  We study the quasi-periodic oscillations from the accretion disk around
rotating traversable wormholes by means of the resonance models. We investigate
the linear stability of the circular geodesic orbits in the equatorial plane
for a general class of wormhole geometries deriving analytical expressions for
the epicyclic frequencies. Since wormholes can often mimic black holes in the
astrophysical observations, we analyze the properties of the quasi-circular
oscillatory motion in comparison with the Kerr black hole. We demonstrate that
wormholes possess distinctive features, which can be observationally
significant. It is characteristic for the Kerr black hole that the orbital and
the epicyclic frequencies obey a constant ordering in the whole range of the
spin parameter. In contrast, for wormhole spacetimes we can have various types
of orderings between the frequencies in the different regions of the parametric
space. This enables the excitation of much more diverse types of resonances
including parametric and forced resonances of lower order, which could lead to
stronger observable signals. In addition, for co-rotating orbits the resonances
can be excited in a very close neighbourhood of the wormhole throat for a wide
range of values of the angular momentum, making wormholes a valuable laboratory
for testing strong gravity.
