

et al. 2015

Phil. Trans. R. Soc. A.

117

113

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One contribution of 11 to a theme issue 'Dissipation and heating in solar wind turbulence' . A review of spectral anisotropy and variance anisotropy for solar wind fluctuations is given, with the discussion covering inertial range and dissipation range scales. For the inertial range, theory, simulations and observations are more or less in accord, in that fluctuation energy is found to be primarily in modes with quasi-perpendicular wavevectors (relative to a suitably defined mean magnetic field), and also that most of the fluctuation energy is in the vector components transverse to the mean field. Energy transfer in the parallel direction and the energy levels in the parallel components are both relatively weak. In the dissipation range, observations indicate that variance anisotropy tends to decrease towards isotropic levels as the electron gyroradius is approached; spectral anisotropy results are mixed. Evidence for and against wave interpretations and turbulence interpretations of these features will be discussed. We also present new simulation results concerning evolution of variance anisotropy for different classes of initial conditions, each with typical background solar wind parameters.

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“…Multispacecraft measurement of solar wind magnetic field fluctuations at the ion gyro-radius or inertial scales often show that the dominant power of fluctuations is in directions of almost perpendicular (to the background magnetic field) propagation (Sahraoui et al 2010;Narita et al 2011;Roberts et al 2013). A less powerful parallel propagating component may also exist (He et al 2011;Podesta and Gary 2011).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Ion Dynamics During the Parametric Instabilities of a Left-Hand Polarized Alfvén Wave in a Proton-Electron-Alpha Plasma

Gao

et al. 2013

ApJ

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The parametric instabilities of an Alfvén wave in a proton-electron plasma system are found to have great influence on proton dynamics, where part of the protons can be accelerated through the Landau resonance with the excited ion acoustic waves, and a beam component along the background magnetic field is formed. In this paper, with a onedimensional hybrid simulation model, we investigate the evolution of the parametric instabilities of a monochromatic left-hand polarized Alfvén wave in a proton-electron-alpha plasma with a low beta. When the drift velocity between the protons and alpha particles is sufficiently large, the wave numbers of the backward daughter Alfvén waves can be cascaded toward higher values due to the modulational instability during the nonlinear evolution of the parametric instabilities, and the alpha particles are resonantly heated in both the parallel and perpendicular direction by the backward waves. On the other hand, when the drift velocity of alpha particles is small, the alpha particles are heated in the linear growth stage of the parametric instabilities due to the Landau resonance with the excited ion acoustic waves. Therefore, the heating occurs only in the parallel direction, and there is no obvious heating in the perpendicular direction. The relevance of our results to the preferential heating of heavy ions observed in the solar wind within 0.3 AU is also discussed in this paper.

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Dispersion relation analysis of solar wind turbulence

Cited by 106 publications

References 20 publications

Solar Wind Turbulence and the Role of Ion Instabilities

Solar Wind Turbulence and the Role of Ion Instabilities

Anisotropy in solar wind plasma turbulence

Ion Dynamics During the Parametric Instabilities of a Left-Hand Polarized Alfvén Wave in a Proton-Electron-Alpha Plasma

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