Numerical Simulations of Stochastic Reconnection

Details Numerical Simulations of Stochastic Reconnection Numerical Simulations of Stochastic Reconnection

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21348513v&link_type=abstract

American Astronomical Society, AAS Meeting #213, #485.13; Bulletin of the American Astronomical Society, Vol. 41, p.457

Physics

Scientific paper

Magnetic reconnection in an ionized medium, like stars, accretion disks, or the interstellar medium, ultimately depends on the action of resistivity on very small scales. We have constructed numerical simulations to test the hypothesis of stochastic reconnection (Lazarian and VIshniac, 1999) - the theory that the reconnection rate in a turbulent, highly conducting medium, depends on the amplitude of the turbulence and not on the microphysics. These tests require three dimensional simulations with appropriately open boundaries. We show that the reconnection speed is enhanced by turbulence for sufficiently strong subalfvenic turbulence. We also show that in this limit the reconnection speed is insensitive to the resistivity of the fluid. In ionized astrophysical systems. This implies that the speed of reconnection is of order the local turbulent velocity, regardless of the nature of the medium.

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