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In recent years hydrodynamical (HD) models have become important to describethe gas kinematics in protoplanetary disks, especially in combination withmodels of photoevaporation and/or magnetic-driven winds. We focus on diagnosingthe the vertical extent of the VSI at 203 cells per scale height and allude atwhat resolution per scale height we obtain convergence. Finally, we determinethe regions where EUV, FUV and X-Rays are dominant in the disk. We performglobal HD simulations using the PLUTO code. We adopt a global isothermalaccretion disk setup, 2.5D (2 dimensions, 3 components) which covers a radialdomain from 0.5 to 5.0 and an approximately full meridional extension. Wedetermine the 50 cells per scale height to be the lower limit to resolve theVSI. For higher resolutions, greater than 50 cells per scale height, we observethe convergence for the saturation level of the kinetic energy. We are alsoable to identify the growth of the `body' modes, with higher growth rate forhigher resolution. Full energy saturation and a turbulent steady state isreached after 70 local orbits. We determine the location of the EUV-heatedregion defined by the radial column density to be 10$^{19}$ cm$^{-2}$ locatedat $H_\mathrm{R}\sim9.7$, and the FUV/X-Rays-heated boundary layer defined by10$^{22}$ cm$^{-2}$ located at $H_\mathrm{R}\sim6.2$, making it necessary tointroduce the need of a hot atmosphere. For the first time, we report thepresence of small scale vortices in the r-Z plane, between the characteristiclayers of large scale vertical velocity motions. Such vortices could lead todust concentration, promoting grain growth. Our results highlight theimportance to combine photoevaporation processes in the future high-resolutionstudies of the turbulence and accretion processes in disks.

Hydrodynamical simulations of protoplanetary disks including irradiation of stellar photons. I. Resolution study for Vertical Shear Instability (VSI)