Turbulent Mangetohydrodynamic Reconnection Mediated by the Plasmoid Instability

Huang, Yi-Min; Bhattacharjee, A.

doi:10.3847/0004-637X/818/1/20

Title: Turbulent Mangetohydrodynamic Reconnection Mediated by the Plasmoid Instability

Journal Article · Wed Feb 03 00:00:00 EST 2016 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/0004-637X/818/1/20· OSTI ID:1565531

Huang, Yi-Min ^[1]; Bhattacharjee, A. ^[1]

Princeton Univ., NJ (United States). Dept. of Astrophysical Sciences, and Princeton Plasma Physics Lab.; Princeton Center for Heliophysics, NJ (United States); Max-Panck Princeton Center for Plasma Physics (MPPC), NJ (United States); Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas (CMSO), Madison, WI (United States)

It has been established that the Sweet–Parker current layer in high Lundquist number reconnection is unstable to the super-Alfvénic plasmoid instability. Past two-dimensional magnetohydrodynamic simulations have demonstrated that the plasmoid instability leads to a new regime where the Sweet–Parker current layer changes into a chain of plasmoids connected by secondary current sheets, and the averaged reconnection rate becomes nearly independent of the Lundquist number. In this work, a three-dimensional simulation with a guide field shows that the additional degree of freedom allows plasmoid instabilities to grow at oblique angles, which interact and lead to self-generated turbulent reconnection. The averaged reconnection rate in the self-generated turbulent state is of the order of a hundredth of the characteristic Alfvén speed, which is similar to the two-dimensional result but is an order of magnitude lower than the fastest reconnection rate reported in recent studies of externally driven three-dimensional turbulent reconnection. Kinematic and magnetic energy fluctuations both form elongated eddies along the direction of the local magnetic field, which is a signature of anisotropic magnetohydrodynamic turbulence. Both energy fluctuations satisfy power-law spectra in the inertial range, where the magnetic energy spectral index is in the range from -2.3 to -2.1, while the kinetic energy spectral index is slightly steeper, in the range from -2.5 to -2.3. Finally, the anisotropy of turbulence eddies is found to be nearly scale-independent, in contrast with the prediction of the Goldreich–Sridhar theory for anisotropic turbulence in a homogeneous plasma permeated by a uniform magnetic field.

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Research Organization:: Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF)

Sponsoring Organization:: USDOE Office of Science (SC)

OSTI ID:: 1565531

Journal Information:: The Astrophysical Journal (Online), Vol. 818, Issue 1; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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