Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration

Lazarían, A.; Vlahos, L.; Kowal, Grzegorz; Yan, Huirong; Beresnyak, Andrey; Pino, E. M. de Gouveia Dal

doi:10.1007/978-1-4614-6455-6_18

Cited by 11 publications

(28 citation statements)

References 246 publications

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“…There have been many theoretical articles on energetic charged particle diffusion associated with interplanetary turbulence. Some more recent papers are Lazarian et al (), Le Roux et al (), Sun et al (), and Subedi et al (). We direct the interested reader to these papers and their references.…”

Section: Effects Of Interplanetary Turbulencementioning

confidence: 99%

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

et al. 2018

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Solar wind turbulence within high‐speed streams is reviewed from the point of view of embedded single nonlinear Alfvén wave cycles, discontinuities, magnetic decreases (MDs), and shocks. For comparison and guidance, cometary plasma turbulence is also briefly reviewed. It is demonstrated that cometary nonlinear magnetosonic waves phase‐steepen, with a right‐hand circular polarized foreshortened front and an elongated, compressive trailing edge. The former part is a form of “wave breaking” and the latter that of “period doubling.” Interplanetary nonlinear Alfvén waves, which are arc polarized, have a ~180° foreshortened front and with an elongated trailing edge. Alfvén waves have polarizations different from those of cometary magnetosonic waves, indicating that helicity is a durable feature of plasma turbulence. Interplanetary Alfvén waves are noted to be spherical waves, suggesting the possibility of additional local generation. They kinetically dissipate, forming MDs, indicating that the solar wind is partially “compressive” and static. The ~2 MeV protons can nonresonantly interact with MDs leading to rapid cross‐field (~5.5% Bohm) diffusion. The possibility of local (~1 AU) generation of Alfvén waves may make it difficult to forecast High‐Intensity, Long‐Duration AE Activity and relativistic magnetospheric electrons with great accuracy. The future Solar Orbiter and Solar Probe Plus missions should be able to not only test these ideas but to also extend our knowledge of plasma turbulence evolution.

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Section: Effects Of Interplanetary Turbulencementioning

confidence: 99%

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

et al. 2018

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“…It has been discussed that turbulence with a large wave energy density plays an important role in the transport of mass and momentum in the magnetotail [e.g., Borovsky and Funsten , ; Zimbardo et al , ]. Understanding the effects of this turbulence is believed to be a key factor in obtaining an overall understanding of the various plasma phenomena that occur both in space and also in astrophysical plasmas [e.g., Birn et al , ; Lazarian et al , ].…”

Section: Introductionmentioning

confidence: 99%

“…It has been argued that turbulence plays a crucial role in the dynamic evolution of magnetic reconnection and that the magnetic energy dissipation rate can be enhanced by turbulence [e.g., Matthaeus and Lamkin , ; Lazarian and Vishniac , ; Loureiro et al , ; Higashimori et al , ; Yokoi et al , ]. In addition to its role in the dynamic evolution of reconnection, turbulence is believed to play an essential role not only in thermal plasma heating but also in nonthermal particle production through the stochastic scattering of particles [e.g., Veltri et al , ; Greco et al , ; Zelenyi et al , , ; Lazarian et al , ]. However, in previous studies, it was postulated that turbulence can be generated in the high β plasma sheet with a high magnetic Reynolds number, but the detailed mechanism required to generate Alfvénic waves and turbulence during the dynamic evolution of reconnection is not understood as yet.…”

Section: Introductionmentioning

confidence: 99%

Generation of Alfvénic waves and turbulence in reconnection jets

Hoshino

Higashimori

2015

JGR Space Physics

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The magnetohydrodynamic linear stability with the localized bulk flow oriented parallel to the neutral sheet is investigated, by including the Hall effect and the guide magnetic field. We observe three different unstable modes: a "streaming tearing" mode at a slow flow speed, a "streaming sausage" mode at a medium flow speed, and a "streaming kink" mode at a fast flow speed. The streaming tearing and sausage modes have a standard tearing mode-like structure with symmetric density fluctuations in the neutral sheet, while the kink mode has an asymmetric fluctuation. The growth rate of the streaming tearing mode decreases with increasing magnetic Reynolds number, while the growth rates of the sausage and kink modes do not depend strongly on the Reynolds number. The sausage and kink modes can be unstable for not only super-Alfvénic flow but also sub-Alfvénic flow when the lobe density is low. The wavelengths of these unstable modes are of the same order of magnitude as the thickness of the plasma sheet. Their maximum growth rates are higher than that of a standard tearing mode, and under a strong guide magnetic field, the growth rates of the sausage and kink modes are enhanced, while under a weak guide magnetic field, they are suppressed. For a thin plasma sheet with the Hall effect, the fluctuations of the streaming modes can exist over the plasma sheet. These unstable modes may be regarded as being one of the processes generating Alfvénic turbulence in the plasma sheet during magnetic reconnection.

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“…Applications to galactic dynamos were discussed by Beck et al (1996). Aspects of magnetic reconnection and particle acceleration in turbulent flows have recently been reviewed by Lazarian et al (2012b). In the present review we begin with turbulence in the interstellar medium, discuss how turbulence is affected by…”

mentioning

confidence: 96%

“…In real turbulent cascade such interactions proceed at every scale of turbulent motions. FromLazarian et al (2012b).…”

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confidence: 99%

Astrophysical Hydromagnetic Turbulence

2013

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Recent progress in astrophysical hydromagnetic turbulence is being reviewed. The physical ideas behind the now widely accepted Goldreich-Sridhar model and its extension to compressible magnetohydrodynamic turbulence are introduced. Implications for cosmic ray diffusion and acceleration is being discussed. Dynamo-generated magnetic fields with and without helicity are contrasted against each other. Certain turbulent transport processes are being modified and often suppressed by anisotropy and inhomogeneities of the turbulence, while others are being produced by such properties, which can lead to new largescale instabilities of the turbulent medium. Applications of various such processes to astrophysical systems are being considered.Keywords magnetic fields · turbulence · Sun: magnetic fields · ISM: magnetic fields PACS 44.25.+f · 47.27.Eq · 47.27.Gs · 47.27.Qb IntroductionHydromagnetic or magnetohydrodynamic (MHD) turbulence plays an important role in many astrophysical settings. In a recent review by Brandenburg and Nordlund (2011), properties of turbulence were discussed for the solar wind, stellar convection zones, the interstellar medium, accretion discs, galaxy clusters, and the early Universe. In an earlier review by Brandenburg and Subramanian (2005), a detailed account of dynamo theory with emphasis on helical dynamos was given. In that review, and also in Brandenburg et al. (2012c), the small-scale dynamo was discussed in detail. Applications to galactic dynamos were discussed by Beck et al. (1996). Aspects of magnetic reconnection and particle acceleration in turbulent flows have recently been reviewed by Lazarian et al. (2012b). In the present review we begin with turbulence in the interstellar medium, discuss how turbulence is affected by

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Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration

Cited by 11 publications

References 246 publications

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

Generation of Alfvénic waves and turbulence in reconnection jets

Astrophysical Hydromagnetic Turbulence

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