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In this paper we propose that flux cancellation on small granular scales($\lesssim 1000$ km) ubiquitously drives reconnection at a multitude of sitesin the low solar atmosphere, contributing to chromospheric/coronal heating andthe generation of the solar wind. We analyse the energy conversion in thesesmall-scale flux cancellation events using both analytical models andthree-dimensional, resistive magnetohydrodynamic (MHD) simulations. Theanalytical models -- in combination with the latest estimates of fluxcancellation rates -- allow us to estimate the energy release rates due tocancellation events, which are found to be of the order $10^6-10^7$ ergcm$^{-2}$sec$^{-1}$, sufficient to heat the chromosphere and corona of theQuiet Sun and active regions, and to power the solar wind. The MHD simulationsconfirm the conversion of energy in reconnecting current sheets, in a geometryrepresenting a small-scale bipole being advected towards an intergranular lane.A ribbon-like jet of heated plasma is accelerated upwards, that could alsoescape the Sun as the solar wind in an open-field configuration. We concludethat through two phases of atmospheric energy release -- pre-cancellation andcancellation -- the cancellation of photospheric magnetic flux fragments andthe associated magnetic reconnection may provide a substantial energy and massflux contribution to coronal heating and solar wind generation.

Coronal Heating and Solar Wind Generation by Flux Cancellation Reconnection