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We investigate the relation between disk mass and mass accretion rate toconstrain the mechanism of angular momentum transport in protoplanetary disks.Dust mass and mass accretion rate in Chamaeleon I are correlated with a slopeclose to linear, similar to the one recently identified in Lupus. Weinvestigate the effect of stellar mass and find that the intrinsic scatteraround the best-fit Mdust-Mstar and Macc-Mstar relations is uncorrelated. Diskswith a constant alpha viscosity can fit the observed relations between dustmass, mass accretion rate, and stellar mass, but over-predict the strength ofthe correlation between disk mass and mass accretion rate when using standardinitial conditions. We find two possible solutions. 1) The observed scatter inMdust and Macc is not primoridal, but arises from additional physical processesor uncertainties in estimating the disk gas mass. Most likely grain growth andradial drift affect the observable dust mass, while variability on large timescales affects the mass accretion rates. 2) The observed scatter is primordial,but disks have not evolved substantially at the age of Lupus and Chamaeleon Idue to a low viscosity or a large initial disk radius. More accurate estimatesof the disk mass and gas disk sizes in a large sample of protoplanetary disks,either through direct observations of the gas or spatially resolvedmulti-wavelength observations of the dust with ALMA, are needed to discriminatebetween both scenarios or to constrain alternative angular momentum transportmechanisms such as MHD disk winds.

Constraints from Dust Mass and Mass Accretion Rate Measurements on Angular Momentum Transport in Protoplanetary Disks