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Recent observations at high spatial resolution have shown that magnetic fluxcancellation occurs on the solar surface much more frequently than previouslythought, and so this led Priest et al 2018 to propose magnetic reconnectiondriven by photospheric flux cancellation as a mechanism for chromospheric andcoronal heating. In particular, they estimated analytically the amount ofenergy released as heat and the height of the energy release during fluxcancellation. In the present work, we take the next step in the theory bysetting up a two-dimensional resistive MHD simulation of two cancelingpolarities in the presence of a horizontal external field and a stratifiedatmosphere in order to check and improve upon the analytical estimates.Computational evaluation of the energy release during reconnection is found tobe in good qualitative agreement with the analytical estimates. In addition, wego further and undertake an initial study of the atmospheric response toreconnection. We find that, during the cancellation, either hot ejections orcool ones or a combination of both hot and cool ejections can be formed,depending on the height of the reconnection location. The hot structures canhave the density and temperature of coronal loops, while the cooler structuresare suggestive of surges and large spicules.

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating II. 2D Theory and Simulations