  It is clear that the solar corona is being heated and that coronal magnetic
fields undergo reconnection all the time. Here we attempt to show that these
two facts are in fact related - i.e. coronal reconnection generates heat. This
attempt must address the fact that topological change of field lines does not
automatically generate heat. We present one case of flux emergence where we
have measured the rate of coronal magnetic reconnection and the rate of energy
dissipation in the corona. The ratio of these two, $P/\dot{\Phi}$, is a current
comparable to the amount of current expected to flow along the boundary
separating the emerged flux from the pre-existing flux overlying it. We can
generalize this relation to the overall corona in quiet Sun or in active
regions. Doing so yields estimates for the contribution to corona heating from
magnetic reconnection. These estimated rates are comparable to the amount
required to maintain the corona at its observed temperature.
