It is found that there exists an empirical linear relation between the high frequency $ high$ and low frequency $ low$ of quasi-periodic oscillations (QPOs) for black hole candidate (BHC), neutron star (NS) and white dwarf (WD) in the binary systems, which spans five orders of magnitude in frequency. For the NS Z (Atoll) sources, $ u_{high}$ and $ u_{low}$ are identified as the lower kHz QPO frequency and horizontal branch oscillations (HBOs) $ h$ (broad noise components); for the black hole candidates and low-luminosity neutron stars, they are the QPOs and broad noise components at frequencies between 1 and 10 Hz; for WDs, they are the ``dwarf nova oscillations (DNOs) and QPOs of cataclysmic variables (CVs). To interpret this relation, our model ascribes $ u_{high}$ to the Alfven wave oscillation frequency at a preferred radius and $ u_{low}$ to the same mechanism at another radius. Then, we can obtain $ low = 0.08 high$ and the relation between the upper kHz QPO frequency $ t$ and HBO to be $ h simeq 56 ({rm Hz}) ( t/{rm kHz})^{2}$, which are in accordance with the observed empirical relations. Furthermore, some implications of model are discussed, including why QPO frequencies of white dwarfs and neutron stars span five orders of magnitude in frequency.
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