Turbulent magnetic reconnection in 2D and 3D

Details Turbulent magnetic reconnection in 2D and 3D Turbulent magnetic reconnection in 2D and 3D

2010-03-12

arxiv.org/abs/1003.2656v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

2 pages, 2 figures, IAU proceedings

Scientific paper

Magnetic field embedded in a perfectly conducting fluid preserves its topology for all time. Although ionized astrophysical objects, like stars and galactic disks, are almost perfectly conducting, they show indications of changes in topology, `magnetic reconnection', on dynamical time scales. Reconnection can be observed directly in the solar corona, but can also be inferred from the existence of large scale dynamo activity inside stellar interiors. Solar flares and gamma ray busts are usually associated with magnetic reconnection. Previous work has concentrated on showing how reconnection can be rapid in plasmas with very small collision rates. Here we present numerical evidence, based on three dimensional simulations, that reconnection in a turbulent fluid occurs at a speed comparable to the rms velocity of the turbulence, regardless of the value of the resistivity. In particular, this is true for turbulent pressures much weaker than the magnetic field pressure so that the magnetic field lines are only slightly bent by the turbulence. These results are consistent with the proposal by Lazarian and Vishniac (1999) that reconnection is controlled by the stochastic diffusion of magnetic field lines, which produces a broad outflow of plasma from the reconnection zone. This work implies that reconnection in a turbulent fluid typically takes place in approximately a single eddy turnover time, with broad implications for dynamo activity and particle acceleration throughout the universe. In contrast, the reconnection in 2D configurations in the presence of turbulence depends on resistivity, i.e. is slow.

Affiliated with

Also associated with

No associations

Rating

Turbulent magnetic reconnection in 2D and 3D 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 Turbulent magnetic reconnection in 2D and 3D, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Turbulent magnetic reconnection in 2D and 3D will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-191177