Invariants in Relativistic MHD Turbulence

Garrison, David; Nguyen, Phu

doi:10.4236/jmp.2016.73028

Cited by 3 publications

(3 citation statements)

References 29 publications

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“…The situation is somewhat different in the case of relativistic compressible theory. The initial studies of relativistic MHD turbulence (see Zhang, MacFadyen, and Wang, 2009;Inoue, Asano, and Ioka, 2011;Beckwith and Stone, 2011;MacFadyen, 2012, 2013;Garrison and Nguyen, 2015) have not revealed much differences between the non-relativistic and relativistic turbulence. However, more recent studies in Lazarian (2016, 2017) provided the decomposition of the turbulent motions into Alfven, slow and fast modes.…”

Section: Relativistic Mhd Turbulencementioning

confidence: 99%

3D turbulent reconnection: Theory, tests, and astrophysical implications

Lazarían¹,

et al. 2020

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Magnetic reconnection, topological change in magnetic fields, is a fundamental process in magnetized plasmas. It is associated with energy release in regions of magnetic field annihilation, but this is only one facet of this process. Astrophysical fluid flows normally have very large Reynolds numbers and are expected to be turbulent, in agreement with observations. In strong turbulence magnetic field lines constantly reconnect everywhere and on all scales, thus making magnetic reconnection an intrinsic part of the turbulent cascade. We note in particular that this is inconsistent with the usual practice of regarding magnetic field lines as persistent dynamical elements. A number of theoretical, numerical, and observational studies starting with the Lazarian & Vishniac 1999 paper proposed that 3D turbulence makes magnetic reconnection fast and that magnetic reconnection and turbulence are intrinsically connected. In particular, we discuss the dramatic violation of the textbook concept of magnetic flux-freezing in the presence of turbulence. We demonstrate that in the presence of turbulence the plasma effects are subdominant to turbulence as far as the magnetic reconnection is concerned. The latter fact justifies an MHD-like treatment of magnetic reconnection on all scales much larger than the relevant plasma scales. We discuss numerical and observational evidence supporting the turbulent reconnection model. In particular, we demonstrate that the tearing reconnection is suppressed in 3D and, unlike the 2D settings, 3D reconnection induces turbulence that makes magnetic reconnection independent of resistivity. We show that turbulent reconnection dramatically affects key astrophysical processes, e.g. star formation, turbulent dynamo, acceleration of cosmic rays. We provide criticism of the concept of "reconnection-mediated turbulence" and explain why turbulent reconnection is very different from enhanced turbulent resistivity and hyper-resistivity, and why the latter have fatal conceptual flaws.

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Section: Relativistic Mhd Turbulencementioning

confidence: 99%

3D turbulent reconnection: Theory, tests, and astrophysical implications

Lazarían¹,

et al. 2020

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“…Fully relativistic MHD turbulence has been studied since 2009 (Zhang et al (2009); Inoue et al (2011); Beckwith and Stone (2011); MacFadyen (2012, 2013); Garrison and Nguyen (2015), see also Radice and Rezzolla (2013) for non-magnetized turbulence). The results in MacFadyen (2012, 2013) for the mean lab-frame Lorentz factor of ∼1.67 and numerical resolutions of up to 2048 3 confirm that there exists an inertial sub-range of relativistic velocity fluctuations with a -5/3 spectral index.…”

Section: Fully Relativistic Mhd Turbulencementioning

confidence: 99%

Theory and Applications of Non-relativistic and Relativistic Turbulent Reconnection

Lazarian¹,

Kowal

Takamoto

et al. 2016

Magnetic Reconnection

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Realistic astrophysical environments are turbulent due to the extremely high Reynolds numbers of the flows. Therefore, the theories of reconnection intended for describing astrophysical reconnection should not ignore the effects of turbulence on magnetic reconnection. Turbulence is known to change the nature of many physical processes dramatically and in this review we claim that magnetic reconnection is not an exception. We stress that not only astrophysical turbulence is ubiquitous, but also magnetic reconnection itself induces turbulence. Thus turbulence must be accounted for in any realistic astrophysical reconnection setup. We argue that due to the similarities of MHD turbulence in relativistic and non-relativistic cases the theory of magnetic reconnection developed for the non-relativistic case can be extended to the relativistic case and we provide numerical simulations that support this conjecture. We also provide quantitative comparisons of the theoretical predictions and results of numerical experiments, including the situations when turbulent reconnection is self-driven, i.e. the turbulence

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“…This relativistic analog of GS95 was successfully tested for the case of decaying turbulence in Cho (2005) under the so-called force-free approximation. 3 The simulations of fully relativistic MHD turbulence (Zhang et al, 2009;Inoue et al, 2011;Beckwith and Stone, 2011;Zrake & MacFadyen, 2012Garrison & Nguyen, 2015) delivered results also consistent with the GS95 expectations. Recent studies of compressible relativistic MHD turbulence in Takamoto & Lazarian (2016 revealed the difference between it and its non-relativistic analog (see Cho & Lazarian 2002, Kowal & Lazarian 2010.…”

Section: Magnetic Reconnection In Relativistic and Strongly Magnetizementioning

confidence: 56%

Gamma-Ray Bursts Induced by Turbulent Reconnection

Lazarían¹,

Zhang

2019

ApJ

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We consider a simple model for gamma-ray bursts induced by magnetic reconnection in turbulent media. The magnetic field in a jet is subject to kink instabilities, which distort the regular structure of the spiral magnetic field, drive turbulence, and trigger reconnection. The resulting reconnection takes place in a high Reynolds number medium, where turbulence is further enhanced and in turn accelerates the reconnection process. This boot-strap reconnection gives rise to bursts of reconnection events, through which the free energy of magnetic field is transformed into a gamma-ray burst. The efficiency of magnetic reconnection and magnetic energy dissipation is not constrained by microphysical properties of plasmas.

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Invariants in Relativistic MHD Turbulence

Cited by 3 publications

References 29 publications

3D turbulent reconnection: Theory, tests, and astrophysical implications

3D turbulent reconnection: Theory, tests, and astrophysical implications

Theory and Applications of Non-relativistic and Relativistic Turbulent Reconnection

Gamma-Ray Bursts Induced by Turbulent Reconnection

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