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We simulate several magnetic reconnection processes in the low solarchromosphere/photosphere, the radiation cooling, heat conduction and ambipolardiffusion are all included. Our numerical results indicate that both the hightemperature($ \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 byplasma density and magnetic fields is one important factor to decide how muchthe plasma can be heated up. The low temperature event is formed in a high$\beta$ magnetic reconnection process, Joule heating is the main mechanism toheat plasma and the maximum temperature increase is only several thousandKelvin. The high temperature explosions can be generated in a low $\beta$magnetic reconnection process, slow and fast-mode shocks attached at the edgesof the well developed plasmoids are the main physical mechanisms to heat theplasma from several thousand Kelvin to over $8\times10^4$~K. Gravity in the lowchromosphere can strongly hinder the plasmoind instability and the formation ofslow-mode shocks in a vertical current sheet. Only small secondary islands areformed; these islands, however, are not well developed as those in thehorizontal current sheets. This work can be applied for understanding theheating mechanism in the low solar atmosphere and could possibly be extended toexplain the formation of common low temperature EBs ($\sim10^4$~K) and the hightenperature IRIS bombs ($\gtrsim 8\times10^4$) in the future.

Heating mechanisms in the low solar atmosphere through magnetic reconnection in current sheets