  In previous work, we derived the most general solution of the collisionless
Boltzmann equation describing the accretion of a kinetic gas into a
Schwarzschild black hole background, and we gave explicit expressions for the
corresponding observables (the current density and stress energy-momentum
tensor) in terms of certain integrals over the distribution function. In this
article, we numerically compute these integrals for the particular case of the
steady-state, spherical symmetric accretion flows which, at infinity, are
described by an equilibrium distribution function of given temperature. We
analyze in detail the behavior of the observables as a function of the
temperature and the radial coordinate, comparing our results with the perfect
fluid model of Bondi-Michel accretion.
