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Inspired by recent observations suggesting that photospheric magnetic fluxcancellation occurs much more frequently than previously thought, weanalytically estimated the energy released from reconnection driven byphotospheric flux cancellation, and proposed that it can act as a mechanism forchromospheric and coronal heating (Priest et al., 2018). Using two-dimensionalsimulations we validated the analytical estimates and studied the resultingatmospheric response (Syntelis et al. 2019). In the present work, we set upthree-dimensional resistive MHD simulations of two cancelling polarities in astratified atmosphere with a horizontal external field to further validate andimprove upon the analytical estimates. The computational evaluation of theparameters associated with the energy release are in good qualitative agreementwith the analytical estimates. The computational Poynting energy flux into thecurrent sheet is in good qualitative agreement with the analytical estimates,after correcting the analytical expression to better account for the horizontalextent of the current sheet. The atmospheric response to the cancellation isthe formation of hot ejections, cool ejections, or a combination of both hotand cool ejections, which can appear with a time difference and/or be spatiallyoffset, depending on the properties of the cancelling region and the resultingheight of the reconnection. Therefore, during the cancellation, a wide spectrumof ejections can be formed, which can account for the variety of multi-thermalejections associated with Ellerman bombs, UV bursts and IRIS bombs, and alsoother ejections associated with small-scale cancelling regions and spicules.

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating III. 3D Simulations and Atmospheric Response