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Photoevaporation of protoplanetary discs by high energy radiation from thecentral young stellar object is currently the favourite model to explain thesudden dispersal of discs from the inside out. While several theoretical workshave provided a detailed pictured of this process, the direct observationalvalidation is still lacking. Emission lines produced in these slow movingprotoplanetary disc winds may bear the imprint of the wind structure and thusprovide a potential diagnostic of the underlying dispersal process. In thispaper we primarily focus on the collisionally excited neutral oxygen line at6300A. We compare our models predictions to observational data and demonstratea thermal origin for the observed blueshifted low-velocity component of thisline from protoplanetary discs. Furthermore our models show that while thisline is a clear tell-tale-sign of a warm, quasi-neutral disc wind, typical ofX-ray photoevaporation, its strong temperature dependence makes it unsuitableto measure detailed wind quantities like mass-loss-rate.

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