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Young solar-type stars are known to be strong X-ray emitters and their X-rayspectra have been widely studied. X-rays from the central star may play acrucial role in the thermodynamics and chemistry of the circumstellar materialas well as in the atmospheric evolution of young planets. In this paper wepresent model spectra based on spectral parameters derived from theobservations of young stars in the Orion Nebula Cluster from the Chandra OrionUltradeep Project (COUP). The spectra are then used to calculate newphotoevaporation prescriptions that can be used in disc and planet populationsynthesis models. Our models clearly show that disc wind mass loss rates arecontrolled by the stellar luminosity in the soft (100 eV - 1 keV) X- ray band.New analytical relations are provided for the mass loss rates and profiles ofphotoevaporative winds as a function of the luminosity in the soft X-ray band.The agreement between observed and predicted transition disc statisticsmoderately improved using the new spectra, but the observed population ofstrongly accreting large cavity discs can still not be reproduced by thesemodels. Furthermore, our models predict a population of non-accretingtransition discs that are not observed. This highlights the importance ofconsidering the depletion of millimeter-sized dust grains from the outer disc,which is a likely reason why such discs have not been detected yet.

The dispersal of protoplanetary discs. II: Photoevaporation models with observationally derived irradiating spectra