  We present the results of Monte Carlo mass-loss predictions for hot low-mass
stars, specifically for Subdwarf B (SdB) stars. It is shown that the mass-loss
rates on the Horizontal Branch (HB) computed from radiative line-driven wind
models are not high enough to create SdB stars. We argue, however, that the
mass loss plays a role in the chemical abundance patterns observed both in
field SdB stars, as well as in cluster HB stars. The derived mass loss recipe
for these (extremely) hot HB stars may also be applied to other groups of hot
low-mass stars, such as post-HB (AGB-manque, UV-bright) stars, over a range in
effective temperatures between 10000 and 50000 Kelvin. Finally, we present
preliminary spectral synthesis on the more luminous SdB stars for which
emission cores in Halpha have been detected (Heber et al. 2002). We find that
these line profiles can indeed be interpreted as the presence for a stellar
wind with mass loss of the order of log(Mdot) = -11 (Msun/year).
