We present preliminary results of modelling 2D magnetic reconnection in the solar transition region environment. Compressible magnetohydrodynamic (MHD) simulations are performed by using a 2D MHD code based on staggered meshes. The present work is an attempt to numerically simulate magnetic reconnection that occurs between newly emerging magnetic flux and the pre-existing network field, which is widely believed to cause explosive events observed in the solar atmosphere. The formation of asymmetric reconnection jets is demonstrated in this study. Nonlinear anisotropic thermal conduction, radiative losses, and volumetric heating are included in the energy equation in order to investigate the formation of reconnection jets more precisely, as these processes are of fundamental importance at that region. The role of both nonlinear anisotropic thermal conduction and radiative losses is found to be significant in the solar transition region.