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We model the mass accretion rate $\dot{M}$ to stellar mass $M_*$ correlationthat has been inferred from observations of intermediate to upper mass T Tauristars---that is $\dot{M} \propto M_*^{1.3 \pm 0.3}$. We explain thiscorrelation within the framework of quiescent disk evolution, in whichaccretion is driven largely by gravitational torques acting in the bulk of themass and volume of the disk. Stresses within the disk arise from the action ofgravitationally driven torques parameterized in our 1D model in terms ofToomre's $Q$ criterion. We do not model the hot inner sub-AU scale region ofthe disk that is likely stable according to this criterion, and appeal to othermechanisms to remove or redistribute angular momentum and allow accretion ontothe star. Our model has the advantage of agreeing with large-scaleangle-averaged values from more complex nonaxisymmetric calculations. The modeldisk transitions from an early phase (dominated by initial conditions inheritedfrom the burst mode of accretion) into a later self-similar mode characterizedby a steeper temporal decline in $\dot{M}$. The models effectively reproducethe spread in mass accretion rates that have been observed for protostellarobjects of $0.2\,\mbox{M}_\odot \le M_* \le 3.0\,\mbox{M}_\odot$, such as thosefound in the $\rho$ Ophiuchus and Taurus star forming regions. We then comparerealistically sampled populations of young stellar objects produced by ourmodel to their observational counterparts. We find these populations to bestatistically coincident, which we argue is evidence for the role ofgravitational torques in the late time evolution of quiescent protostellardisks.

The Role of Angular Momentum Transport in Establishing the Accretion Rate--Protostellar Mass Correlation