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

Hellinger, Petr; Montagud-Camps, Victor; Franci, Luca; Matteini, Lorenzo; Papini, Emanuele; Verdini, A.; Landi, Simone

doi:10.3847/1538-4357/ac5fad

Cited by 15 publications

(8 citation statements)

References 37 publications

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“…A major difference, however, can be appreciated by comparing with Figures 5(c)-(h): reconnection heats the electrons preferentially in the parallel direction with respect to the local magnetic field and the ions in the perpendicular direction. The latter result appears to be in agreement with the fact that a sheared in-plane ion flow tends to transfer energy to the in-plane ion pressure tensor components via the action of the symmetric part of the strain tensor (Del Sarto et al 2016;Del Sarto & Pegoraro 2017;Yang et al 2017;Matthaeus et al 2020;Bandyopadhyay et al 2021;Hellinger et al 2022). Again, we observe a significant lack of symmetry, as particles are heated only on one side of the X-point, typically the same for both species.…”

Section: Standard and Electron-only Reconnectionsupporting

confidence: 88%

“…This strongly supports the idea that coherent structures such as vortices, discontinuities, and thin intense current sheets can play a key role in mediating the turbulent cascade (e.g., Gosling 2007;Greco et al 2012;Karimabadi et al 2013;Osman et al 2014;Franci et al 2016Franci et al , 2017Perrone et al 2016;Wan et al 2016;Yang et al 2017;Camporeale et al 2018;Papini et al 2020Papini et al , 2021Agudelo Rueda et al 2021;Smith & Vasquez 2021, and references therein). Particle energization in collisionless plasmas can proceed via the pressure-strain coupling, which starts to play an important role around the ion scales and by which the kinetic energy of a spatially inhomogeneous flow is anisotropically transferred to internal energy (Del Sarto et al 2016;Del Sarto & Pegoraro 2017;Yang et al 2017;Matthaeus et al 2020;Bandyopadhyay et al 2021;Hellinger et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind

Franci

Papini

Micera

et al. 2022

ApJ

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We perform a high-resolution, 2D, fully kinetic numerical simulation of a turbulent plasma system with observation-driven conditions, in order to investigate the interplay between turbulence, magnetic reconnection, and particle heating from ion to subelectron scales in the near-Sun solar wind. We find that the power spectra of the turbulent plasma and electromagnetic fluctuations show multiple power-law intervals down to scales smaller than the electron gyroradius. Magnetic reconnection is observed to occur in correspondence of current sheets with a thickness of the order of the electron inertial length, which form and shrink owing to interacting ion-scale vortices. In some cases, both ion and electron outflows are observed (the classic reconnection scenario), while in others—typically for the shortest current sheets—only electron jets are present (“electron-only reconnection”). At the onset of reconnection, the electron temperature starts to increase and a strong parallel temperature anisotropy develops. This suggests that in strong turbulence electron-scale coherent structures may play a significant role for electron heating, as impulsive and localized phenomena such as magnetic reconnection can efficiently transfer energy from the electromagnetic fields to particles.

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Section: Standard and Electron-only Reconnectionsupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind

Franci

Papini

Micera

et al. 2022

ApJ

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“…As higher order models, such as compressible Hall MHD or compressible two fluid MHD, are considered, the regime of validity can be pushed to smaller scales 9,20 . Another empirical approach is to introduce pressure strain interactions 52 as an approximation 19 .…”

Section: Energy Transfer: Von Kármán Howarth Equationmentioning

confidence: 99%

Effect of a guide field on the turbulence like properties of magnetic reconnection

Adhikari¹,

Shay²,

Parashar³

et al. 2023

Preprint

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“…For weakly collisional plasmas (such as those in the solar wind), it is necessary to include the effects of plasma compressibility (Hellinger et al 2021a) and treat the pressure as a tensor (Hellinger et al 2022). The pressure-strain interaction, which couples the magnetic+kinetic energy to the internal energy (Del Sarto et al 2016), may work as an effective dissipation channel, as seen in direct kinetic numerical simulations (Yang et al 2017;Matthaeus et al 2020;Hellinger et al 2022;Arró et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Anisotropy of plasma turbulence at ion scales: Hall and pressure–strain effects

Hellinger,

Verdini,

Montagud-Camps

et al. 2024

A&A

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We investigated the properties of plasma turbulence at ion scales in the solar wind context. We concentrated on the behaviour of the Hall physics and the pressure strain interaction and their anisotropy owing to the ambient magnetic field. We studied the results of a three-dimensional hybrid simulation of decaying plasma turbulence using the K\'arm\'an-Howarth-Monin (KHM) equation, which quantifies different turbulent processes. The isotropised KHM analysis shows that kinetic plus magnetic (kinetic+magnetic) energy decays at large scales; this energy cascades from large to small scales via the magneto-hydrodynamic non-linearity that is partly continued via the Hall coupling around the ion scales. The cascading kinetic+magnetic energy is partly dissipated at small scales via resistive dissipation. This standard dissipation is complemented by the pressure-strain interaction, which plays the role of an effective dissipation mechanism and starts to act at relatively large scales. The pressure--strain interaction has two components, compressive and incompressive. Compressive interaction is connected with the velocity dilatation, which mostly reversibly exchanges kinetic+magnetic and internal energies. Incompressive interaction mostly irreversibly converts the kinetic+magnetic energy to internal energy. The compressive effects lead to important oscillations of the turbulence properties, but the compressibility is strongly reduced when averaged over a time period spanning a few periods of the oscillations. The ambient magnetic field induces a strong spectral anisotropy. The turbulent fluctuations exhibit larger scales along the magnetic field compared to the perpendicular directions. The KHM results show the corresponding anisotropy of turbulent processes: their characteristic scales shift to larger scales in the quasi-parallel direction with respect to the ambient magnetic field compared to the quasi-perpendicular direction. This anisotropy is weak at large scales owing to the initial isotropic spectrum, and becomes progressively stronger at small scales.

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

Cited by 15 publications

References 37 publications

Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind

Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind

Effect of a guide field on the turbulence like properties of magnetic reconnection

Anisotropy of plasma turbulence at ion scales: Hall and pressure–strain effects

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