  We present H alpha emission line spectra of 7 post-AGB stars. Typically, they
have a P-Cygni type profile with a very strong emission component and a
relatively narrow absorption component. These lines are formed in the fast
post-AGB wind which in most cases has a velocity of around 100 km/s. Hence the
emission originates close to the central star and the absorption occurs in the
fast wind itself or in the region where the fast wind sweeps up the slow wind.
The emission profile has very broad wings. It is still unclear what causes
these wings.
