Nonlinear Reconnection in Magnetized Turbulence

Loureiro, Nuno; Boldyrev, Stanislav

doi:10.3847/1538-4357/ab6a95

Cited by 27 publications

(29 citation statements)

References 72 publications

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“…In general, observations more often find evidence for KAW-like fluctuations than for whistler-wave-like fluctuations (Smith, Vasquez & Hollweg 2011;Salem et al 2012;Podesta 2013;Goldstein et al 2015). Another mechanism proposed to carry the turbulent cascade to subproton scales is magnetic reconnection (Sundkvist et al 2007;Franci et al 2017;Loureiro & Boldyrev 2020).…”

Section: Introductionmentioning

confidence: 99%

“…The problem is rooted in the fact that the range of spatial (L) and temporal (τ ) scales involves fluid-like behaviour at L ρ i , d i , where ρ i is the ion gyroradius and d i is the ion inertial length, as well as kinetic behaviour and energy dissipation at subproton scales, L ρ i , d i . In addition, since plasmas are often in a turbulent state, the presence of a turbulent field alters the onset and evolution of reconnection events (Matthaeus & Lamkin 1986;Strauss 1988;Lazarian & Vishniac 1999;Kim & Diamond 2001;Servidio et al 2011;Boldyrev & Loureiro 2017;Adhikari et al 2020;Loureiro & Boldyrev 2020). It is unclear how turbulence and reconnection affect each other and how the energy is partitioned between particles and fields through both processes.…”

Section: Introductionmentioning

confidence: 99%

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Three-dimensional magnetic reconnection in particle-in-cell simulations of anisotropic plasma turbulence

et al. 2021

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We use three-dimensional (3-D) fully kinetic particle-in-cell simulations to study the occurrence of magnetic reconnection in a simulation of decaying turbulence created by anisotropic counter-propagating low-frequency Alfvén waves consistent with critical-balance theory. We observe the formation of small-scale current-density structures such as current filaments and current sheets as well as the formation of magnetic flux ropes as part of the turbulent cascade. The large magnetic structures present in the simulation domain retain the initial anisotropy while the small-scale structures produced by the turbulent cascade are less anisotropic. To quantify the occurrence of reconnection in our simulation domain, we develop a new set of indicators based on intensity thresholds to identify reconnection events in which both ions and electrons are heated and accelerated in 3-D particle-in-cell simulations. According to the application of these indicators, we identify the occurrence of reconnection events in the simulation domain and analyse one of these events in detail. The event is related to the reconnection of two flux ropes, and the associated ion and electron exhausts exhibit a complex 3-D structure. We study the profiles of plasma and magnetic-field fluctuations recorded along artificial-spacecraft trajectories passing near and through the reconnection region. Our results suggest the presence of particle heating and acceleration related to small-scale reconnection events within magnetic flux ropes produced by the anisotropic Alfvénic turbulent cascade in the solar wind. These events are related to current structures of the order of a few ion inertial lengths in size.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Three-dimensional magnetic reconnection in particle-in-cell simulations of anisotropic plasma turbulence

et al. 2021

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“…This is the essence of recent papers on reconnection-modified inertial ranges in MHD turbulence (Mallet et al. 2017; Loureiro & Boldyrev 2020).…”

Section: Onset Models Based On the Tearing Instability Of Thin Currenmentioning

confidence: 87%

“…In Mallet et al. (2017) and Loureiro & Boldyrev (2020) (and references therein) the anisotropy of cascading eddies increases as the energy transfer marches to smaller scales, until current sheets form, whose tearing growth rate might be comparable to the nonlinear cascade time: the effects of the tearing of turbulent eddies alters the slope of turbulence inertial range spectra at higher wave numbers. On the other hand, the turbulence consequences of the self-similar current sheet collapse starting from a laminar configuration have been presented in Uzdensky, Loureiro & Schekochihin (2010) and Tenerani & Velli (2020).…”

Section: Discussionmentioning

confidence: 99%

“…Closer to the Earth, the magnetosheath and plasma sheet are also noisy, bursty and randomly structured (Borovsky et al 1997). Within the framework of fluid theories of ongoing nonlinear cascades, scales associated with magnetic reconnection appear critically, and there is little doubt that reconnection plays an important role in the transition from inertial to dissipative scales, perhaps even within the inertial range (Servidio et al 2009;Loureiro & Boldyrev 2020;Mallet, Schekochihin & Chandran 2017). Reciprocally, turbulence may provide a triggering mechanism, or accelerate the dynamics of reconnection once it has started (Matthaeus & Lamkin 1986;Matthaeus & Velli 2011;Lazarian, Eyink & Vishniac 2012).…”

Section: Introduction To Magnetic Reconnectionmentioning

confidence: 99%

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Onset of fast magnetic reconnection and particle energization in laboratory and space plasmas

et al. 2020

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The onset of magnetic reconnection in space, astrophysical and laboratory plasmas is reviewed discussing results from theory, numerical simulations and observations. After a brief introduction on magnetic reconnection and approach to the question of onset, we first discuss recent theoretical models and numerical simulations, followed by observations of reconnection and its effects in space and astrophysical plasmas from satellites and ground-based detectors, as well as measurements of reconnection in laboratory plasma experiments. Mechanisms allowing reconnection spanning from collisional resistivity to kinetic effects as well as partial ionization are described, providing a description valid over a wide range of plasma parameters, and therefore applicable in principle to many different astrophysical and laboratory environments. Finally, we summarize the implications of reconnection onset physics for plasma dynamics throughout the Universe and illustrate how capturing the dynamics correctly is important to understanding particle acceleration. The goal of this review is to give a view on the present status of this topic and future interesting investigations, offering a unified approach.

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Magnetic reconnection: MHD theory and modelling

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Priest

2022

Living Rev Sol Phys

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In this review we focus on the fundamental theory of magnetohydrodynamic reconnection, together with applications to understanding a wide range of dynamic processes in the solar corona, such as flares, jets, coronal mass ejections, the solar wind and coronal heating. We summarise only briefly the related topics of collisionless reconnection, non-thermal particle acceleration, and reconnection in systems other than the corona. We introduce several preliminary topics that are necessary before the subtleties of reconnection can be fully described: these include null points (Sects. 2.1–2.2), other topological and geometrical features such as separatrices, separators and quasi-separatrix layers (Sects. 2.3, 2.6), the conservation of magnetic flux and field lines (Sect. 3), and magnetic helicity (Sect. 4.6). Formation of current sheets in two- and three-dimensional fields is reviewed in Sect. 5. These set the scene for a discussion of the definition and properties of reconnection in three dimensions that covers the conditions for reconnection, the failure of the concept of a flux velocity, the nature of diffusion, and the differences between two-dimensional and three-dimensional reconnection (Sect. 4). Classical 2D models are briefly presented, including magnetic annihilation (Sect. 6), slow and fast regimes of steady reconnection (Sect. 7), and non-steady reconnection such as the tearing mode (Sect. 8). Then three routes to fast reconnection in a collisional or collisionless medium are described (Sect. 9). The remainder of the review is dedicated to our current understanding of how magnetic reconnection operates in three dimensions and in complex magnetic fields such as that of the Sun’s corona. In Sects. 10–12, 14.1 the different regimes of reconnection that are possible in three dimensions are summarised, including at a null point, separator, quasi-separator or a braid. The role of 3D reconnection in solar flares (Sect. 13) is reviewed, as well as in coronal heating (Sect. 14), and the release of the solar wind (Sect. 15.2). Extensions including the role of reconnection in the magnetosphere (Sect. 15.3), the link between reconnection and turbulence (Sect. 16), and the role of reconnection in particle acceleration (Sect. 17) are briefly mentioned.

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Nonlinear Reconnection in Magnetized Turbulence

Cited by 27 publications

References 72 publications

Three-dimensional magnetic reconnection in particle-in-cell simulations of anisotropic plasma turbulence

Three-dimensional magnetic reconnection in particle-in-cell simulations of anisotropic plasma turbulence

Onset of fast magnetic reconnection and particle energization in laboratory and space plasmas

Magnetic reconnection: MHD theory and modelling

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