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It is found that there exists an empirical linear relation between the highfrequency $\nhigh$ and low frequency $\nlow$ 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,  $\nu_{high}$ and $\nu_{low}$ are identified as the lower kHz QPO frequencyand horizontal branch oscillations (HBOs) $\nh$ (broad noise components); forthe black hole candidates and low-luminosity neutron stars, they are the QPOsand broad noise components at frequencies between 1 and 10 Hz; for WDs, theyare the ``dwarf nova oscillations'' (DNOs) and QPOs of cataclysmic variables(CVs). To interpret this relation, our model ascribes $\nu_{high}$ to theAlfv\'en wave oscillation frequency at a preferred radius and $\nu_{low}$ tothe same mechanism at another radius. Then, we can obtain $\nlow = 0.08  \nhigh$ and the relation between the upper kHz QPO frequency $\nt$ and HBO tobe $\nh \simeq 56 ({\rm Hz}) (\nt/{\rm kHz})^{2}$, which are in accordance withthe observed empirical relations. Furthermore, some implications of model arediscussed, including why QPO frequencies of white dwarfs and neutron stars spanfive orders of magnitude in frequency. \\Comment: 11 pages, 1 figure, accepted by PAS

Interpretations for Low‐ and High‐Frequency QPO Correlations of X‐Ray Sources among White Dwarfs, Neutron Stars, and Black Holes