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As the classic viscous paradigm for protoplanetary disk accretion ischallenged by the observational evidence of low turbulence, the alternativescenario of MHD disk winds is being explored as potentially able to reproducethe same observed features traditionally explained with viscosity. Although thetwo models lead to different disk properties, none of them has been ruled outby observations - mainly due to instrumental limitations. In this work, wepresent a viable method to distinguish between the viscous and MHD frameworkbased on the different evolution of the distribution in the disk mass($M_{\mathrm{d}}$) - accretion rate ($\dot M$) plane of a disk population. Witha synergy of analytical calculations and 1D numerical simulations, performedwith the population synthesis code \texttt{Diskpop}, we find that bothmechanisms predict the spread of the observed ratio $M_{\mathrm{d}}/\dot M$ ina disk population to decrease over time; however, this effect is much lesspronounced in MHD-dominated populations as compared to purely viscouspopulations. Furthermore, we demonstrate that this difference is detectablewith the current observational facilities: we show that convolving theintrinsic spread with the observational uncertainties does not affect ourresult, as the observed spread in the MHD case remains significantly largerthan in the viscous scenario. While the most recent data available show abetter agreement with the wind model, ongoing and future efforts to obtaindirect gas mass measurements with ALMA and ngVLA will cause a reassessment ofthis comparison in the near future.

The time evolution of $M_{\mathrm{d}}/\dot M$ in protoplanetary discs as a way to disentangle between viscosity and MHD winds