Can turbulent reconnection be fast in 2D?
نویسندگان
چکیده
منابع مشابه
Fast Reconnection of Magnetic Fields in Turbulent Fluids
Reconnection is the process by which magnetic fields in a conducting fluid change their topology. This process is essential for understanding a wide variety of astrophysical processes, including stellar and galactic dynamos and astrophysical turbulence. To account for solar flares, solar cycles, and the structure of the galactic magnetic field, reconnection must be fast, propagating with a spee...
متن کاملOn Turbulent Reconnection
We examine the dynamics of turbulent reconnection in 2D and 3D reduced MHD by calculating the effective dissipation due to coupling between small–scale fluctuations and large–scale magnetic fields. Sweet–Parker type balance relations are then used to calculate the global reconnection rate. Two approaches are employed — quasi–linear closure and an eddy-damped fluid model. Results indicate that d...
متن کاملExplosive turbulent magnetic reconnection.
We report simulation results for turbulent magnetic reconnection obtained using a newly developed Reynolds-averaged magnetohydrodynamics model. We find that the initial Harris current sheet develops in three ways, depending on the strength of turbulence: laminar reconnection, turbulent reconnection, and turbulent diffusion. The turbulent reconnection explosively converts the magnetic field ener...
متن کاملTurbulent reconnection and its implications.
Magnetic reconnection is a process of magnetic field topology change, which is one of the most fundamental processes happening in magnetized plasmas. In most astrophysical environments, the Reynolds numbers corresponding to plasma flows are large and therefore the transition to turbulence is inevitable. This turbulence, which can be pre-existing or driven by magnetic reconnection itself, must b...
متن کاملTurbulent Magnetic Reconnection in Two Dimensions
Two-dimensional numerical simulations of the effect of background turbulence on 2D resistive magnetic reconnection are presented. For sufficiently small values of the resistivity (η) and moderate values of the turbulent power ( ), the reconnection rate is found to have a much weaker dependence on η than the Sweet-Parker scaling of η and is even consistent with an η-independent value. For a give...
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ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2010
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921311017911