# Radiation pressure clear-out of dusty photoevaporating discs

## TL;DR

This paper demonstrates that radiation pressure can rapidly clear dust from pressure traps in photoevaporating protoplanetary discs within about 100,000 years, transforming them into dust-depleted, gas-rich structures resembling debris discs.

## Contribution

It introduces a new mechanism where radiation pressure effectively removes dust from pressure traps, challenging previous models that predicted longer-lived dust-rich phases.

## Key findings

- Radiation pressure can deplete dust in pressure traps within ~10^5 years.
- Discs become dust-depleted and optically thin, resembling debris discs.
- Many young stars with debris discs may have undergone this dust-clearing process.

## Abstract

Theoretical models of protoplanetary disc dispersal predict a phase where photoevaporation has truncated the disc at several AU, creating a pressure trap which is dust-rich. Previous models predicted this phase could be long-lived (~Myr), contrary to the observational constraints. We show that dust in the pressure trap can be removed from the disc by radiation pressure exerting a significant acceleration, and hence radial velocity, on small dust particles that reside in the surface layers of the disc. The dust in the pressure trap is not subject to radial drift so it can grow to reach sizes large enough to fragment. Hence small particles removed from the surface layers are replaced by the fragments of larger particles. This link means radiation pressure can deplete the dust at all particle sizes. Through a combination of 1D and 2D models, along with secular models that follow the disc's long-term evolution, we show that radiation pressure can deplete dust from pressure traps created by photoevaporation in ~1e5 years, while the photoevaporation created cavity still resides at 10s of AU. After this phase of radiation pressure removal of dust, the disc is gas-rich and dust depleted and radially optically thin to stellar light, having observational signatures similar to a gas-rich, young debris disc. Indeed many of the young stars (~<10 Myr old) classified as hosting a debris disc may rather be discs that have undergone this process.