  Outflows driven by large-scale magnetic fields likely play an important role
in the evolution and dispersal of protoplanetary disks, and in setting the
conditions for planet formation. We extend our 2-D axisymmetric non-ideal MHD
model of these outflows by incorporating radiative transfer and simplified
thermochemistry, with the twin aims of exploring how heating influences wind
launching, and illustrating how such models can be tested through observations
of diagnostic spectral lines. Our model disks launch magnetocentrifugal
outflows primarily through magnetic tension forces, so the mass-loss rate
increases only moderately when thermochemical effects are switched on. For
typical field strengths, thermochemical and irradiation heating are more
important than magnetic dissipation. We furthermore find that the entrained
vertical magnetic flux diffuses out of the disk on secular timescales as a
result of non-ideal MHD. Through post-processing line radiative transfer, we
demonstrate that spectral line intensities and moment-1 maps of atomic oxygen,
the HCN molecule, and other species show potentially observable differences
between a model with a magnetically driven outflow and one with a weaker,
photoevaporative outflow. In particular, the line shapes and velocity
asymmetries in the moment-1 maps could enable the identification of outflows
emanating from the disk surface.
