Blueshifted [OI] lines from protoplanetary discs: the smoking gun of X-ray photoevaporation

TL;DR

This paper investigates blueshifted [OI] emission lines in protoplanetary discs, providing observational evidence that supports X-ray photoevaporation as a key dispersal mechanism, while highlighting the line's temperature sensitivity.

Contribution

It offers the first direct observational validation linking blueshifted [OI] lines to X-ray driven disc winds, confirming theoretical predictions.

Findings

Blueshifted [OI] lines originate from warm, quasi-neutral disc winds.

The [OI] 6300A line is a thermal emission, not suitable for measuring wind mass-loss rates.

Models match observed line profiles, supporting X-ray photoevaporation as a dispersal process.

Abstract

Photoevaporation of protoplanetary discs by high energy radiation from the central young stellar object is currently the favourite model to explain the sudden dispersal of discs from the inside out. While several theoretical works have provided a detailed pictured of this process, the direct observational validation is still lacking. Emission lines produced in these slow moving protoplanetary disc winds may bear the imprint of the wind structure and thus provide a potential diagnostic of the underlying dispersal process. In this paper we primarily focus on the collisionally excited neutral oxygen line at 6300A. We compare our models predictions to observational data and demonstrate a thermal origin for the observed blueshifted low-velocity component of this line from protoplanetary discs. Furthermore our models show that while this line is a clear tell-tale-sign of a warm, quasi-neutral disc wind, typical of X-ray photoevaporation, its strong temperature dependence makes it unsuitable to measure detailed wind quantities like mass-loss-rate.