Scaling laws for the energy transfer in space plasma turbulence

Marino, Raffaele; Sorriso‐Valvo, L.

doi:10.1016/j.physrep.2022.12.001

Cited by 60 publications

(29 citation statements)

References 489 publications

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“…While for the isothermal model, the energy cascade is due to the compressible component 2C iso e (direct cascade), for the polytropic model, there is a competition between both flux components ε 1C and ε 2C throughout the inertial range. We note that ε 1C and 2C poly e have a few constant scales (less than a decade), which could be due to some specific scale features or simply insufficient statistical convergence of the third-order component (see, Marino & Sorriso-Valvo 2023). This behavior has two consequences, (i) breaking the constant polytropic energy cascade rate, and (ii) the total polytropic cascade rate is of the order of the incompressible cascade rate.…”

Section: The Energy Cascade Ratesmentioning

confidence: 94%

“…Moreover, this exact relation has been used to estimate the energy cascade rate in the solar wind and different planetary magnetosheaths (Sorriso-Valvo et al 2007;MacBride et al 2008;Bandyopadhyay et al 2020aBandyopadhyay et al , 2020bAndrés et al 2021). For a recent detailed review of scaling laws and exact relations in plasma turbulence, see Marino & Sorriso-Valvo (2023).…”

Section: Introductionmentioning

confidence: 99%

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Observation of Turbulent Magnetohydrodynamic Cascade in the Jovian Magnetosheath

Andrés

Bandyopadhyay

McComas

et al. 2023

ApJ

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We present the first estimation of the energy cascade rate in Jupiter’s magnetosheath (MS). We use in situ observations from the Jovian Auroral Distributions Experiment and the magnetometer investigation instruments on board the Juno spacecraft, in concert with two recent compressible models, to investigate the cascade rate in the magnetohydrodynamic (MHD) scales. While a high level of compressible density fluctuations is observed in the Jovian MS, a constant energy flux exists in the MHD inertial range. The compressible isothermal and polytropic energy cascade rates increase in the MHD range when density fluctuations are present. We find that the energy cascade rate in Jupiter’s magnetosheath is at least 2 orders of magnitude (100 times) smaller than the corresponding typical value in the Earth’s magnetosheath.

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Section: The Energy Cascade Ratesmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Observation of Turbulent Magnetohydrodynamic Cascade in the Jovian Magnetosheath

Andrés

Bandyopadhyay

McComas

et al. 2023

ApJ

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“…The flux can be positive or negative, depending on the direction of transfer to small or large scales, or to both as in MHD with a strong uniform field, or in rotating stratified flows [52][53][54] . Similar coupled laws have been derived (for recent reviews, see [55][56][57] ), for kinetic helicity as well as for MHD 58,59 , Hall MHD and electron MHD 60 for the total energy and cross-helicity invariants, with further extensions to magnetic helicity and generalized helicity in Hall MHD, and to the compressible case 61 .…”

Section: Measuring Dissipation Through Exact Lawsmentioning

confidence: 60%

The role of field correlations on turbulent dissipation

Pouquet¹

2023

Preprint

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Nonlinear phenomena and turbulence are central to our understanding and modeling the dynamics of fluids and plasmas, and yet they still resist analytical resolutions in many instances. However, progress has been made recently, displaying a richness of phenomena which was somewhat unexpected a few years back, such as the double constant-flux cascades of a same invariant to both the large and to the small scales, or the presence of non-Gaussian wings in the large-scale fields, for fluids and plasmas. Here, I will concentrate on the direct measurement of the magnitude of dissipation and an evaluation of intermittency in a turbulent plasma using exact laws stemming from invariance principles and involving cross-correlation tensors with both the velocity and the magnetic fields. I will illustrate these points through scaling laws, together with data analysis from existing experiments, observations and numerical simulations. Finally, I will also briefly explore the possible implications for validity and use of several modeling strategies. To appear, Plasma Physics & Controlled Fusion, 2023.

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“…In the attempt to reconcile the remote-sensing and in situ observations in a unified view of the heating of the coronal plasma and the subsequent acceleration of the solar wind, local measurements of the coronal regions are needed. At present, PSP has only occasionally entered the solar corona (Kasper et al 2021;Bandyopadhyay et al 2022;Zank et al 2022;Zhao et al 2022;Marino & Sorriso-Valvo 2023), although its progressively shrinking orbits will ensure that the spacecraft spends extended periods immersed in the coronal plasma. Even then, though, single-spacecraft measurements will provide only one-point information, precluding a clear understanding of how the global (magnetic) configuration of coronal sources affects local dynamics and turbulence properties in space plasmas.…”

Section: Introductionmentioning

confidence: 99%

Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves?

Telloni

Zank

Adhikari

et al. 2023

ApJ

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Evidence for the presence of ion cyclotron waves (ICWs), driven by turbulence, at the boundaries of the current sheet is reported in this paper. By exploiting the full potential of the joint observations performed by Parker Solar Probe and the Metis coronagraph on board Solar Orbiter, local measurements of the solar wind can be linked with the large-scale structures of the solar corona. The results suggest that the dynamics of the current sheet layers generates turbulence, which in turn creates a sufficiently strong temperature anisotropy to make the solar-wind plasma unstable to anisotropy-driven instabilities such as the Alfvén ion cyclotron, mirror-mode, and firehose instabilities. The study of the polarization state of high-frequency magnetic fluctuations reveals that ICWs are indeed present along the current sheet, thus linking the magnetic topology of the remotely imaged coronal source regions with the wave bursts observed in situ. The present results may allow improvement of state-of-the-art models based on the ion cyclotron mechanism, providing new insights into the processes involved in coronal heating.

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Scaling laws for the energy transfer in space plasma turbulence

Cited by 60 publications

References 489 publications

Observation of Turbulent Magnetohydrodynamic Cascade in the Jovian Magnetosheath

Observation of Turbulent Magnetohydrodynamic Cascade in the Jovian Magnetosheath

The role of field correlations on turbulent dissipation

Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves?

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