The temperature and density configuration in the solar chromosphere results in a partially ionised plasma. This introduces a perpendicular component of resistivity (Cowling resistivity) which acts perpendicular to the magnetic field and aids diffusion in the plasma. Taking as initial condition a Harris current sheet in equilibrium, a velocity driver is specified far from the centre of the current sheet which creates a propagating wave that triggers the 2D reconnection event. The start-up and reconnection phases are then analysed to determine the behaviour of reconnection in the solar chromosphere.