  In recent years hydrodynamical (HD) models have become important to describe
the gas kinematics in protoplanetary disks, especially in combination with
models of photoevaporation and/or magnetic-driven winds. We focus on diagnosing
the the vertical extent of the VSI at 203 cells per scale height and allude at
what resolution per scale height we obtain convergence. Finally, we determine
the regions where EUV, FUV and X-Rays are dominant in the disk. We perform
global HD simulations using the PLUTO code. We adopt a global isothermal
accretion disk setup, 2.5D (2 dimensions, 3 components) which covers a radial
domain from 0.5 to 5.0 and an approximately full meridional extension. We
determine the 50 cells per scale height to be the lower limit to resolve the
VSI. For higher resolutions, greater than 50 cells per scale height, we observe
the convergence for the saturation level of the kinetic energy. We are also
able to identify the growth of the `body' modes, with higher growth rate for
higher resolution. Full energy saturation and a turbulent steady state is
reached after 70 local orbits. We determine the location of the EUV-heated
region defined by the radial column density to be 10$^{19}$ cm$^{-2}$ located
at $H_\mathrm{R}\sim9.7$, and the FUV/X-Rays-heated boundary layer defined by
10$^{22}$ cm$^{-2}$ located at $H_\mathrm{R}\sim6.2$, making it necessary to
introduce the need of a hot atmosphere. For the first time, we report the
presence of small scale vortices in the r-Z plane, between the characteristic
layers of large scale vertical velocity motions. Such vortices could lead to
dust concentration, promoting grain growth. Our results highlight the
importance to combine photoevaporation processes in the future high-resolution
studies of the turbulence and accretion processes in disks.
