  Superhalo electrons appear to be continuously present in the interplanetary
medium, even at very quiet times, with a power-law spectrum at energies above
$\sim$2 keV. Here we numerically investigate the generation of superhalo
electrons by magnetic reconnection in the solar wind source region, using the
MHD and test particle simulations for both single X-line reconnection and
multiple X-line reconnection. We find that the direct current electric field,
produced in the magnetic reconnection region, can accelerate electrons from an
initial thermal energy of T $\sim10^5$ K up to hundreds of keV. After
acceleration, some of the accelerated electrons, together with the nascent
solar wind flow driven by the reconnection, propagate upwards along the
newly-opened magnetic field lines into the interplanetary space, while the rest
move downwards into the lower atmosphere. Similar to the observed superhalo
electrons at 1 AU, the flux of the upward-traveling accelerated electrons
versus 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 anomalous
resistivity parameter $\alpha$ (uniform resistivity $\eta$) increases. These
modeling results suggest that the acceleration in the solar wind source region
may contribute to superhalo electrons.
