  We present a method to derive outflow velocities in the solar corona using
different data sets including solar wind mass flux coming from the SWAN/SOHO
instrument, electron density values from LASCO-C2 and interplanetary solar wind
velocities derived from ground-based Interplanetary Scintillation Observations
(IPS).
  In a first step, we combine the LASCO electron densities at 6 solar radii and
the IPS velocities, and compare the product to the SWAN mass fluxes. It is
found that this product represents the actual mass flux at 6 solar radii for
the fast wind, but not for the slow wind. In regions dominated by the slow
wind, the fluxes derived from SWAN are systematically smaller. This is
interpreted as a proof that the fast solar wind has reached its terminal
velocity at about 6 solar radii and expands with constant velocity beyond this
distance. On the contrary, the slow solar wind has reached only half of its
terminal value and is thus accelerated further out.
  In a second step, we combine the LASCO-C2 density profiles and the SWAN flux
data to derive velocity profiles in the corona between 2.5 and 6 solar radii.
Such profiles can be used to test models of the acceleration mechanism of the
fast solar wind.
