期刊
ASTROPHYSICAL JOURNAL
卷 850, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aa9754
关键词
magnetic fields; magnetic reconnection; magnetohydrodynamics (MHD); plasmas; turbulence
资金
- NSF-DOE Partnership in Basic Plasma Science and Engineering [DE-SC0016215]
- NSF CAREER [1654168]
- National Science Foundation [NSF AGS-1261659, NSF PHY-1707272]
- University of Wisconsin-Madison
- U.S. Department of Energy (DOE) [DE-SC0016215] Funding Source: U.S. Department of Energy (DOE)
- Direct For Mathematical & Physical Scien
- Division Of Physics [1654168] Funding Source: National Science Foundation
It has recently been proposed that the inertial interval in magnetohydrodynamic (MHD) turbulence is terminated at small scales not by a Kolmogorov-like dissipation region, but rather by a new sub-inertial interval mediated by tearing instability. However, many astrophysical plasmas are nearly collisionless so the MHD approximation is not applicable to turbulence at small scales. In this paper, we propose an extension of the theory of reconnection-mediated turbulence to plasmas which are so weakly collisional that the reconnection occurring in the turbulent eddies is caused by electron inertia rather than by resistivity. We find that the transition scale to reconnection-mediated turbulence depends on the plasma beta and on the assumptions of the plasma turbulence model. However, in all of the cases analyzed, the energy spectra in the reconnection-mediated interval range from E(k(perpendicular to))dk(perpendicular to) alpha k(perpendicular to)(-8/3)dk(perpendicular to) to E(k(perpendicular to))dk(perpendicular to) alpha k(perpendicular to)(-3)dk(perpendicular to).
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