Photoevaporation of Grain-Depleted Protoplanetary Disks around Intermediate-Mass Stars: Investigating Possibility of Gas-Rich Debris Disks as Protoplanetary Remnants

Abstract

Debris disks are classically considered to be gas-less systems, but recent (sub)millimeter observations have detected tens of those with rich gas content. The origin of the gas component remains unclear; namely, it can be protoplanetary remnants and/or secondary products deriving from large bodies. In order to be protoplanetary in origin, the gas component of the parental protoplanetary disk is required to survive for $\gtrsim 10\mathrm{Myr}$. However, previous models predict $\lesssim 10\mathrm{Myr}$ lifetimes because of efficient photoevaporation at the late stage of disk evolution. In the present study, we investigate photoevaporation of gas-rich, optically-thin disks around intermediate-mass stars at a late stage of the disk evolution. The evolved system is modeled as those where radiation force is sufficiently strong to continuously blow out small grains ($\lesssim 4\mu \mathrm{m}$), which are an essential component for driving photoevaporation via photoelectric heating induced by stellar far-ultraviolet (FUV). We find that the grain depletion reduces photoelectric heating, so that FUV photoevaporation is not excited. Extreme-ultraviolet (EUV) photoevaporation is dominant and yields a mass-loss rate of $2$--$5\times 10^{-10}({\Phi }_{\mathrm{EUV}}/10^{41}{\mathrm{s}}^{-1}{)}^{1/2}{M}_{\odot }{\mathrm{yr}}^{-1}$, where ${\Phi }_{\mathrm{EUV}}$ is the EUV emission rate. The estimated lifetimes of the gas component are $\sim 50(M_{\mathrm{disk}}/10^{-2}{M}_{\odot })({\Phi }_{\mathrm{EUV}}/10^{41}{\mathrm{s}}^{-1}{)}^{1/2}\mathrm{Myr}$ and depend on the ``initial'' disk mass at the point small grains have been depleted in the system. With an order estimation, we show that the gas component can survive for a much longer time around A-type stars than lower-mass stars. This trend is consistent with the higher frequency of gas-rich debris disks around A-type stars, implying the possibility of the gas component being protoplanetary remnants.

arXiv commentAccepted for publication in ApJ

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