  We predict mass-loss rates for the late evolutionary phases of low-mass
stars, with special emphasis on the consequences for the morphology of the
Horizontal Branch (HB). We show that the computed rates, as predicted by the
most plausible mechanism of radiation pressure on spectral lines, are too low
to produce EHB/sdB stars. This invalidates the scenario recently outlined by
Yong et al. (2000) to create these objects by mass loss on the HB. We argue,
however, that mass loss plays a role in the distribution of rotational
velocities of hot HB stars, and may -- together with the enhancement of heavy
element abundances due to radiative levitation -- provide an explanation for
the so-called ``low gravivity problem. The mass loss recipe derived for hot HB
(and extreme HB, sdB, sdOB) stars may also be applied to post-HB (AGB-manque,
UV-bright) stars over a range in effective temperatures between 12500 -- 40000
K.
