# Rapid destruction of protoplanetary discs due to externalphotoevaporation in star-forming regions

## TL;DR

This study uses N-body simulations to show that external photoevaporation by massive stars rapidly disperses protoplanetary discs, especially in dense, substructured, and collapsing star-forming regions, affecting planet formation timelines.

## Contribution

It provides new insights into how initial conditions of star-forming regions influence disc dispersal rates due to external photoevaporation, highlighting faster dispersal than previously observed.

## Key findings

- Discs in dense, substructured regions are dispersed within 1 Myr.
- Half of large discs are photoevaporated within 1 Myr in certain regions.
- Lower-density regions allow longer disc survival, but still experience rapid dispersal.

## Abstract

We analyse N-body simulations of star-forming regions to investigate the effects of external far and extreme ultra-violet photoevaporation from massive stars on protoplanetary discs. By varying the initial conditions of simulated star-forming regions, such as the spatial distribution, net bulk motion (virial ratio), and density, we investigate which parameters most affect the rate at which discs are dispersed due to external photoevaporation. We find that disc dispersal due to external photoevaporation is faster in highly substructured star-forming regions than in smooth and centrally concentrated regions. Sub-virial star-forming regions undergoing collapse also show higher rates of disc dispersal than regions that are in virial equilibrium or are expanding. In moderately dense ($\sim$100 M$_{\odot}$ pc$^{-3}$) regions, half of all protoplanetary discs with radii $\geq$ 100 AU are photoevaporated within 1 Myr, three times faster than is currently suggested by observational studies. Discs in lower-density star-forming regions ($\sim$10 M$_{\odot}$ pc$^{-3}$) survive for longer, but half are still dispersed on short timescales ($\sim$2 Myr). This demonstrates that the initial conditions of the star forming regions will greatly impact the evolution and lifetime of protoplanetary discs. These results also imply that either gas giant planet formation is extremely rapid and occurs before the gas component of discs is evaporated, or gas giants only form in low-density star-forming regions where no massive stars are present to photoevaporate gas from protoplanetary discs.