An Introduction to Fluid and MHD Turbulence for Astrophysical Flows: Theory, Observational and Numerical Data, and Modeling

Carbone, V.; Pouquet, A.

doi:10.1007/978-3-642-00210-6_3

Cited by 12 publications

(5 citation statements)

References 86 publications

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“…The q th‐order generalized structure function S q of a one‐dimensional variable u ( x ) can be written as

S_{q} (δx) = < | u (x + δx) - u (x) |^{q} >

where <> denotes an ensemble average of the increments of the variable taken over all pairs of points ( x , x + δ x ) separated by a scale δ x that quantifies the scale of interest. In the case of turbulent signals these quantities ( S q ( δ x )) are representative of fluctuations at the scale δ x (Carbone & Pouquet, ). If the analyzed signal describes a system that meets the scale invariance properties, these structure functions will scale as

S_{q} (δx) \approx δ x^{ξ (q)}

where ξ ( q ) is the scaling index of the q th‐order structure function.…”

Section: Methods Of Analysismentioning

confidence: 99%

Scaling Features of High‐Latitude Geomagnetic Field Fluctuations at Swarm Altitude: Impact of IMF Orientation

et al. 2017

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This paper attempts to explore the statistical scaling features of high‐latitude geomagnetic field fluctuations at Swarm altitude. Data for this study are low‐resolution (1 Hz) magnetic data recorded by the vector field magnetometer on board Swarm A satellite over 1 year (from 15 April 2014 to 15 April 2015). The first‐ and second‐order structure function scaling exponents and the degree of intermittency of the fluctuations of the intensity of the horizontal component of the magnetic field at high northern latitudes have been evaluated for different interplanetary magnetic field orientations in the GSM Y‐Z plane and seasons. In the case of the first‐order structure function scaling exponent, a comparison between the average spatial distributions of the obtained values and the statistical convection patterns obtained using a Super Dual Auroral Radar Network dynamic model (CS10 model) has been also considered. The obtained results support the idea that the knowledge of the scaling features of the geomagnetic field fluctuations can help in the characterization of the different ionospheric turbulence regimes of the medium crossed by Swarm A satellite. This study shows that different turbulent regimes of the geomagnetic field fluctuations exist in the regions characterized by a double‐cell convection pattern and in those regions near the border of the convective structures.

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“…The q th‐order generalized structure function S q of a one‐dimensional variable u ( x ) can be written as

S_{q} (δx) = < | u (x + δx) - u (x) |^{q} >

S_{q} (δx) \approx δ x^{ξ (q)}

where ξ ( q ) is the scaling index of the q th‐order structure function.…”

Section: Methods Of Analysismentioning

confidence: 99%

Scaling Features of High‐Latitude Geomagnetic Field Fluctuations at Swarm Altitude: Impact of IMF Orientation

et al. 2017

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“…Magnetohydrodynamic (MHD) FDT is relevant to plasmas in astrophysical systems as well as fusion reactors (see Carbone and Pouquet [48] for a recent review). The advection-diffusion mechanism controls the statistical properties of magnetic field 17 in MHD FDT (especially if the applied magnetic field is weak, Bershadskii and Sreenivasan [51]).…”

Section: Magnetohydrodynamic Turbulencementioning

confidence: 99%

“…Magnetohydrodynamic (MHD) FDT is relevant to plasmas in astrophysical systems as well as fusion reactors (see Carbone and Pouquet [29] for a recent review). In view of the advection-diffusion mechanism that controls the statistical properties of magnetic field 11 the MHD FDT (Shivamoggi [32]) presents a convenient framework to explore the role of the advection-diffusion mechanism in the FTS development.…”

Section: Magnetohydrodynamic Turbulencementioning

confidence: 99%

Singularities in fully developed turbulence

Shivamoggi

2015

Physics Letters A

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“…Note that some of the concepts to be delineated below are well known, see e.g. [13] (see also [28,[123][124][125][126], and references therein), and the implications for astrophysical turbulence have been reviewed for example in [49,146,157].…”

Section: The Equationsmentioning

confidence: 99%

A Review of the Possible Role of Constraints in MHD Turbulence

Pouquet¹

2015

Rotation and Momentum Transport in Magnetized Plasmas

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A review of some of the issues that have arisen over the years concerning the energy distribution among scales for magnetohydrodynamics (MHD) turbulence is given here. A variety of tools are employed to that effect, and a central role is played by taking into consideration the ideal (nondissipative) invariants, namely the total energy, the magnetic helicity and the cross-correlations between the velocity and the magnetic field (concentrating on the three-dimensional case). These concepts, based mostly on theory, models and direct numerical simulations, are briefly put in the context of observations, in particular the solar wind, and some of the remaining open questions are delineated as well. New results on ideal MHD dynamics in three dimensions on equivalent grids of up to 6144 3 points using the Taylor-Green flow generalized to MHD are also mentioned.

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An Introduction to Fluid and MHD Turbulence for Astrophysical Flows: Theory, Observational and Numerical Data, and Modeling

Cited by 12 publications

References 86 publications

Scaling Features of High‐Latitude Geomagnetic Field Fluctuations at Swarm Altitude: Impact of IMF Orientation

Scaling Features of High‐Latitude Geomagnetic Field Fluctuations at Swarm Altitude: Impact of IMF Orientation

Singularities in fully developed turbulence

A Review of the Possible Role of Constraints in MHD Turbulence

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