Physics – Plasma Physics
Scientific paper
Nov 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..dpp..8s03c&link_type=abstract
American Physical Society, Division of Plasma Physics Meeting, November 10-15, 1996, abstract #8S.03
Physics
Plasma Physics
Scientific paper
Cosmic and galactic magnetic fields are believed to result from amplification by turbulence. To understand this process the buildup of magnetic energy in a zero-resistivity turbulent MHD plasma is considered in numerical simulations using both the Direct Interaction Approximation and the Realizable Markovian Closure of Bowman and Krommes. In the earliest stages of growth when the magnetic field is dynamically unimportant, magnetic energy grows rapidly on scales much smaller than the scale of the smallest turbulent eddies, if the resistivity is sufficiently small.(Kulsrud, R., and Anderson, S. 1992, ApJ, 396, 606) However, it is shown that at some point before the magnetic field reaches equipartition with even the smallest turbulent eddies, dynamic effects prevent further growth of the smallest scale magnetic fields. When the magnetic energy reaches equipartition with the smallest turbulent eddies, the magnetic energy is concentrated near the smallest turbulent scale. The magnetic energy continues to grow for a few large-eddy turnover times until it reaches rough equipartition with the velocity turbulence at all scales, and a k-3/2 spectrum is set up. Implications for both the galactic and protogalactic dynamos will be discussed.
Chandran Benjamin
Kulsrud Russell
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