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Fast Reconnection of Weak Magnetic FieldsFast magnetic reconnection refers to annihilation or topological rearrangement of magnetic fields on a timescale that is independent (or nearly independent) of the plasma resistivity. The resistivity of astrophysical plasmas is so low that reconnection is of little practical interest unless it is fast. Yet, the theory of fast magnetic reconnection is on uncertain ground, as models must avoid the tendency of magnetic fields to pile up at the reconnection layer, slowing down the flow. In this paper it is shown that these problems can be avoided to some extent if the flow is three dimensional. On the other hand, it is shown that in the limited but important case of incompressible stagnation point flows, every flow will amplify most magnetic fields. Although examples of fast magnetic reconnection abound, a weak, disordered magnetic field embedded in stagnation point flow will in general be amplified, and should eventually modify the flow. These results support recent arguments against the operation of turbulent resistivity in highly conducting fluids.
Document ID
19980055029
Acquisition Source
Goddard Space Flight Center
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Zweibel, Ellen G.
(Joint Inst. for Lab. Astrophysics Boulder, CO United States)
Date Acquired
September 6, 2013
Publication Date
January 1, 1998
Publication Information
Publication: Physics Plasmas
Publisher: American Inst. of Physics
Volume: 5
Issue: 1
ISSN: 1070-664X
Subject Category
Astrophysics
Report/Patent Number
NASA/CR-1998-208148
NAS 1.26:208148
Funding Number(s)
CONTRACT_GRANT: NSF AST-95-21179
CONTRACT_GRANT: NAG5-4063
CONTRACT_GRANT: NAG5-2256
Distribution Limits
Public
Copyright
Public Use Permitted.
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