2025ApJ...992...85M

We perform 2D global magnetohydrodynamic (MHD) simulations including the full nonideal MHD effects (ohmic diffusion, Hall effect, and ambipolar diffusion) and approximate radiation transport to understand the dynamics and thermal structure of the inner protoplanetary disks (PPDs). We have developed a simple radiative transfer model for PPDs that reasonably treats stellar nonthermal (X-ray and ultraviolet (XUV)), stellar thermal (optical/infrared), and reemitted radiation, reproducing the temperature structures from Monte Carlo radiative transfer. Our simulations show fast one-sided surface accretion (∼10% of Keplerian velocity) and asymmetric disk winds when the vertical magnetic field is aligned with the disk angular momentum. The asymmetry is due to the failure of the wind on the side with the accretion layer. On the accreting surface, clumps are repeatedly generated and accrete, driven by radiative feedback. For the antialigned fields, surface accretion becomes more moderate and time variable, while the winds remain largely symmetric. For the thermal structure, accretion heating does not affect the disk temperature in any of our runs. This is because (1) the accretion energy dissipates via Joule heating at two to three gas scale heights, where low optical depth enables efficient radiative cooling, and (2) the winds remove ≳10% of the accretion energy. In contrast, the winds enhance radiative heating by elevating the irradiation front. These results highlight the importance of coupling between gas dynamics and radiation transport in PPDs and provide observable magnetic activities such as fast episodic accretion, wind asymmetry, and molecular survival in XUV-irradiated winds.