Asymmetric Magnetic Reconnection: General Theory and Collisional Simulations

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Circulation of Heavy Ions and Their Dynamical Effects in the Magnetosphere: Recent Observations and Models (2014, methodology): “Using prescribed cusp and nightside auroral outflow, this effect was quantified using the Cassak-Shay formula for reconnection rate (Cassak and Shay 2007) and by integrating the reconnection electric field across the X-line to get a total dawn-dusk potential drop.”
Smilei : A collaborative, open-source, multi-purpose particle-in-cell code for plasma simulation (2017, methodology): “Using the Cassak-Shay estimate of the inflow velocity [66], we need to position the plume on the magnetospheric side at about 20 c/ωpi from the initial magnetopause position.”
Altered solar wind-magnetosphere interaction at low Mach numbers: Coronal mass ejections (2008, background): “…l-0 03 77 24 0, v er si on 1 - 21 A pr 2 00 9 Theory and simulations show that four parameters govern the reconnection rate for non-identical plasmas: the magnetic field strengths and the mass densities on each side of the reconnection site [Cassak and Shay, 2007; see also Swisdak and Drake, 2007].”
Collisionless magnetic reconnection in an asymmetric current sheet (2008, background): “[33] In initial-value simulations, the reconnection rate was found to be considerably smaller (cEy/vAB0 � 0.03–0.04, corresponding to a Cassak and Shay [2007] reconnection rate parameter ~”