Protoplanetary disc `isochrones' and the evolution of discs in the $\dot{M}-M_{\mathrm{d}}$ plane

Abstract

In this paper, we compare simple viscous diffusion models for the disc evolution with the results of recent surveys of the properties of young protoplanetary discs. We introduce the useful concept of `disc isochrones' in the accretion rate - disc mass plane and explore a set of Montecarlo realization of disc initial conditions. We find that such simple viscous models can provide a remarkable agreement with the available data in the Lupus star forming region, with the key requirement that the average viscous evolutionary timescale of the discs is comparable to the cluster age. Our models produce naturally a correlation between mass accretion rate and disc mass that is shallower than linear, contrary to previous results and in agreement with observations. We also predict that a linear correlation, with a tighter scatter, should be found for more evolved disc populations. Finally, we find that such viscous models can reproduce the observations in the Lupus region only in the assumption that the efficiency of angular momentum transport is a growing function of radius, thus putting interesting constraints on the nature of the microscopic processes that lead to disc accretion.

8 pages, 6 Figures, MNRAS, accepted

References in corpus (11)

• Accretion disc viscosity: how big is alpha?
• X-Shooter spectroscopy of young stellar objects in Lupus: Accretion properties of class II and transitional objects
• A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation
• Accretion in the Rho-Oph pre-main sequence stars
• Mass inventory of the giant-planet formation zone in a solar nebula analog
• Grain growth in the envelopes and disks of Class I protostars
• Temperaments of young stars: Rapid mass-accretion rate changes in T Tauri and Herbig Ae stars
• Magnetically self-regulated formation of early protoplanetary discs
• Accretion in protoplanetary disks: the imprint of core properties
• Constraints from Dust Mass and Mass Accretion Rate Measurements on Angular Momentum Transport in Protoplanetary Disks
• Protoplanetary Disks as (Possibly) Viscous Disks

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• X-Shooter survey of disk accretion in Upper Scorpius I. Very high accretion rates at age>5 Myr