Magnetic Reconnection, Turbulence, and Collisionless Shock

Details Magnetic Reconnection, Turbulence, and Collisionless Shock Magnetic Reconnection, Turbulence, and Collisionless Shock

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ap%26ss.298..219j&link_type=abstract

Astrophysics and Space Science, Volume 298, Issue 1-2, pp. 219-226

Astronomy and Astrophysics

Astrophysics

1

Magnetic Reconnection, Plasma Instability, Turbulence, Collisionless Shock, Laboratory Experiment

Scientific paper

A short summary of recent progress in measuring and understanding turbulence during magnetic reconnection in laboratory plasmas is given. Magnetic reconnection is considered as a primary process to dissipate magnetic energy in laboratory and astrophysical plasmas. A central question concerns why the observed reconnection rates are much faster than predictions made by classical theories, such as the Sweet Parker model based on MHD with classical Spitzer resistivity. Often, the local resistivity is conjectured to be enhanced by turbulence to accelerate reconnection rates either in the context of the Sweet Parker model or by facilitating setup of the Pestchek model. Measurements at a dedicated laboratory experiment, called MRX or Magnetic Reconnection Experiment, have indicated existence of strong electromagnetic turbulence in current sheets undergoing fast reconnection. The origin of the turbulence has been identified as right-hand polarized whistler waves, propagating obliquely to the reconnecting field, with a phase velocity comparable to the relative drift velocity. These waves are consistent with an obliquely propagating electromagnetic lower-hybrid drift instability driven by drift speeds large compared to the Alfven speed in high-beta plasmas. Interestingly, this instability may explain electromagnetic turbulence also observed in collisionless shocks, which are common in energetic astrophysical phenomena.

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