The dispersal of planet-forming discs. A new generation of X-ray photoevaporation models.

The modality of disc dispersal is thought to be of fundamental importance to planet formation, yet the responsible mechanism is still largely unconstrained. Photoevaporation from the central star is currently a promising avenue to investigate, but the models developed to date do not yet have enough predictive power for a piecewise comparison with the observations. We focus on creating new and improved hydrodynamical models of wind profiles from stellar irradiation at different wavelengths (EUV, X-rays) in order to have better constraints for current and future observations. We provide several fits of the total mass-loss rate as a function of star's X-ray luminosity, stellar mass, and carbon depletion, which can be used as simple prescriptions in population synthesis models of planet formation, as well as to produce line profiles within the wind for different disc inclinations. We find that the total mass-loss rate is increased by a factor 2 with respect to the previous models and the X-ray photoevaporation can explain a larger fraction of observed transition discs. Although these differences are small, they can significantly impact planet formation and their architecture