  We present the Galactic disk vertical velocity analysis using OB type stars
(OB), Red Clump stars (RC), and Main-Sequence-Turn-Off stars (MSTO) with
different average age populations crossed matched with LAMOST DR5 and Gaia DR3.
We reveal the vertical velocities of the three populations varies clearly with
the Galactocentric distance ($R$) and the younger stellar population has
stronger increasing trend in general. The bending and breathing modes indicated
by the vertical motions are dependent on the populations and they are varying
with spatial locations. These vertical motions may be due to the Galactic warp,
or minor mergers, or non-equilibrium of the disk. Assuming the warp is the
dominant component, we find that the warp amplitude ($\gamma$, $Z_\omega$) for
OB (younger population) is larger than that for RC (medium population) and the
later one is also larger than that for MSTO (older population), which is in
agreement with other independent analyses of stellar density distribution, and
supports the warp is long-lived, non-steady structure and has time evolution.
This conclusion is robust whether or not the line-of-nodes $\phi_w$ is fixed or
as a free parameter (with $\phi_w$ is around 3$-$8.5$^{\circ}$ as best fit).
Furthermore, we find that warp is lopsided with asymmetries along azimuthal
angle ($\phi$).
