Neither the collisional hydrodynamic nor the collisionless kinetic models have yet been able to fully explain the acceleration of the fast solar wind without ad hoc assumptions of additional energy input or suprathermal electron populations at the base of the models in the lower corona. Separate research has shown that plasma naturally forms a Current Free Double Layer when expanding into a lower-density region, the effect of which is to generate a suprathermal electron population and beams of fast ions on the low potential side. It is suggested that the expansion of the dense plasma in the body of the Sun will form a stationary Current Free Double Layer below the photosphere and thus provide initial ion acceleration together with the type of electron velocity distribution function that kinetic models require as boundary conditions. The turbulence generated by the outflowing particle beams colliding with the low-density plasma in and above the upper chromosphere may contribute to the additional wave energy which the hydrodynamic models require. The implications of the present model for the coronal heating problem are also explored.