  Based on Cepheids located near the solar circle, we have determined the
Galactocentric distance of the Sun $R_0$ and the Galactic rotation velocity at
the solar distance $V_0$. For our analysis we used a sample of $\sim$200
classical Cepheids from the catalogue by Skowron et al. (2019), where the
distances to them were determined from the period-luminosity relation. For
these stars the proper motions and line-of-sight velocities were taken from the
Gaia DR3 catalogue. The values of $R_0$ found lie within the range [7.8-8.3]
kpc, depending on the heliocentric distance of the sample stars, on the adopted
solar velocity relative to the local standard of rest, and on whether or not
the perturbations caused by the Galactic spiral density wave are taken into
account. The dispersion of the $R_0$ estimates is $\sim$2 kpc. Similarly, the
values of $V_0$ lie within the range [240-270] km s$^{-1}$ with a dispersion of
the estimates of 70-90 km s$^{-1}$. We consider the following estimates to be
the final ones: $R_0=8.24\pm0.20$ kpc and $V_0=268\pm8$ km s$^{-1}$ found by
taking into account the perturbations from the Galactic spiral density wave.
