Lowest accreting protoplanetary discs consistent with X-ray photoevaporation driving their final dispersal

TL;DR

This study compares different photoevaporation models for protoplanetary disc dispersal and finds that X-ray driven photoevaporation best explains the observed low accretion rate discs.

Contribution

The paper demonstrates that X-ray photoevaporation models align with recent observations of low accreting discs, favoring this mechanism over EUV and FUV models.

Findings

X-ray photoevaporation explains low accretion rates in protoplanetary discs.

Other models like EUV and FUV are inconsistent with observed data.

Distribution of accretion rates supports X-ray driven dispersal.

Abstract

Photoevaporation from high energy stellar radiation has been thought to drive the dispersal of protoplanetary discs. Different theoretical models have been proposed, but their predictions diverge in terms of the rate and modality at which discs lose their mass, with significant implications for the formation and evolution of planets. In this paper we use disc population synthesis models to interpret recent observations of the lowest accreting protoplanetary discs, comparing predictions from EUV-driven, FUV-driven and X-ray driven photoevaporation models. We show that the recent observational data of stars with low accretion rates (low accretors) point to X-ray photoevaporation as the preferred mechanism driving the final stages of protoplanetary disc dispersal. We also show that the distribution of accretion rates predicted by the X-ray photoevaporation model is consistent with observations, while other dispersal models tested here are clearly ruled out.