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We analyse current measurements of accretion rates onto pre-main sequencestars as a function of stellar mass, and conclude that the steep dependance ofaccretion rates on stellar mass is real and not driven by selection/detectionthreshold, as has been previously feared. These conclusions are reached bymeans of statistical tests including a survival analysis which can account forupper limits. The power-law slope of the Mdot-M* relation is found to be in therange of 1.6-1.9 for young stars with masses lower than 1 Msun. The measuredslopes and distributions can be easily reproduced by means of a simple discmodel which includes viscous accretion and X-ray photoevaporation. We concludethat the Mdot-M* relation in pre-main sequence stars bears the signature ofdisc dispersal by X-ray photoevaporation, suggesting that the relation is astraight- forward consequence of disc physics rather than an imprint of initialconditions.

The Mdot - M* relation of pre-main sequence stars: a consequence of X-ray driven disc evolution