  We study the emissivity properties of a geometrically thin, optically thick,
steady accretion disc about a static boson star. Starting from a numerical
computation of the metric potentials and the rotational velocities of the
particles in the vicinity of the compact object, we obtain the power per unit
area, the temperature of the disc, and the spectrum of the emitted radiation.
In order to see if different central objects could be actually distinguished,
all these results are compared with the case of a central Schwarzschild black
hole of equal mass. We considered different situations both for the boson star,
assumed with and without self-interactions, and the disc, whose internal
commencement can be closer to the center than in the black hole case. We
finally make some considerations about the Eddington luminosity, which becomes
radially dependent for a transparent object. We found that, particularly at
high energies, differences in the emitted spectrum are notorious. Reasons for
that are discussed.
