  Nanoflare models for heating the solar corona usually assume magnetic
braiding and reconnection as the source of the energy. However, recent
observations at record spatial resolution from the {\sc Sunrise} balloon
mission suggest that photospheric magnetic flux cancellation is much more
common than previously realised. We therefore examine the possibility of
three-dimensional reconnection driven by flux cancellation as a cause of
chromospheric and coronal heating. In particular, we estimate how the heights
and amount of energy release produced by flux cancellation depend on flux size,
flux cancellation speed and overlying field strength.
