  We have studied the kinematics of a unique sample of young open star clusters
(OSCs) with high vertical velocities, $15<W<40$ km s$^{-1}$. The
characteristics of these clusters were taken from the catalogue by Hunt and
Reffert (2023), where their mean proper motions, line-of-sight velocities, and
distances were calculated using Gaia DR3 data. These OSCs are located within
0.6 kpc of the Sun and form two clumps: one in the region of the Sco-Cen OB
association and the other one in the region of the Per OB3-Per OB2
associations. The OSC group of 47 members in the region of the Sco-Cen
association is shown to expand along the $y$ axis, $\partial V/\partial
y=51\pm12$ km s$^{-1}$ kpc$^{-1}$. This group also has a positive rotation
around the $z$ axis with an angular velocity of $71\pm11$ km s$^{-1}$
kpc$^{-1}$ and a negative rotation around the $x$ axis with an angular velocity
of $-35\pm5$ km s$^{-1}$ kpc$^{-1}$. Based on the velocities of 27 OSCs from
the region of the Per OB3-Per OB2 associations, we have found no gradients
differing significantly from zero. We have studied the kinematics of more than
1700 stars selected by Luhman (2022) as probable members of the Sco-Cen OB
association. These stars are shown to have no high vertical velocities. The
expansion coefficient of the stellar system in the $xy$ plane has been found
from all stars to be $K_{xy}=43.2\pm2.2$ km s$^{-1}$ kpc$^{-1}$. Based on stars
from the three UCL, LCC, and V1062 Sco groups with a mean age $\sim$20 Myr, for
the first time we have found a volume expansion coefficient of the stellar
system differing significantly from zero, $K_{xyz}=43.2\pm3.4$ km s$^{-1}$
kpc$^{-1}$.
