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

被引:149
作者
Lazarian, Alex [1 ]
Eyink, Gregory L. [2 ,3 ]
Jafari, Amir [3 ]
Kowal, Grzegorz [4 ]
Li, Hui [5 ]
Xu, Siyao [1 ]
Vishniac, Ethan T. [3 ]
机构
[1] Univ Wisconsin, Dept Astron, 475 North Charter St, Madison, WI 53706 USA
[2] Johns Hopkins Univ, Dept Appl Math & Stat, Baltimore, MD 21218 USA
[3] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA
[4] Univ Sao Paulo, Escola Artes Ciencias & Humanidades, Av Arlindo Bettio,1000 Vila Guaraciaba, BR-03828000 Sao Paulo, SP, Brazil
[5] Los Alamos Natl Lab, Los Alamos, NM 87545 USA
关键词
COMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCE; FAST MAGNETIC RECONNECTION; STAR-FORMATION; AMBIPOLAR-DIFFUSION; PARTICLE-ACCELERATION; ENERGY-DISSIPATION; FIELD STRENGTHS; CURRENT SHEETS; COSMIC-RAYS; OBSERVATIONAL CONSTRAINTS;
D O I
10.1063/1.5110603
中图分类号
O35 [流体力学]; O53 [等离子体物理学];
学科分类号
070204 ; 080103 ; 080704 ;
摘要
Magnetic reconnection, topological changes 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 magnetic field lines as persistent dynamical elements. A number of theoretical, numerical, and observational studies starting with the paper done by Lazarian and Vishniac [Astrophys. J. 517, 700-718 (1999)] 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 a magnetohydrodynamiclike treatment of magnetic reconnection on all scales much larger than the relevant plasma scales. We discuss the 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, and 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.
引用
收藏
页数:62
相关论文
共 354 条
[1]   Existence of electromagnetic-hydrodynamic waves [J].
Alfven, H .
NATURE, 1942, 150 :405-406
[2]   Scale decomposition in compressible turbulence [J].
Aluie, Hussein .
PHYSICA D-NONLINEAR PHENOMENA, 2013, 247 (01) :54-65
[3]  
[Anonymous], 2002, HEART, V88, pi1, DOI DOI 10.1103/PHYSREVLETT.88.245001
[4]  
[Anonymous], 2009, TOWN PLANN REV, V80, pi, DOI DOI 10.1103/PHYSREVE.80.025401
[5]  
[Anonymous], 2011, IEEE COMMUN SOC, V8, P6
[6]  
[Anonymous], 2018, CANCER DISCOV, V8, pOF6, DOI DOI 10.1103/PHYSREVX.8.011022
[7]  
[Anonymous], 1965, QJRAS
[8]  
[Anonymous], 2016, EUR J PREV CARDIOL, V23, pNP1, DOI DOI 10.1063/1.4972082
[9]  
[Anonymous], 2009, LUSOTOPIE, V16, pxiii, DOI DOI 10.1063/1.3274462
[10]  
[Anonymous], 2009, LUSOTOPIE, V16, pxiii, DOI DOI 10.1063/1.3264103