  We discuss the possibility that high-frequency QPOs in neutron-star binary
systems may result from forced resonant oscillations of matter in the innermost
parts of the accretion disc, excited by gravitational perturbations coming from
asymmetries of the neutron star or from the companion star. We find that
neutron-star asymmetries could, in principle, be effective for inducing both
radial and vertical oscillations of relevant amplitude while the binary
companion might possibly produce significant radial oscillations but not
vertical ones. Misaligned neutron-star quadrupole moments of a size advocated
elsewhere for explaining limiting neutron star periods could be large enough
also for the present purpose.
