  A simple one-dimensional axisymmetric disc model is applied to the kinematics
of OB stars near the Sun obtained from Gaia DR3 catalogue. The model determines
the 'local centrifugal speed' $V_\mathrm{c}(R_{0})$ - defined as the circular
velocity in the Galactocentric rest frame, where the star would move in a
near-circular orbit if the potential is axisymmetric with the local potential
of the Galaxy. We find that the $V_\mathrm{c}(R_{0})$ values and their gradient
vary across the selected region of stars within the solar neighbourhood. By
comparing with an N-body/hydrodynamic simulation of a Milky Way-like galaxy, we
find that the kinematics of the young stars in the solar neighbourhood is
affected by the Local arm, which makes it difficult to measure
$V_\mathrm{c}(R_{0})$. However, from the resemblance between the observational
data and the simulation, we suggest that the known rotational velocity gap
between the Coma Bernices and Hyades-Pleiades moving groups could be driven by
the co-rotation resonance of the Local arm, which can be used to infer the
azimuthally averaged circular velocity. We find that $V_\mathrm{c}(R)$ obtained
from the $\mathrm{D}<2$ kpc sample is well matched with this gap at the
position of the Local arm. Hence, we argue that our results from the
$\mathrm{D}<2$ kpc sample, $V_\mathrm{c}(R_{0})= 233.95\pm2.24$ km
$\mathrm{s}^{-1}$, is close to the azimuthally averaged circular velocity
rather than the local centrifugal speed, which is influenced by the presence of
the Local arm.
