Effects of turbulence on magnetic reconnection: 3D numerical simulations Conferences

abstract

• AbstractTurbulent reconnection is studied by means of three dimensional (3D) compressible magnetohydrodynamical numerical calculations. The process of homogeneous turbulence is set up by adding three-dimensional solenoidal random forcing implemented in the spectral space at small wave numbers with no correlation between velocity and forcing. We apply the initial Harris current sheet configuration together with a density profile calculated from the numerical equilibrium of magnetic and gas pressures. We assume that there is no external driving of the reconnection. The reconnection develops as a result of the initial vector potential perturbation. We use open boundary conditions. Our main goal is to find the dependencies of reconnection rate on different properties of turbulence. The results of our simulations show that turbulence significantly affects the topology of magnetic field near the diffusion region. We present that the reconnection speed does not depend on the Reynolds numbers as well the magnetic diffusion. In addition, a fragmentation of current sheet decreases the disparity in inflow/outflow ratios. When we apply the large scale and more powerful turbulence the reconnection is faster.

authors

• Otmianowska-Mazur, Katarzyna
• Kowal, G
• Lazarian, A
• Vishniac, Ethan

status

• published 

publication date

• November 2008

has subject area

• 0201 Astronomical and Space Sciences (FoR)

published in

• Proceedings of the International Astronomical Union  Journal

presented at event

• 259th Symposium of the International-Astronomical-Union  Conference

keywords

• Astronomy & Astrophysics
• MHD
• Physical Sciences
• Science & Technology
• magnetic fields
• numerical simulations
• turbulence

Digital Object Identifier (DOI)

• 10.1017/s1743921309031536

International Standard Book Number (ISBN) 13

• 978-0-521-88990-2

start page

• 671

end page

• 674

volume

• 4

issue

• S259