  We examine the influence of the quadrupole moment of a slowly rotating
neutron star on the oscillations of non-slender accretion tori. We apply
previously developed methods to perform analytical calculations of frequencies
of the radial epicyclic mode of a torus in the specific case of the
Hartle-Thorne geometry. We present here our preliminary results and provide a
brief comparison between the calculated frequencies and the frequencies
previously obtained assuming both standard and linearized Kerr geometry.
Finally, we shortly discuss the consequences for models of high-frequency
quasi-periodic oscillations observed in low-mass X-ray binaries.
