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The strong X-ray irradiation from young solar-type stars may play a crucialrole in the thermodynamics and chemistry of circumstellar discs, driving theirevolution in the last stages of disc dispersal as well as shaping theatmospheres of newborn planets. In this paper we study the influence of stellarmass on circumstellar disc mass-loss rates due to X-ray irradiation, extendingour previous study of the mass-loss rate's dependence on the X-ray luminosityand spectrum hardness. We focus on stars with masses between 0.1 and 1 Solarmass, which are the main target of current and future missions to findpotentially habitable planets. We find a linear relationship between themass-loss rates and the stellar masses when changing the X-ray luminosityaccordingly with the stellar mass. This linear increase is observed also whenthe X-ray luminosity is kept fixed because of the lower disc aspect ratio whichallows the X-ray irradiation to reach larger radii. We provide new analyticalrelations for the mass-loss rates and profiles of photoevaporative winds as afunction of the stellar mass that can be used in disc and planet populationsynthesis models. Our photoevaporative models correctly predict the observedtrend of inner-disc lifetime as a function of stellar mass with an increasedsteepness for stars smaller than 0.3 Solar mass, indicating that X-rayphotoevaporation is a good candidate to explain the observed disc dispersalprocess.

The dispersal of protoplanetary discs -- III: Influence of stellar mass on disc photoevaporation