  Magnetized winds may be important in dispersing protoplanetary disks and
influencing planet formation. We carry out global full magnetohydrodynamic
simulations in axisymmetry, coupled with ray-tracing radiative transfer,
consistent thermochemistry, and non-ideal MHD diffusivities. Magnetized models
lacking EUV photons ($h\nu>13.6\ \mathrm{eV}$) feature warm molecular outflows
that have typical poloidal speeds $\gtrsim 4\ \mathrm{km\ s}^{-1}$. When the
magnetization is sufficient to drive accretion rates $\sim 10^{-8}\ M_\odot\
\mathrm{yr}^{-1}$, the wind mass-loss rate is comparable. Such outflows are
driven not centrifugally but by the pressure of toroidal magnetic fields
produced by bending the poloidal field. Both the accretion and outflow rates
increase 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-ray
radiation near the wind base. Adding EUV irradiation to the system heats,
ionizes, and accelerates the part of the outflow nearest the symmetry axis, but
reduces the overall mass-loss rate by exerting pressure on the wind base. Most
of our models are non-turbulent, but some with reduced dust abundance and
therefore higher ionization fractions exhibit magnetorotational instabilities
near the base of the wind.
