Anisotropic Turbulent Spectra in the Terrestrial Magnetosheath as Seen by the Cluster Spacecraft

Sahraoui, Fouad; Belmont, Gérard; Rezeau, Laurence; Cornilleau‐Wehrlin, N.; Pinçon, Jean-Louis; Balogh, A.

doi:10.1103/physrevlett.96.075002

Cited by 199 publications

(264 citation statements)

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“…Instead there appears to be a limit on how turbulent these fluctuations can be whether it is due to a limit on the number of modes associated with the fluctuations (as is thought to be the case in the LAPD [15]) or whether there is a limit on how much power can be distributed to higher frequencies (or smaller scales). In SSX, this latter issue may arise due to boundary or temporal development limits, both of which are not encountered by solar wind plasma (but may be relevant for the more bounded turbulent system of the magnetosheath [38,39], for example). The results of the CH plane analysis highlight that more work is needed to push laboratory plasma turbulence research into the fully developed regime.…”

Section: Ch Comparison Of Ssx Wind and Lapd Datamentioning

confidence: 99%

Permutation entropy and statistical complexity analysis of turbulence in laboratory plasmas and the solar wind

et al. 2015

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. 2015. Permutation entropy and statistical complexity analysis of turbulence in laboratory plasmas and the solar wind. Phys. Rev. E 91, 023101.PHYSICAL REVIEW E 91, 023101 (2015) Permutation entropy and statistical complexity analysis of turbulence in laboratory plasmas and the solar wind The Bandt-Pompe permutation entropy and the Jensen-Shannon statistical complexity are used to analyze fluctuating time series of three different turbulent plasmas: the magnetohydrodynamic (MHD) turbulence in the plasma wind tunnel of the Swarthmore Spheromak Experiment (SSX), drift-wave turbulence of ion saturation current fluctuations in the edge of the Large Plasma Device (LAPD), and fully developed turbulent magnetic fluctuations of the solar wind taken from the Wind spacecraft. The entropy and complexity values are presented as coordinates on the CH plane for comparison among the different plasma environments and other fluctuation models. The solar wind is found to have the highest permutation entropy and lowest statistical complexity of the three data sets analyzed. Both laboratory data sets have larger values of statistical complexity, suggesting that these systems have fewer degrees of freedom in their fluctuations, with SSX magnetic fluctuations having slightly less complexity than the LAPD edge I sat . The CH plane coordinates are compared to the shape and distribution of a spectral decomposition of the wave forms. These results suggest that fully developed turbulence (solar wind) occupies the lower-right region of the CH plane, and that other plasma systems considered to be turbulent have less permutation entropy and more statistical complexity. This paper presents use of this statistical analysis tool on solar wind plasma, as well as on an MHD turbulent experimental plasma.

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Section: Ch Comparison Of Ssx Wind and Lapd Datamentioning

confidence: 99%

Permutation entropy and statistical complexity analysis of turbulence in laboratory plasmas and the solar wind

et al. 2015

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“…Two main similarities with solar wind turbulence emerged from those studies: the turbulence in strongly anisotropic (k k ⊥ ) at subproton and electron scales (Sahraoui et al 2004;Mangeney et al 2006;Sahraoui et al 2006) and kinetic instabilities and nonlinear structures are present (Sahraoui et al 2004;Sahraoui 2008;Alexandrova et al 2008b). Major differences with the solar wind do exist, however, e.g., (i) magnetosheath turbulence evolves in a 'confined' space limited by the bow shock and the magnetopause and these boundaries may influence the anisotropy of the turbulence (Sahraoui et al 2006;Yordanova et al 2008), and, (ii) in contrast to the solar wind, the fluctuations are dominated by zero-frequency compressible fluctuations (e.g., mirror modes Sahraoui et al 2006). In a recent large survey of STAFF waveform data obtained in the magnetosheath, Huang et al (2014) quantified the differences in spectral slopes found in the solar wind and magnetosheath in the magnetic energy spectra between the ion and electrons scales (see Fig.…”

Section: Electron Scale Turbulencementioning

confidence: 99%

Section: Electron Scale Turbulencementioning

confidence: 99%

“…Indeed, only a handful of studies have been carried out in recent years (see e.g., Sahraoui et al 2003Sahraoui et al , 2004Mangeney et al 2006;Sahraoui et al 2006;Alexandrova et al 2008b;Yordanova et al 2008;He et al 2011). Two main similarities with solar wind turbulence emerged from those studies: the turbulence in strongly anisotropic (k k ⊥ ) at subproton and electron scales (Sahraoui et al 2004;Mangeney et al 2006;Sahraoui et al 2006) and kinetic instabilities and nonlinear structures are present (Sahraoui et al 2004;Sahraoui 2008;Alexandrova et al 2008b). Major differences with the solar wind do exist, however, e.g., (i) magnetosheath turbulence evolves in a 'confined' space limited by the bow shock and the magnetopause and these boundaries may influence the anisotropy of the turbulence (Sahraoui et al 2006;Yordanova et al 2008), and, (ii) in contrast to the solar wind, the fluctuations are dominated by zero-frequency compressible fluctuations (e.g., mirror modes Sahraoui et al 2006).…”

Section: Electron Scale Turbulencementioning

confidence: 99%

“…P (ω, k), the main product of the k-filtering technique, has been used in a number of studies and in a number of different ways, including determining three-dimensional dispersion relations in identifying the plasma modes that characterize fluctuations in the magnetosheath (Glassmeier et al 2001;Sahraoui et al 2003Sahraoui et al , 2004, in the high latitude magnetic cusps (Grison et al 2005), in the magnetotail in conjunction with magnetic reconnection (Eastwood et al 2009;Huang et al 2010); and in the solar wind. Three-dimensional wavenumber spectra of turbulence have been produced by integrating over the angular frequencies P (k) = P (ω, k)dω in studies of lowfrequency magnetosheath turbulence (Sahraoui et al 2006), MHD-scale turbulence in the foreshock and solar wind (Narita et al 2006(Narita et al , 2010, and kinetic-scale turbulence in the solar wind (Sahraoui et al 2010b). Constantinescu et al (2006) have used spherical wave decomposition instead of plane waves to locate regions in space where wave generation is occurring.…”

Section: Turbulencementioning

confidence: 99%

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Multipoint observations of plasma phenomena made in space by Cluster

et al. 2015

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Plasmas are ubiquitous in nature, surround our local geospace environment, and permeate the universe. Plasma phenomena in space give rise to energetic particles, the aurora, solar flares and coronal mass ejections, as well as many energetic phenomena in interstellar space. Although plasmas can be studied in laboratory settings, it is often difficult, if not impossible, to replicate the conditions (density, temperature, magnetic and electric fields, etc.) of space. Single-point space missions too numerous to list have described many properties of near-Earth and heliospheric plasmas as measured both in situ and remotely (see http://www.nasa.gov/missions/#.U1mcVmeweRY for a list of NASA-related missions). However, a full description of our plasma environment requires three-dimensional spatial measurements. Cluster is the first, and until data begin flowing from the Magnetospheric Multiscale Mission (MMS), the only mission designed to describe the three-dimensional spatial structure of plasma phenomena in geospace. In this paper, we concentrate on some of the many plasma phenomena that have been studied using data from Cluster. To date, there have been more than 2000 refereed papers published using Cluster data but in this paper we will, of necessity, refer to only a small fraction of the published work. We have focused on a few basic plasma phenomena, but, for example, have not dealt with most of the vast body of work describing dynamical phenomena in Earth's magnetosphere, including the dynamics of current sheets in Earth's magnetotail and the morphology of the dayside high latitude cusp. Several review articles and special publications are available that describe aspects of that research in detail and interested readers are referred to them (see for example, Escoubet et al.

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The turbulence evolution in the high β region of the Earth's foreshock

Pang

Huang

et al. 2013

JGR Space Physics

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[1] In this paper, we study the foreshock turbulence evolution in high β region via both Cluster observation on 29 March 2002 and 1-D hybrid simulation. The quasi-sinusoidal and the irregular wave trains are both detected in this event. The former one is believed to be generated by ion-ion right-hand nonresonant instability due to the right-hand polarization and antisunward propagation in the plasma frame. Since the ion distribution associated with the wave train is more "intermediate" rather than "diffused", we suggest that the wave train reported in this paper can be viewed as a "midstep" of "isolated" and "irregular". From the quasi-sinusoidal to the irregular waveform, the corresponding polarizations appear to transit: right-hand wave of higher frequency (wave number) is substituted by a left-hand wave with lower frequency (wave number) in spacecraft frame. Then the 1-D hybrid simulation is applied for two cases with various velocities to study such polarization transition. By comparing observation results with the simulation, such polarization transition and "inversed cascade" (wave energy transferring from large wave number to small wave number) can be understood as the consequence of decay instability. Although decay instability cannot be initiated in high beta (β > 1) plasma in magnetohydrodynamic theory, such β dependence can be modified by ion kinetic effect. Moreover, it is found that in simulation no matter which right-hand instability is dominant in early stage, left-hand wave will be the prime component of magnetic field disturbance in the final stage.

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Anisotropic Turbulent Spectra in the Terrestrial Magnetosheath as Seen by the Cluster Spacecraft

Cited by 199 publications

References 19 publications

Permutation entropy and statistical complexity analysis of turbulence in laboratory plasmas and the solar wind

Permutation entropy and statistical complexity analysis of turbulence in laboratory plasmas and the solar wind

Multipoint observations of plasma phenomena made in space by Cluster

The turbulence evolution in the high β region of the Earth's foreshock

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