  Detailed analysis of kinematics of the Milky Way disk in the solar
neighborhood based on the GAIA DR3 catalog reveals the existence of
peculiarities in the stellar velocity distribution perpendicular to the
galactic plane. We study the influence of resonances -- the outer Lindblad
resonance and the outer vertical Lindblad resonance -- of a rotating bar with
stellar oscillations perpendicular to the plane of the disk, and their role in
shaping the spatial and the velocity distributions of stars. We find that the
$Z$ and $V_Z$ distributions of stars with respect to $L_Z$ are affected by the
outer Lindblad resonance. The existence of bar resonance with stellar
oscillations perpendicular to the plane of the disk is demonstrated for a long
(large semi-axis 5 kpc) and fast rotating bar with $\Omega_{b}= 60.0$
$km~s^{-1}~kpc^{-1}$. We show also that, in the model with the long and fast
rotating bar, some stars in the 2:1 OLR region deviate far from their original
places, entering the bar region. A combination of resonance excitation of
stellar motions at the 2:1 OLR region together with strong interaction of the
stars with the bar potential leads to the formation of the group of 'escapees',
i.e., stars that deviate in $R$ and $Z$ -- directions at large distances from
the resonance region. Simulations, however, do not demonstrate any noticeable
effect on $V_Z$-distribution of stars in the solar neighborhood
