  Recent multi-wavelength observations suggest that inner parts of
protoplanetary disks (PPDs) have shorter lifetimes for heavier host stars.
Since PPDs around high-mass stars are irradiated by strong ultra-violet
radiation, photoevaporation may provide an explanation for the observed trend.
We perform radiation hydrodynamics simulations of photoevaporation of PPDs for
a wide range of host star mass of $M_* =0.5$-$7.0 M_{\odot}$. We derive disk
mass-loss rate $\dot{M}$, which has strong stellar dependence as $\dot{M}
\approx 7.30\times10^{-9}(M_{*}/M_{\odot})^{2}M_{\odot}\rm{yr}^{-1}$. The
absolute value of $\dot{M}$ scales with the adopted far-ultraviolet and X-ray
luminosities. We derive the surface mass-loss rates and provide polynomial
function fits to them. We also develop a semi-analytic model that well
reproduces the derived mass-loss rates. The estimated inner disk lifetime
decreases as the host star mass increases, in agreement with the observational
trend. We thus argue that photoevaporation is a major physical mechanism for
PPD dispersal for a wide range of the stellar mass and can account for the
observed stellar mass dependence of the inner disk lifetime.
