  We consider a time dependent, spherically outflowing wind, in Schwarzschild
space-time, consisting of electron-positron pairs and photons . Without
assuming thermal equilibrium, we account for the microphysics, including
two-body processes and their radiative three-body variants. We present a
finite-difference scheme for solving the general relativistic kinetic Boltzmann
equations for electron-positron pairs and photons. We apply this to the
concrete example of a wind from a hot, bare, strange star, predicted to be a
powerful source of hard X-ray photons and pairs created by the Coulomb barrier
at the quark surface. We study the kinetics of the wind particles and the
emerging emission in photons and pairs for stationary winds with total
luminosities in the range 10^{34}-10^{39} ergs/s, for different values of the
injected photon-to-pair ratio. The wind parameters--such as the mean optical
depth for photons, the rates of particle number and energy outflows, bulk
velocity, and number density of the pair plasma--are presented as functions of
the distance from the stellar surface, as well as characteristics of the
emergent radiation. We find that photons dominate in the emerging emission, and
the emerging photon spectrum is rather hard and differs substantially from the
thermal spectrum expected from a neutron star with the same luminosity. This
might help distinguish the putative bare strange stars from neutron stars.
