Energy transfer in reconnection and turbulence

Adhikari, Subash; Parashar, T. N.; Shay, M. A.; Matthaeus, W. H.; Pyakurel, Prayash Sharma; Fordin, S; Stawarz, J. E.; Eastwood, J. P.

doi:10.1103/physreve.104.065206

Cited by 25 publications

(23 citation statements)

References 64 publications

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“…Note that the incompressible Hall cascade rate in Hellinger et al (2018) is twice the correct value (see Ferrand et al 2019) so that the decrease of the effective incompressible cascade rate at subion scales is underestimated there. The decrease of the incompressible rate at subion scales is in agreement with other previous simulation and observation works (Bandyopadhyay et al 2020;Adhikari et al 2021).…”

Section: Discussionsupporting

confidence: 93%

“…One way to discern and quantify different turbulent processes is the Kármán-Howarth-Monin (KHM) equation (de Kármán & Howarth 1938;Monin & Yaglom 1975;Frisch 1995) that connects the energy decay/injection with its cascade and dissipation. Recently, the incompressible version of the KHM equation for the Hall-magnetohydrodynamic (MHD) approximation (Politano & Pouquet 1998;Galtier 2008;Hellinger et al 2018;Ferrand et al 2019) was used to study the ion transition in simulations as well as observations (Hellinger et al 2018;Bandyopadhyay et al 2020;Adhikari et al 2021). These results indicate that at ion scales there is indeed a transition from an MHD-to a Halldominated turbulent cascade.…”

Section: Introductionmentioning

confidence: 99%

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Ion-scale Transition of Plasma Turbulence: Pressure–Strain Effect

Hellinger

Montagud-Camps

Franci

et al. 2022

ApJ

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We investigate properties of solar-wind-like plasma turbulence using direct numerical simulations. We analyze the transition from large, magnetohydrodynamic (MHD) scales to the ion characteristic ones using two-dimensional hybrid (fluid electrons and kinetic ions) simulations. To capture and quantify turbulence properties, we apply the Karman–Howarth–Monin (KHM) equation for compressible Hall–MHD (extended by considering the plasma pressure as a tensor quantity) to the numerical results. The KHM analysis indicates that the transition from MHD to ion scales (the so-called ion break in the power spectrum) results from a combination of an onset of Hall physics and an effective dissipation owing to the pressure–strain energy-exchange channel and resistivity. We discuss the simulation results in the context of the solar wind.

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Section: Discussionsupporting

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Ion-scale Transition of Plasma Turbulence: Pressure–Strain Effect

Hellinger

Montagud-Camps

Franci

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…Note that the incompressible Hall cascade rate in Hellinger et al (2018) is twice the correct value (cf., Ferrand et al 2019) so that the decrease of the effective incompressible cascade rate at sub-ion scales is underestimated there. The decrease of the incompressible rate at sub-ion scales is in agreement with other previous simulation and observation works (Bandyopadhyay et al 2020;Adhikari et al 2021).…”

Section: Discussionsupporting

confidence: 93%

“…One way how to discern and quantify different turbulent processes is the Kármán-Howarth-Monin (KHM) equation (de Kármán & Howarth 1938;Monin & Yapetr.hellinger@asu.cas.cz glom 1975;Frisch 1995) that connects the energy decay/injection with its cascade and dissipation. Recently, the incompressible version of the KHM equation for the Hall MHD (Politano & Pouquet 1998;Galtier 2008;Hellinger et al 2018;Ferrand et al 2019) was used to study the ion transition in simulations as well as observations (Hellinger et al 2018;Bandyopadhyay et al 2020;Adhikari et al 2021). These results indicate that at ion scales there is indeed a transition from a MHD to a Hall dominated turbulent cascade.…”

Section: Introductionmentioning

confidence: 99%

Ion-scale transition of plasma turbulence: Pressure-strain effect

Hellinger,

Montagud-Camps,

Franci

et al. 2022

Preprint

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We investigate properties of solar wind-like plasma turbulence using direct numerical simulations. We analyze the transition from large, magnetohydrodynamic (MHD) scales to the ion characteristic ones using two-dimensional hybrid (fluid electrons, kinetic ions) simulations. To capture and quantify turbulence properties, we apply the Karman-Howarth-Monin (KHM) equation for compressible Hall MHD (extended by considering the plasma pressure as a tensor quantity) to the numerical results. The KHM analysis indicates that the transition from MHD to ion scales (the so called ion break in the power spectrum) results from a combination of an onset of Hall physics and of an effective dissipation owing to the pressure-strain energy-exchange channel and resistivity. We discuss the simulation results in the context of the solar wind.

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“…Here we are concerned with energy balance across scales, measured using the von Kármán-Howarth equation (Verdini et al 2015;Hellinger et al 2018;Ferrand et al 2019;Adhikari et al 2021) and filtered Vlasov-Maxwell equations Matthaeus et al 2020). In both scale filtering and structure function representations, crucial elements are energy loss at large scales, energy flux in an intermediate range, and dissipation at small scales.…”

Section: Introductionmentioning

confidence: 99%

Pressure-Strain Interaction as the Energy Dissipation Estimate in Collisionless Plasma

Yang,

Matthaeus,

Roy

et al. 2022

Preprint

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The dissipative mechanism in weakly collisional plasma is a topic that pervades decades of studies without a consensus solution. We compare several energy dissipation estimates based on energy transfer processes in plasma turbulence and provide justification for the pressure-strain interaction as a direct estimate of the energy dissipation rate. The global and scale-by-scale energy balances are examined in 2.5D and 3D kinetic simulations. We show that the global internal energy increase and the temperature enhancement of each species are directly tracked by the pressure-strain interaction. The incompressive part of the pressure-strain interaction dominates over its compressive part in all simulations considered. The scale-by-scale energy balance is quantified by scale filtered Vlasov-Maxwell equations, a kinetic plasma approach, and the lag dependent von Kármán-Howarth equation, an approach based on fluid models. We find that the energy balance is exactly satisfied across all scales, but the lack of a well-defined inertial range influences the distribution of the energy budget among different terms in the inertial range. Therefore, the widespread use of the Yaglom relation to estimating dissipation rate is questionable in some cases, especially when the scale separation in the system is not clearly defined. In contrast, the pressure-strain interaction balances exactly the dissipation rate at kinetic scales regardless of the scale separation.

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Energy transfer in reconnection and turbulence

Cited by 25 publications

References 64 publications

Ion-scale Transition of Plasma Turbulence: Pressure–Strain Effect

Ion-scale Transition of Plasma Turbulence: Pressure–Strain Effect

Ion-scale transition of plasma turbulence: Pressure-strain effect

Pressure-Strain Interaction as the Energy Dissipation Estimate in Collisionless Plasma

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