Radiation hydrodynamics simulations of protoplanetary disks: Stellar mass dependence of the disk photoevaporation rate. (arXiv:2012.14852v3 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Komaki_A/0/1/0/all/0/1">Ayano Komaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakatani_R/0/1/0/all/0/1">Riouhei Nakatani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshida_N/0/1/0/all/0/1">Naoki Yoshida</a>
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 $dot{M}
approx 7.30times10^{-9}(M_{*}/M_{odot})^{2}M_{odot}rm{yr}^{-1}$. 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.
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 $dot{M}
approx 7.30times10^{-9}(M_{*}/M_{odot})^{2}M_{odot}rm{yr}^{-1}$. 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.
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