  We simulate several magnetic reconnection processes in the low solar
chromosphere/photosphere, the radiation cooling, heat conduction and ambipolar
diffusion are all included. Our numerical results indicate that both the high
temperature($ \gtrsim 8\times10^4$~K) and low temperature($\sim 10^4$~K)
magnetic reconnection events can happen in the low solar atmosphere
($100\sim600$~km above the solar surface). The plasma $\beta$ controlled by
plasma density and magnetic fields is one important factor to decide how much
the plasma can be heated up. The low temperature event is formed in a high
$\beta$ magnetic reconnection process, Joule heating is the main mechanism to
heat plasma and the maximum temperature increase is only several thousand
Kelvin. The high temperature explosions can be generated in a low $\beta$
magnetic reconnection process, slow and fast-mode shocks attached at the edges
of the well developed plasmoids are the main physical mechanisms to heat the
plasma from several thousand Kelvin to over $8\times10^4$~K. Gravity in the low
chromosphere can strongly hinder the plasmoind instability and the formation of
slow-mode shocks in a vertical current sheet. Only small secondary islands are
formed; these islands, however, are not well developed as those in the
horizontal current sheets. This work can be applied for understanding the
heating mechanism in the low solar atmosphere and could possibly be extended to
explain the formation of common low temperature EBs ($\sim10^4$~K) and the high
tenperature IRIS bombs ($\gtrsim 8\times10^4$) in the future.
