  We aim to understand the effect of stellar evolution on the evolution of
protoplanetary disks. We focus in particular on the disk evolution around
intermediate-mass (IM) stars, which evolve more rapidly than low-mass ones. We
numerically solve the long-term evolution of disks around 0.5-5 solar-mass
stars considering viscous accretion and photoevaporation (PE) driven by stellar
far-ultraviolet (FUV), extreme-ultraviolet (EUV), and X-ray emission. We also
take stellar evolution into account and consider the time evolution of the PE
rate. We find that the FUV, EUV, and X-ray luminosities of IM stars evolve by
orders of magnitude within a few Myr along with the time evolution of stellar
structure, stellar effective temperature, or accretion rate. Therefore, the PE
rate also evolves with time by orders of magnitude, and we conclude that
stellar evolution is crucial for the disk evolution around IM stars.
