Magnetic Reconnection in Plasmas

Details Magnetic Reconnection in Plasmas Magnetic Reconnection in Plasmas

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ap%26ss.242..165b&link_type=abstract

Astrophysics and Space Science, Volume 242, Issue 1-2, pp. 165-207

Astronomy and Astrophysics

Astrophysics

24

Magnetic Fields, Reconnection, Mhd Turbulence, Cosmic Plasmas

Scientific paper

A review of the present status of the theory of magnetic reconnection is given. In strongly collisional plasmas reconnection proceeds via resistive current sheets, i.e. quasi-stationary macroscopic Sweet-Parker sheets at intermediate values of the magnetic Reynolds numberR m , or mirco-current sheets in MHD turbulence, which develops at highR m . In hot, dilute plasmas the reconnection dynamics is dominated by nondissipative effects, mainly the Hall term and electron inertia. Reconnection rates are found to depend only on the ion mass, being independent of the electron inertia and the residual dissipation coefficients. Small-scale whistler turbulence is readily excited giving rise to an anomalous electron viscosity. Hence reconnection may be much more rapid than predicted by conventional resistive theory.

Affiliated with

Also associated with

No associations

Rating

Magnetic Reconnection in Plasmas does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Magnetic Reconnection in Plasmas, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetic Reconnection in Plasmas will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1643664