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

Lazarian, Alex; Eyink, Gregory L.; Jafari, Amir; Kowal, Grzegorz; Li, Hui; Xu, Siyao; Vishniac, Ethan T.

doi:10.1063/1.5110603

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

Journal Article · Wed Jan 29 00:00:00 EST 2020 · Physics of Plasmas

DOI:https://doi.org/10.1063/1.5110603· OSTI ID:1764228

Lazarian, Alex ^[1]; Eyink, Gregory L. ^[2];

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Univ. of Wisconsin, Madison, WI (United States)
Johns Hopkins Univ., Baltimore, MD (United States)
Univ. de Sao Paolo (Brazil)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

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.

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Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE Laboratory Directed Research and Development (LDRD) Program; USDOE Advanced Research Projects Agency - Energy (ARPA-E); USDOE Office of Science (SC), Fusion Energy Sciences (FES); US Air Force Office of Scientific Research (AFOSR)

Grant/Contract Number:: 89233218CNA000001; AR0000565; FG02-04ER5475; 1914599; FA9550-11-1-0184

OSTI ID:: 1764228

Alternate ID(s):: OSTI ID: 1595866

Report Number(s):: LA-UR-20-28591; TRN: US2206155

Journal Information:: Physics of Plasmas, Vol. 27, Issue 1; ISSN 1070-664X

Publisher:: American Institute of Physics (AIP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 109 works

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Self-organized Criticality in Multi-pulse Gamma-Ray Bursts Lyu, Fen; Li, Ya-Ping; Hou, Shu-Jin arXiv https://doi.org/10.48550/arxiv.2009.06180	preprint	January 2020
Magnetic reconnection in partially ionized plasmas Ni, Lei; Ji, Hantao; Murphy, Nicholas A. arXiv https://doi.org/10.48550/arxiv.2003.13233	preprint	January 2020

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