  Observations of X-ray emissions from binary systems have always been
considered important tools to test the validity of General Relativity in
strong-field regimes. The pairs and triplets of high frequency quasi-periodic
oscillations observed in binaries containing a black hole candidate, in
particular, have been proposed as a means to measure more directly the black
hole properties such as its mass and spin. Numerous models have been suggested
over the years to explain the QPOs and the rich phenomenology accompanying
them. Many of these models rest on a number of assumptions and are at times in
conflict with the most recent observations. We here propose a new, simple model
in which the QPOs result from basic p-mode oscillations of a non-Keplerian disc
of finite size. We show that within this new model all of the key properties of
the QPOs: a) harmonic ratios of frequencies even as the frequencies change; b)
variations in the relative strength of the frequencies with spectral energy
distribution and with photon energy; c) small and systematic changes in the
frequencies, can all be explained simply given a single reasonable assumption.
