Identifying intermittency events in the solar wind

Bruno, R.; Carbone, V.; Veltri, P.; Pietropaolo, E.; Bavassano, B.

doi:10.1016/s0032-0633(01)00061-7

Cited by 281 publications

(324 citation statements)

References 50 publications

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“…PVI turns out to be a useful and easily implemented measure, but it is not unique. Other methods, some based on wavelets [64] such as the local intermittency measure (LIM) [65,66], or distinct techniques such as the phase coherence index the [67] and others, are also useful in quantifying intermittent signals. Our preference for use of PVI is based on its simplicity of implementation, and we are confident that results based on PVI can also be obtained with different methods; for a comparison of PVI and Haar wavelets, see [64].…”

Section: Evidence For Coherent Structures In the Solar Windmentioning

confidence: 99%

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

Matthaeus

Wan

Servidio

et al. 2015

Phil. Trans. R. Soc. A.

187

139

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Section: Evidence For Coherent Structures In the Solar Windmentioning

confidence: 99%

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

Matthaeus

Wan

Servidio

et al. 2015

Phil. Trans. R. Soc. A.

187

139

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“…Later, Mariani et al (1973) adopted it to explain the observed variations of the occurrence rate of discontinuities in the interplanetary magnetic field. Recently, Bruno et al (2001Bruno et al ( , 2004 and Chang et al (2004) noted that the existence of flux tubes in the solar wind will introduce another source of solar wind intermittency. Although the concept of flux tubes has been noted by many authors, few attempts have been put forth to verify the existence of these structures.…”

Section: Introductionmentioning

confidence: 99%

Identifying Current-Sheet-like Structures in the Solar Wind

2007

ApJ

101

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In past years, measurements of the solar wind plasma have advanced our understanding of MHD turbulence tremendously. At small scales, the solar wind is believed to be ve'xry multifractal with nonlinear interactions causing an intermittent energy dissipation, leading to possible current-sheet structures. In this Letter, we propose a systematic data analysis procedure to examine the existence of current sheets in the solar wind. We show that by studying the integrated distribution function of the angle between two unit magnetic fields and F(v, z ) b(t) , as well as its z-dependence, one can unambiguously identify the existence of current-sheet-like structureŝ b(t ϩ z ) in the solar wind. Using this procedure, we analyze magnetic field data from the VHM/FGM instrument on board the spacecraft Ulysses for two periods, one in solar maximum and the other in solar minimum. In both cases, current sheets are clearly inferred. Furthermore, we also outline a procedure that allows the identification of the actual locations of these current sheets. Results from our analysis and the implications of the existence of current sheets in the solar wind are discussed.

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“…The characteristics of the spectral properties of fluctuations in the incompressible interplanetary medium were provided in classical statistical theory via the phase space distribution obtained from ideal MHD invariants by Matthaeus and Goldstein (1982) followed by a confirmation of the existence of solar wind multi-fractal structures (Burlaga, 1991(Burlaga, , 1992. The PDFs of the magnetic field and plasma fluctuations were analyzed and linked to intermittency of the solar wind MHD fluctuations Tu, 1994, 1997) along with detailed investigations of the non-Gaussian characteristics (Bruno et al, 2001;Hnat et al, 2003). WIND, ACE and Voyager observations of interplanetary multi-scale statistical properties verify that the leptokurtic, long-tailed shapes of the PDFs at small scales represent correctly the characteristics of intermittent turbulence and approach a Gaussian, reflecting a decoupled state, on large scales (Sorriso-Valvo et al, 1999;Leubner and Vörös, 2005a,b;Leubner et al, 2006), thus confirming that the probability of rare events is raised on small scales.…”

Section: Introductionmentioning

confidence: 99%

Consequences of entropy bifurcation in non-Maxwellian astrophysical environments

Leubner

2008

Nonlin. Processes Geophys.

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Abstract. Non-extensive systems, accounting for long-range interactions and correlations, are fundamentally related to non-Maxwellian distributions where a duality of equilibria appears in two families, the non-extensive thermodynamic equilibria and the kinetic equilibria. Both states emerge out of particular entropy generalization leading to a class of probability distributions, where bifurcation into two stationary states is naturally introduced by finite positive or negative values of the involved entropic index kappa. The limiting Boltzmann-Gibbs-Shannon state (BGS), neglecting any kind of interactions within the system, is subject to infinite entropic index and thus characterized by self-duality. Fundamental consequences of non-extensive entropy bifurcation, manifest in different astrophysical environments, as particular core-halo patterns of solar wind velocity distributions, the probability distributions of the differences of the fluctuations in plasma turbulence as well as the structure of density distributions in stellar gravitational equilibrium are discussed. In all cases a lower entropy core is accompanied by a higher entropy halo state as compared to the standard BGS solution. Data analysis and comparison with high resolution observations significantly support the theoretical requirement of nonextensive entropy generalization when dealing with systems subject to long-range interactions and correlations.

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Identifying intermittency events in the solar wind

Cited by 281 publications

References 50 publications

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

Identifying Current-Sheet-like Structures in the Solar Wind

Consequences of entropy bifurcation in non-Maxwellian astrophysical environments

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