  Photoevaporation and magnetically driven winds are two independent mechanisms
to remove mass from protoplanetary disks. In addition to accretion, the effect
of these two principles acting concurrently could be significant and the
transition between those two has not been extensively studied and quantified in
the literature yet. In order to contribute to the understanding of disk winds,
we present the phenomena emerging in the framework of two-dimensional
axisymmetric, non-ideal magnetohydrodynamic simulations including EUV-/ X-ray
driven photoevaporation. Of particular interest are the examination of the
transition region between photoevaporation and magnetically driven wind, the
possibility of emerging magneto-centrifugal wind effects, as well as the
morphology of the wind itself depending on the strength of the magnetic field.
We use the PLUTO code in a 2.5D axisymmetric configuration with additional
treatment of EUV-/ X-ray heating and dynamic ohmic diffusion based on a
semi-analytical chemical model. We identify the transition between both outflow
types to occur for values of the initial plasma beta $\beta \geq 10^7$, while
magnetically driven winds generally outperform photoevaporation for stronger
fields. In our simulations we observe irregular and asymmetric outflows for
stronger magnetic fields. In the weak field regime the photoevaporation rates
are slightly lowered by perturbations of the gas density in the inner regions
of the disk. Overall, our results predict a wind with a lever arm smaller than
1.5, consistent with a hot magneto-thermal wind. Stronger accretion flows are
present for values of $\beta < 10^7$.
