  Mass-loss rate is one of the most important stellar parameters. We aim to
provide mass-loss rates as a function of subdwarf parameters and to apply the
formula for individual subdwarfs, to predict the wind terminal velocities, to
estimate the influence of the magnetic field and X-ray ionization on the
stellar wind, and to study the interaction of subdwarf wind with mass loss from
Be and cool companions. We used our kinetic equilibrium (NLTE) wind models with
the radiative force determined from the radiative transfer equation in the
comoving frame (CMF) to predict the wind structure of subluminous hot stars.
Our models solve stationary hydrodynamical equations, that is the equation of
continuity, equation of motion, and energy equation and predict basic wind
parameters. We predicted the wind mass-loss rate as a function of stellar
parameters, namely the stellar luminosity, effective temperature, and
metallicity. The derived wind parameters (mass-loss rates and terminal
velocities) agree with the values derived from the observations. The radiative
force is not able to accelerate the homogeneous wind for stars with low
effective temperatures and high surface gravities. We discussed the properties
of winds of individual subdwarfs. The X-ray irradiation may inhibit the flow in
binaries with compact components. In binaries with Be components, the winds
interact with the disk of the Be star. Stellar winds exist in subluminous stars
with low gravities or high effective temperatures. Despite their low mass-loss
rates, they are detectable in the ultraviolet spectrum and cause X-ray
emission. Subdwarf stars may lose a significant part of their mass during the
evolution. The angular momentum loss in magnetic subdwarfs with wind may
explain their low rotational velocities. Stellar winds are especially important
in binaries, where they may be accreted on a compact or cool companion.
(abridged)
