What determines the reconnection rate at the dayside magnetosphere

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Circulation of Heavy Ions and Their Dynamical Effects in the Magnetosphere: Recent Observations and Models (2014, result): “A similar result was found in roundabout fashion in an earlier, single-fluid MHD investigation of reconnection rates (Borovsky et al. 2008).”
Substorm and magnetosphere characteristic scales inferred from the SuperMAG auroral electrojet indices (2011, background): “Figure 9 shows the distribution of several possible driving functions (based on 10 min averages), including Bz, EKL, dFMP/dt, and the Borovsky function [Borovsky et al., 2008].”
Altered solar wind-magnetosphere interaction at low Mach numbers: Coronal mass ejections (2008, methodology): “Twodimensional [Borovsky and Hesse, 2007; Birn et al., 2007] and three-dimensional [Borovsky et al., 2008a] MHD simulations were performed to determine the parameters that control such asymmetric magnetic reconnection.”
A statistical look at plasmaspheric drainage plumes (2008, background): “…is where does the plasmaspheric-plume plasma go after the flux tubes are opened by dayside reconnection [Freeman et al., 1977; Elphic et al., 1997; Su et al., 2001b] and does this drained plasma impact the mechanics of the magnetosphere [Borovsky et al., 2008; Borovsky and Steinberg, 2006].”