Global evolution and dispersal of protoplanetary disks ( PPDs ) is governed by disk angular momentum transport and mass-loss processes .
Recent numerical studies suggest that angular momentum transport in the inner region of PPDs is largely driven by magnetized disk wind , yet the wind mass-loss rate remains unconstrained .
On the other hand , disk mass loss has conventionally been attributed to photoevaporation , where external heating on the disk surface drives a thermal wind .
We unify the two scenarios by developing a 1D model of magnetized disk winds with a simple treatment of thermodynamics as a proxy for external heating .
The wind properties largely depend on 1 ) the magnetic field strength at the wind base , characterized by the poloidal Alfvén speed v _ { Ap } , 2 ) the sound speed c _ { s } near the wind base , and 3 ) how rapidly poloidal field lines diverge ( achieve R ^ { -2 } scaling ) .
When v _ { Ap } \gg c _ { s } , corotation is enforced near the wind base , resulting in centrifugal acceleration .
Otherwise , the wind is accelerated mainly by the pressure of the toroidal magnetic field .
In both cases , the dominant role played by magnetic forces likely yields wind outflow rates that well exceed purely hydrodynamical mechanisms .
For typical PPD accretion-rate and wind-launching conditions , we expect v _ { Ap } to be comparable to c _ { s } at the wind base .
The resulting wind is heavily loaded , with total wind mass loss rate likely reaching a considerable fraction of wind-driven accretion rate .
Implications for modeling global disk evolution and planet formation are also discussed .