High-frequency quasi-periodic oscillations (HF QPOs) which appear in the X-ray fluxes of low-mass X-ray binaries remain an unexplained phenomenon. Among other ideas it was suggested that a non-linear resonance between two oscillation modes in an accretion disc orbiting a black hole or a neutron star plays role in exciting the observed modulation. Several possible resonances have been discussed. A particular model assumes disc-oscillation modes with the resonant eigenfrequencies equal to radial and vertical epicyclic frequency of geodesic orbital motion. This model has been discussed for black hole microquasar sources as well as for a group of neutron star sources. Assuming several neutron (strange) star equations of state and Hartle-Thorne geometry of rotating stars, we briefly compare the frequencies expected from the model to those observed. Our comparison implies the neutron star radius RNS to be larger than is the related radius of the marginally stable circular orbit rms for nuclear matter equations of state and spin frequencies up to 800Hz. For the same range of spin and a strange star (MIT) equation of state, it is RNS ∼ rms . The ”Paczynski modulation” mechanism considered within the model requires RNS < rms . However, we have found this condition to be fulfilled only for the strange matter equation of state, masses below 1M⊙ , and spin frequencies above 800Hz. This result most likely falsifies the postulation of the neutron star 3:2 resonant eigenfrequencies being equal to the frequencies of geodesic radial and vertical epicyclic modes. We suggest that the 3:2 epicyclic modes could stay among the possible choices only if a fairly non-geodesic accretion flow is assumed, or if a different modulation mechanism operates.