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Magnetized winds may be important in dispersing protoplanetary disks andinfluencing planet formation. We carry out global full magnetohydrodynamicsimulations in axisymmetry, coupled with ray-tracing radiative transfer,consistent thermochemistry, and non-ideal MHD diffusivities. Magnetized modelslacking EUV photons ($h\nu>13.6\ \mathrm{eV}$) feature warm molecular outflowsthat have typical poloidal speeds $\gtrsim 4\ \mathrm{km\ s}^{-1}$. When themagnetization is sufficient to drive accretion rates $\sim 10^{-8}\ M_\odot\\mathrm{yr}^{-1}$, the wind mass-loss rate is comparable. Such outflows aredriven not centrifugally but by the pressure of toroidal magnetic fieldsproduced by bending the poloidal field. Both the accretion and outflow ratesincrease with the poloidal field energy density, the former almost linearly.The mass-loss rate is also strongly affected by ionization due to UV and X-rayradiation near the wind base. Adding EUV irradiation to the system heats,ionizes, and accelerates the part of the outflow nearest the symmetry axis, butreduces the overall mass-loss rate by exerting pressure on the wind base. Mostof our models are non-turbulent, but some with reduced dust abundance andtherefore higher ionization fractions exhibit magnetorotational instabilitiesnear the base of the wind.

Global Simulations of Protoplanetary Disk Outflows with Coupled Non-ideal Magnetohydrodynamics and Consistent Thermochemistry