We outline a theory for the origin and acceleration of the fast solar wind
as a consequence of network microflares releasing a spectrum of high freque
ncy Alfven waves which heat (by cyclotron absorption) the corona close to t
he Sun. The significant features of our model of the fast wind are that the
acceleration is rapid with the sonic point at around two solar radii, the
proton temperatures are high (similar to 5 million degrees) and the minor i
ons are correspondingly hotter roughly in proportion to their mass. Moreove
r we argue that since the energy flux needed to power the quiet corona in c
losed field regions is about the same as that needed to drive the fast sola
r wind, and also because at deeper levels (< 2 x 10(5) K) there is no great
difference in the properties of supergranules and network in closed and op
en field regions, the heating process (i.e., dissipation of high frequency
waves) must be the same in both cases.