  Turbulence is crucial for protoplanetary disk dynamics, and Vertical Shear
Instability (VSI) is a promising mechanism in outer disk regions to generate
turbulence. We use Athena++ radiation module to study VSI in full and
transition disks, accounting for radiation transport and stellar irradiation.
We find that the thermal structure and cooling timescale significantly
influence VSI behavior. The inner rim location and radial optical depth affect
disk kinematics. Compared with previous vertically-isothermal simulations, our
full disk and transition disks with small cavities have a superheated
atmosphere and cool midplane with long cooling timescales, which suppresses the
corrugation mode and the associated meridional circulation. This temperature
structure also produces a strong vertical shear at $\mathrm{\tau_*}$ = 1,
producing an outgoing flow layer at $\tau_* < 1$ on top of an ingoing flow
layer at $\tau_* \sim 1$. The midplane becomes less turbulent, while the
surface becomes more turbulent with effective $\alpha$ reaching $\sim10^{-2}$
at $\tau_* \lesssim$1. This large surface stress drives significant surface
accretion, producing substructures. Using temperature and cooling time
measured/estimated from radiation-hydro simulations, we demonstrate that less
computationally-intensive simulations incorporating simple orbital cooling can
almost reproduce radiation-hydro results. By generating synthetic images, we
find that substructures are more pronounced in disks with larger cavities. The
higher velocity dispersion at the gap edge could also slow particle settling.
Both properties are consistent with recent Near-IR and ALMA observations. Our
simulations predict that regions with significant temperature changes are
accompanied by significant velocity changes, which can be tested by ALMA
kinematics/chemistry observations.
