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Photoevaporation of planet forming discs by high energy radiation from thecentral star is potentially a crucial mechanism for disc evolution and it mayplay an important role in the formation and evolution of planetary system. Wepresent here a new generation of X-ray photoevaporation models for solar-typestars, based on a new set of hydrodynamical simulations, which account forstellar irradiation via a new, significantly improved, parameterisation of gastemperatures, based on detailed photoionisation and radiation transfercalculations. This is the first of a series of papers aiming at providing alibrary of models which cover the observed parameter space in stellar and discmass, metallicity and stellar X-ray properties. We focus here on solar-typestars (0.7 M$_\odot$) with relatively low-mass discs (1% of the stellar mass)and explore the dependence of the wind mass loss rates on stellar X-rayluminosity. We model primordial discs as well as transition discs at variousstages of evolution. Our 2D hydrodynamical models are then used to derivesimple recipes for the mass loss rates that are suitable for inclusion inone-dimensional disc evolution and/or planet formation models typicallyemployed for population synthesis studies. Line profiles from typical winddiagnostics ([OI] 6300 $\overset{\lower.5em\circ}{\mathrm{A}}$ and [NeII] 12.8$\mu$m) are also calculated for our models and found to be roughly in agreementwith previous studies. Finally, we perform a population study of transitiondiscs by means of one-dimensional viscous evolution models including our newphotoevaporation prescription and find that roughly a half of observedtransition discs cavities and accretion rates could be reproduced by ourmodels.

The dispersal of protoplanetary discs I: A new generation of X-ray photoevaporation models