Intermittent character of interplanetary magnetic field fluctuations

Bruno, R.; Carbone, V.; Chapman, Sandra C.; Hnat, B.; Noullez, A.; Sorriso‐Valvo, L.

doi:10.1063/1.2711429

Cited by 29 publications

(17 citation statements)

References 35 publications

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“…53. However, Bruno et al (2007), providing further evidence of such behavior, can only offer the strong suggestion of a trend that would be difficult to prove in all generality. Although suggested by the authors, given the fact that magnetic power tends to dominate over velocity fluctuations as demonstrated repeatedly by determinations of the Alfvén ratio, it is difficult to entertain the notion that magnetic field turbulence in the solar wind behaves as a passive scalar.…”

Section: Intermittency In the Solar Windmentioning

confidence: 90%

“…This limitation does introduce constraints which makes the statistical testing of different intermittency models that predict different deviations from the p/3 law quite difficult. An intriguing recent result concerning the roles that are played, respectively, by the solar wind itself and the embedded interplanetary magnetic field in interplanetary turbulence has been published recently (Bruno et al 2007). It has been found earlier that the magnetic its temperature field ( , advected as a scalar field in the flow) and for the solar wind speed (u) and the interplanetary magnetic field magnitude (b).…”

Section: Intermittency In the Solar Windmentioning

confidence: 98%

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Turbulence in the Solar Atmosphere and Solar Wind

Petrosyan

Balogh

Goldstein³

et al. 2010

Space Sci Rev

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The objective of this review article is to critically analyze turbulence and its role in the solar atmosphere and solar wind, as well as to provide a tutorial overview of topics worth clarification. Although turbulence is a ubiquitous phenomenon in the sun and its heliosphere, many open questions exist concerning the physical mechanisms of turbulence generation in solar environment. Also, the spatial and temporal evolution of the turbulence A. Petrosyan ( ) Space Research Institute of the Russian Academy Sciences,

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Section: Intermittency In the Solar Windmentioning

confidence: 90%

Section: Intermittency In the Solar Windmentioning

confidence: 98%

Turbulence in the Solar Atmosphere and Solar Wind

Petrosyan

Balogh

Goldstein³

et al. 2010

Space Sci Rev

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“…A key objective of the present work is to relate some aspects of the Ulysses solar wind measurements: their spectral power density, intermittency (Bruno et al 2003(Bruno et al , 2007, and spatial location. Generalizing somewhat, the solar wind spectral power density is observed to scale approximately as f À1 (Ruzmaikin et al 1995b;Goldstein et al 1995b) at lower frequencies ( 1 mHz), and as f À5 = 3 (Bavassano et al 1982;Ruzmaikin et al 1993;Horbury et al 1995a), reminiscent of the inertial range of Kolmogorov (1941), at higher frequencies ($10Y100 mHz).…”

Section: Introductionmentioning

confidence: 99%

The Signature of Evolving Turbulence in Quiet Solar Wind as Seen byUlysses

Nicol

Chapman

Dendy

2008

ApJ

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Solar wind fluctuations, such as magnetic field or velocity, show power-law power spectra suggestive both of an inertial range of intermittent turbulence (with $À5/3 exponent), and at lower frequencies, of fluctuations of coronal origin (with $À1 exponent). The Ulysses spacecraft spent many months in the quiet fast solar wind above the Sun's polar coronal holes in a highly ordered magnetic field. We use statistical analysis methods such as the generalized structure function (GSF ) and extended self-similarity (ESS) to quantify the scaling of the moments of the probability density function of fluctuations in the magnetic field. The GSFs give power law scaling in the f À1 range of the form hj y(t þ ) À y(t)j m i $ (m) , but ESS is required to reveal scaling in the inertial range, which is of the form hj y(t þ ) À y(t)j m i $ ½g( ) (m) . We find that g( ) is independent of spacecraft position and g( ) $ À log 10 (k ) . The f À1 scaling fluctuates with radial spacecraft position. This confirms that, whereas the f À1 fluctuations are directly influenced by the corona, the inertial range fluctuations are consistent with locally evolving turbulence, but with an envelope g( ), which captures the formation of the quiet fast solar wind.

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“…The generation of two-channel flows via MRI makes the shearing box model a test-case to study coherent structures in turbulent flows. Coherent structures are responsible for several important features observed in space and astrophysical plasmas such as nonGaussianity (Sorriso-Valvo et al 2001;Hily-Blant and Falgarone 2009;Falceta-Gonçalves et al 2014), multifractality (Bershadskii and Sreenivasan 2004;Bruno et al 2007;Miranda et al 2013) and phase synchronization among scales (Koga et al 2007;.…”

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confidence: 99%

On–off intermittency and amplitude-phase synchronization in Keplerian shear flows

Miranda¹,

Rempel²,

Chian³

2015

Monthly Notices of the Royal Astronomical Society

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We study the development of coherent structures in local simulations of the magnetorotational instability in accretion discs in regimes of on-off intermittency. In a previous paper [Chian et al., Phys. Rev. Lett. 104, 254102 (2010)], we have shown that the laminar and bursty states due to the on-off spatiotemporal intermittency in a one-dimensional model of nonlinear waves correspond, respectively, to nonattracting coherent structures with higher and lower degrees of amplitude-phase synchronization. In this paper we extend these results to a three-dimensional model of magnetized Keplerian shear flows. Keeping the kinetic Reynolds number and the magnetic Prandtl number fixed, we investigate two different intermittent regimes by varying the plasma beta parameter. The first regime is characterized by turbulent patterns interrupted by the recurrent emergence of a large-scale coherent structure known as two-channel flow, where the state of the system can be described by a single Fourier mode. The second regime is dominated by the turbulence with sporadic emergence of coherent structures with shapes that are reminiscent of a perturbed channel flow. By computing the Fourier power and phase spectral entropies in three-dimensions, we show that the large-scale coherent structures are characterized by a high degree of amplitude-phase synchronization.

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Intermittent character of interplanetary magnetic field fluctuations

Abstract: Physics of Plasmas, 14, p. 2901, http://dx.doi.org./10.1063/1.2711429International audienc

Cited by 29 publications

References 35 publications

Turbulence in the Solar Atmosphere and Solar Wind

Turbulence in the Solar Atmosphere and Solar Wind

The Signature of Evolving Turbulence in Quiet Solar Wind as Seen byUlysses

On–off intermittency and amplitude-phase synchronization in Keplerian shear flows

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