  The final stages of a protoplanetary disk are essential for our understanding
of the formation and evolution of planets. Photoevaporation is an important
mechanism that contributes to the dispersal of an accretion disk and has
significant consequences for the disk's lifetime. However, the combined effects
of photoevaporation and star-disk interaction have not been investigated in
previous studies. We combined an implicit disk evolution model with a
photoevaporative mass-loss profile. By including the innermost disk regions
down to 0.01 AU, we could calculate the star-disk interaction, the stellar spin
evolution, and the transition from an accreting disk to the propeller regime
self-consistently. Starting from an early Class II star-disk system, we
calculated the long-term evolution of the system until the disk becomes almost
completely dissolved. Photoevaporation has a significant effect on disk
structure and evolution. The radial extent of the dead zone decreases, and the
number of episodic accretion events (outbursts) is reduced by high stellar
X-ray luminosities. Reasonable accretion rates in combination with
photoevaporative gaps are possible for a dead zone that is still massive enough
to develop episodic accretion events. Furthermore, the stellar spin evolution
during the Class II evolution is less affected by the star-disk interaction in
the case of high X-ray luminosities. Our results suggest that the formation of
planets, especially habitable planets, in the dead zone is strongly impaired in
the case of strong X-ray luminosities. Additionally, the importance of the
star-disk interaction during the Class II phase with respect to the stellar
spin evolution is reduced.
