Eclipses BY the Wolf-Rayet component of V444 Cyg will be used to chart
 density (hence expansion velocity) and clumping with height in the WR wind.
 Similarly, eclipses OF the Wolf-Rayet component will be used to measure
 electron temperature throughout the inner 10 WR radii of the wind where the
 gas is accelerating rapidly.  These data will therefore give us a complete
 detailed empirical model of the outer atmosphere of a WR star.  This model
 will then provide the means of determining precisely where energy and momentum
 must be injected into the wind to produce the observed mass loss, which in turn
 will confront theories for driving winds in hot stars.  The degree of clumping,
 for example, determines the local pressures available for driving the wind,
 which will depend on the driving force field.