  Motivated by recent studies showing an apparent correlation between the
high-frequency quasi-periodic oscillations (QPOs) and the low-frequency, type-C
QPO in low-mass, black hole X-ray binaries (LMXBs), we explore a model that
explains all three QPOs in terms of an oscillating, precessing hot flow in the
truncated-disk geometry. Our model favors attributing the two high-frequency
QPOs, often occurring in a near 3:2 frequency ratio, to the breathing and
vertical epicyclic frequency modes of the hot, thick flow, although we can not
rule out the Keplerian and m=-1 radial epicyclic modes. In either case, the
type-C QPO is attributed to precession. The correlation of the QPOs comes from
the fact that all three frequencies are associated with the same geometrical
structure. While the exact QPO frequencies are sensitive to the black hole mass
and spin, their evolution over the course of an outburst is mainly tied to the
truncation radius between the geometrically thin, optically thick disk and the
inner, hot flow. We show that, in the case of the LMXB GRO J1655-40, this model
can explain the one simultaneous observation of all three QPOs and that an
extrapolation of the model appears to match lower frequency observations where
only two of the three components are seen. Thus, this model may be able to
unify multiple QPO observations using the properties of a single, simple,
geometrical model.
