Radiation hydrodynamics simulations of protoplanetary disks: Stellar mass dependence of the disk photoevaporation rate

Abstract

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 $M_{\ast }=0.5$-$7.0M_{\odot }$. We derive disk mass-loss rate $\dot{M}$, which has strong stellar dependence as $\dot{M}\approx 7.30\times 10^{-9}(M_{\ast }/M_{\odot }{)}^2{M}_{\odot }{\mathrm{yr}}^{-1}$. 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.

15 pages, 12figures, ApJ in press

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Cited by in corpus (4)

• Large gaps and high accretion rates in photoevaporative transition disks with a dead zone
• Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level
• The importance of X-ray frequency in driving photoevaporative winds
• The dispersal of protoplanetary discs -- III: Influence of stellar mass on disc photoevaporation