Kelvin-Helmholtz vortices and secondary instabilities in super-magnetosonic regimes

Palermo, F.; Faganello, Matteo; Califano, Francesco; Пегораро, Ф.

doi:10.5194/angeo-29-1169-2011

Cited by 12 publications

(7 citation statements)

References 33 publications

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“…Concerning the late evolution, the sharp variations associated with the shock can trigger the development of secondary instabilities at the boundary region of a vortex, as observed in Palermo et al (2011b) and Henri et al (2012).…”

Section: Super-magnetosonic Flowsmentioning

confidence: 99%

Magnetized Kelvin–Helmholtz instability: theory and simulations in the Earth’s magnetosphere context

Faganello

Califano

2017

J. Plasma Phys.

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The Kelvin–Helmholtz instability, proposed a long time ago for its role in and impact on the transport properties at magnetospheric flanks, has been widely investigated in the Earth’s magnetosphere context. This review covers more than fifty years of theoretical and numerical efforts in investigating the evolution of Kelvin–Helmholtz vortices and how the rich nonlinear dynamics they drive allow solar wind plasma bubbles to enter into the magnetosphere. Special care is devoted to pointing out the main advantages and weak points of the different plasma models that can be adopted for describing the collisionless magnetospheric medium and in underlying\ud the important role of the three-dimensional geometry of the system

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Section: Super-magnetosonic Flowsmentioning

confidence: 99%

Magnetized Kelvin–Helmholtz instability: theory and simulations in the Earth’s magnetosphere context

Faganello

Califano

2017

J. Plasma Phys.

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“…Moreover, the density jump between the magnetosheath and magnetospheric plasmas drives fluid-like secondary instabilities such as the Rayleigh-Taylor instability [13][14][15] . On top of that, the downstream increase of the magnetosheath velocity leads to super-magnetosonic regimes for which the KH vortices act as obstacles to the plasma flow, generating quasi perpendicular shocks 10,16,17 , thus modifying the transport properties of the plasma of the solar windmagnetosphere. It is thus crucial to establish the role of these different secondary instabilities on the dynamics of the system, since they strongly influence the increase of the width of the mixing layer and its internal dynamics that are the most important factors for the evolution at the flank of the Earth's Magnetosphere.…”

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confidence: 99%

Nonlinear evolution of the magnetized Kelvin-Helmholtz instability: From fluid to kinetic modeling

et al. 2013

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The nonlinear evolution of collisionless plasmas is typically a multi-scale process where the energy is injected at large, fluid scales and dissipated at small, kinetic scales. Accurately modelling the global evolution requires to take into account the main micro-scale physical processes of interest. This is why comparison of different plasma models is today an imperative task aiming at understanding cross-scale processes in plasmas. We report here the first comparative study of the evolution of a magnetized shear flow, through a variety of different plasma models by using magnetohydrodynamic, Hall-MHD, two-fluid, hybrid kinetic and full kinetic codes. Kinetic relaxation effects are discussed to emphasize the need for kinetic equilibriums to study the dynamics of collisionless plasmas in non trivial configurations. Discrepancies between models are studied both in the linear and in the nonlinear regime of the magnetized Kelvin-Helmholtz instability, to highlight the effects of small scale processes on the nonlinear evolution of collisionless plasmas. We illustrate how the evolution of a magnetized shear flow depends on the relative orientation of the fluid vorticity with respect to the magnetic field direction during the linear evolution when kinetic effects are taken into account. Even if we found that small scale processes differ between the different models, we show that the feedback from small, kinetic scales to large, fluid scales is negligable in the nonlinear regime. This study show that the kinetic modeling validates the use of a fluid approach at large scales, which encourages the development and use of fluid codes to study the nonlinear evolution of magnetized fluid flows, even in the colisionless regime.

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“…The pressure anisotropy grows in absolute value in correspondence to the compressed or rarefied regions. Plasma rarefaction occurs mainly inside the vortices during their formation, see [29,30], while compression is mainly observed around the vortices in the form of a ribbon structure (surrounded by thin strips of rarefied plasma) or in between the vortices. In the same regions the magnetic field is also strongly reduced because of the plasma expansion or enhanced because of plasma compression thus affecting the value of β ∆ anis , see equation (14).…”

Section: Magnetized Regimementioning

confidence: 99%

Pressure anisotropy generation in a magnetized plasma configuration with a shear flow velocity

Camillis

Cerri

Califano

et al. 2016

Plasma Phys. Control. Fusion

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The nonlinear evolution of the Kelvin Helmholtz instability in a magnetized plasma with a perpendicular flow close to, or in, the supermagnetosonic regime can produce a significant parallel-toperpendicular pressure anisotropy. This anisotropy, localized inside the flow shear region, can make the configuration unstable either to the mirror or to the firehose instability and, in general, can affect the development of the KHI. The interface between the solar wind and the Earth's magnetospheric plasma at the magnetospheric equatorial flanks provides a relevant setting for the development of this complex nonlinear dynamics.

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Kelvin-Helmholtz vortices and secondary instabilities in super-magnetosonic regimes

Cited by 12 publications

References 33 publications

Magnetized Kelvin–Helmholtz instability: theory and simulations in the Earth’s magnetosphere context

Magnetized Kelvin–Helmholtz instability: theory and simulations in the Earth’s magnetosphere context

Nonlinear evolution of the magnetized Kelvin-Helmholtz instability: From fluid to kinetic modeling

Pressure anisotropy generation in a magnetized plasma configuration with a shear flow velocity

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