Scaling of Reconnection and Stability of Current Sheets in Large Systems

Details Scaling of Reconnection and Stability of Current Sheets in Large Systems Scaling of Reconnection and Stability of Current Sheets in Large Systems

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh43a..06y&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH43A-06

Physics

2723 Magnetic Reconnection (7526, 7835), 7513 Coronal Mass Ejections (2101), 7519 Flares, 7831 Laboratory Studies And Experimental Techniques, 7835 Magnetic Reconnection (2723, 7526)

Scientific paper

The scaling of collisionless reconnection in large systems has been a subject of considerable interest recently. We have carried out a sequence of 2D simulations using the same initial conditions for large systems using resistive MHD, Hall MHD and fully kinetic particle-in-cell models. It is shown that the dynamics of thin current sheets is sensitive to the mechanism that breaks field lines (spatially uniform resistivity, electron inertia, and/or electron pressure tensor), and that velocity shear along the thin current sheets plays an important role in controlling their geometry and stability. In the resistive MHD model, the long thin current sheet spanning Y-points becomes near-explosively unstable to secondary tearing, producing plasmoids copiously. In Hall MHD, the nonlinear dynamics changes qualitatively, as the Y-points contract spontaneously to form X-points thwarting the secondary tearing instabilities seen in the resistive MHD study. A steady state is eventually realized due to a balance between the spatial gradients of the current density and the velocity shear. Collisionless PIC simulations show a very different dynamics, exhibiting the tendency to form extended thin current sheets and secondary tearing instabilities. We address the issue of scaling in all three models, especially the dependence on system size and the dissipation mechanism, and discuss the relevance of these results to solar flares and magnetospheric substorms.

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