  The recent model of quasi-periodic oscillations in neutron star binaries
(Osherovich and Titarchuk 1999, Titarchuk and Osherovich 1999) has suggested
the existence of two branches of QPOs due to the influence of Coriolis force on
the linear Keplerian oscillator: one branch with frequencies from 400 to 1200
Hz and another branch with frequencies an order of magnitude lower. The
frequencies of the high branch nu_h hold a hybrid frequency relation with the
Keplerian frequency nu_K: nu_h^2=nu_K^2+ [Omega/pi]^2, where Omega is the
rotational frequency of the star's magnetosphere. The frequency of the low
branch is nu_L=(Omega/pi)(nu_K/nu_h) sin(delta), where delta is a small angle
between vector Omega and the vector normal to the plane of Keplerian
oscillations. The observations of the source 4U 1702-42 (Markwardt et al 1999)
have shown that the centroid of the 35 Hz QPO tracks the frequency of the
kilohertz oscillations. We interpret the 35 Hz oscillations as nu_L and find
delta=3.9^o +/- 0.2^o. Our results make 4U 1702-42 the second source (after Sco
X-1) for which the theoretically derived lower branch is identified (within our
model) and delta is calculated. The inferred angle delta stays approximately
the same over the significant range of nu_K (650 - 900 Hz), as expected from
the model. Based on our model we present a classification of QPO frequencies in
the source 4U 1702-42 observed above and below nu_L.
