  Properties of plasmoid-dominated turbulent reconnection in a low-$\beta$
background plasma are investigated by resistive magnetohydrodynamic (MHD)
simulations. In the $\beta_{\rm in} < 1$ regime, where $\beta_{\rm in}$ is
plasma $\beta$ in the inflow region, the reconnection site is dominated by
shocks and shock-related structures and plasma compression is significant. The
effective reconnection rate increases from $0.01$ to $0.02$ as $\beta_{\rm in}$
decreases. We hypothesize that plasma compression allows faster reconnection
rate, and then we estimate a speed-up factor, based on a compressible MHD
theory. We validate our prediction by a series of MHD simulations. These
results suggest that the plasmoid-dominated reconnection can be twice faster
than expected in the $\beta \ll 1$ environment in a solar corona.
