The effect of ultra-violet photon pumping of H$_2$ in dust-deficient protoplanetary disks

TL;DR

This study uses radiation hydrodynamics simulations to explore how ultra-violet H$_2$ pumping influences the structure and mass-loss of dust-deficient protoplanetary disks, revealing its significant role in late-stage disk evolution.

Contribution

It demonstrates that H$_2$ pumping significantly enhances photoevaporation in dust-deficient disks, affecting their long-term evolution, a novel insight into disk dispersal mechanisms.

Findings

H$_2$ pumping increases mass-loss in dust-deficient disks.

Mass-loss rates remain around 10^{-10}-10^{-11} M_sun/yr despite dust reduction.

H$_2$ pumping shapes the disk mass-loss profile, especially in inner regions.

Abstract

We perform radiation hydrodynamics simulations to study the structure and evolution of a photoevaporating protoplanetary disk. Ultraviolet and X-ray radiation from the host star heats the disk surface, where H$_2$ pumping also operates efficiently. We run a set of simulations with varying the amount of dust grains, or the dust-to-gas mass ratio, which determines the relative importance between photoelectric heating and H$_2$ pumping. We show that H$_2$ pumping and X-ray heating contribute stronger to the mass-loss of the disk if the dust-to-gas mass ratio is $\mathcal{D}\leq10^{-3}$.The disk mass loss rate decreases with a lower dust amount, but remains around $10^{-10-11} M_{\odot} {\rm yr}^{-1}$. In such dust-deficient disks, H$_2$ pumping enhances photoevaporation from the inner disk region and shapes the disk mass-loss profile. We thus argue that the late-stage disk evolution is affected by the ultra-violet H$_2$ pumping effect. The mass-loss rates derived from our simulations can be used in the study of long-term disk evolution.