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Recent infrared and submillimeter observations suggest that theprotoplanetary disk lifetime depends on the central stellar mass. The diskdispersal is thought to be driven by viscous accretion, magneto-hydrodynamics(MHD) winds, and photoevaporation by the central star. We perform a set ofone-dimensional simulations of long-term disk evolution that include all thethree processes. We vary the stellar mass in the range of 0.5-7M$_{\odot}$, andstudy the mass dependence of the disk evolution. We show that a significantfraction of the disk gas is lost by MHD winds in the early stage, but the laterdisk evolution is mainly governed by photoevaporation. The disk radiusdecreases as photoevaporation clears out the gas in the outer disk efficiently.The qualitative evolutionary trends of the disk mass are remarkably similar forthe wide range of the central stellar mass we consider, and the time evolutionof the disk mass can be well fitted by a simple function. The dispersal time isapproximately ten million years for low mass stars with weak mass dependence,but gets as short as two million years around a 7M$_{\odot}$ star. In thelatter case, a prominent inner hole is formed by the combined effect ofaccretion and MHD winds within about one million years. The strength of the MHDwind and viscous accretion controls the overall mass-loss rate, but does notalter the dependence of the dispersal timescale on the central stellar mass.

Simulations of Protoplanetary Disk Dispersal: Stellar Mass Dependence of the Disk Lifetime