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We study the quasi-periodic oscillations from the accretion disk aroundrotating traversable wormholes by means of the resonance models. We investigatethe linear stability of the circular geodesic orbits in the equatorial planefor a general class of wormhole geometries deriving analytical expressions forthe epicyclic frequencies. Since wormholes can often mimic black holes in theastrophysical observations, we analyze the properties of the quasi-circularoscillatory motion in comparison with the Kerr black hole. We demonstrate thatwormholes possess distinctive features, which can be observationallysignificant. It is characteristic for the Kerr black hole that the orbital andthe epicyclic frequencies obey a constant ordering in the whole range of thespin parameter. In contrast, for wormhole spacetimes we can have various typesof orderings between the frequencies in the different regions of the parametricspace. This enables the excitation of much more diverse types of resonancesincluding parametric and forced resonances of lower order, which could lead tostronger observable signals. In addition, for co-rotating orbits the resonancescan be excited in a very close neighbourhood of the wormhole throat for a widerange of values of the angular momentum, making wormholes a valuable laboratoryfor testing strong gravity.

Quasi-periodic oscillations from the accretion disk around rotating traversable wormholes