Effect of MHD Wind-driven Disk Evolution on the Observed Sizes of Protoplanetary Disks

It is still unclear whether the evolution of protoplanetary disks, a key ingredient in theory planet formation, driven by viscous turbulence or magnetic disk winds. As viscously evolving disks expand outward over time, sizes discriminant test for studying evolution. However, it how observed size changes time if Combining thermochemical code DALI with analytical wind-driven model presented Tabone et al. (2021a), we study gas outer radius as measured from CO rotational emission ($R_{\rm CO, 90\%}$). The $R_{\rm 90\%}$ mass, physical stays constant time. For $\alpha_{\rm DW}$, an extension $\alpha-$Shakura-Sunyaev parameter to accretion, decreases linearly Its initial set mass and characteristic $R_c$, but only $R_c$ affects 90\%}$, larger resulting steeper decrease 90\%}$. time-dependent DW}$ approximately during most lifetime until rapidly shrinks dissipates. DW}$-models are able reproduce $\sim1-3$ Lupus $\sim5-11$ Myr old Upper Sco star-forming regions. they likely overpredict younger $(\lessapprox0.7\ \mathrm{Myr})$ disks.