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Superhalo electrons appear to be continuously present in the interplanetarymedium, even at very quiet times, with a power-law spectrum at energies above$\sim$2 keV. Here we numerically investigate the generation of superhaloelectrons by magnetic reconnection in the solar wind source region, using theMHD and test particle simulations for both single X-line reconnection andmultiple X-line reconnection. We find that the direct current electric field,produced in the magnetic reconnection region, can accelerate electrons from aninitial thermal energy of T $\sim10^5$ K up to hundreds of keV. Afteracceleration, some of the accelerated electrons, together with the nascentsolar wind flow driven by the reconnection, propagate upwards along thenewly-opened magnetic field lines into the interplanetary space, while the restmove downwards into the lower atmosphere. Similar to the observed superhaloelectrons at 1 AU, the flux of the upward-traveling accelerated electronsversus energy displays a power-law distribution at $\sim$ 2 $-$ 100 keV, $f(E)\sim E^{-\delta}$, with a $\delta$ of $\sim$ 1.5 $-$ 2.4. For single (multiple)X-line reconnection, the spectrum becomes harder (softer) as the anomalousresistivity parameter $\alpha$ (uniform resistivity $\eta$) increases. Thesemodeling results suggest that the acceleration in the solar wind source regionmay contribute to superhalo electrons.

Numerical Simulation of Superhalo Electrons Generated by Magnetic Reconnection in the Solar Wind Source Region