Acceleration of the fast solar wind by the emergence of new magnetic flux

Recent observations have shown that small magnetic loops are continuously e merging within supergranules in the solar photosphere. The subsequent recon nection of this emerging flux with field lines which open into the corona s hould define the Poynting's vector and mass flux into the corona. These two quantities uniquely determine the final energy flow and speed of the stead y, fast solar wind. It is also pointed out that if the consequence of the e mergence of new flux and its reconnection is lateral displacements of coron al magnetic field lines, this process should increase the magnetic field en ergy in the corona in a definable manner. The resulting dissipation of this energy, by work done on the plasma or by Joule heating, defines the spatia l distribution for the heating of the corona. A simple model is constructed that yields profiles for the acceleration of the fast solar wind and for c oronal temperatures that are reasonable.