High-Lundquist Number Resistive MHD Simulations of Turbulent Magnetic Reconnection with Secondary Island Formation and Enhanced Reconnection Rate

Details High-Lundquist Number Resistive MHD Simulations of Turbulent Magnetic Reconnection with Secondary Island Formation and Enhanced Reconnection Rate High-Lundquist Number Resistive MHD Simulations of Turbulent Magnetic Reconnection with Secondary Island Formation and Enhanced Reconnection Rate

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm51c1836r&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM51C-1836

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Computation

[0545] Computational Geophysics / Modeling, [2723] Magnetospheric Physics / Magnetic Reconnection, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7863] Space Plasma Physics / Turbulence

Scientific paper

We present our latest results based on large-scale two dimensional resistive magnetohydrodynamic (MHD) simulations for the magnetic reconnection process in the configuration of island coalescence instability. These simulations are performed using a fairly standard pseudo spectral code, which has been well tested for accuracy, convergence, and compared well with codes using other methods. Cases with a range of Lundquist number S are run using resolutions up to 81922 and thus with S up to 2 × 105. It is found that the reconnection rate is consistent with the Sweet-Parker theory with no tearing instability of the Sweet-Parker current sheet or secondary island (plasmoid) formation when simulations are well resolved and without external noise. However, secondary islands have been observed to form, with faster reconnection rate in simulations superimposed with turbulence (noise). We will present results on the scaling of reconnection rate with S, as well as turbulence levels. This work is supported by a NASA grant NNX08BA71G, and a NSF grant AGS-0962477.

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