  We calculate the disk and boundary layer luminosities for accreting rapidly
rotating neutron stars with low magnetic fields in a fully general relativistic
manner. Rotation increases the disk luminosity and decreases the boundary layer
luminosity. A rapid rotation of the neutron star substantially modifies these
quantities as compared to the static limit. For a neutron star rotating close
to the centrifugal mass shed limit, the total luminosity has contribution only
from the extended disk. For such maximal rotation rates, we find that much
before the maximum stable gravitational mass configuration is reached, there
exists a limiting central density, for which particles in the innermost stable
orbit will be more tightly bound than those at the surface of the neutron star.
We also calculate the angular velocity profiles of particles in Keplerian
orbits around the rapidly rotating neutron star. The results are illustrated
for a representative set of equation of state models of neutron star matter.
