Do accretion-powered stellar winds help spin down T Tauri stars?

How T Tauri stars remain slowly rotating while still accreting material is a long-standing puzzle. Current models suggest that these stars may lose angular momentum through magnetospheric ejections of disk material (MEs) and accretion-powered stellar winds (APSWs). The individual contribution of each mechanism to the stellar spin evolution, however, is unclear. We explore how these two scenarios could be distinguished by applying stellar spin models to near-term observations. We produce synthetic stellar populations of accreting Class II stars with spreads in the parameters governing the spin-down processes and find that an APSW strongly affects the ratio of the disk truncation radius to the corotation radius, $\mathcal{R}=R_{\mathrm{t}}\mathrm{/}{R}_{\mathrm{c}\mathrm{o}}$. The ME and APSW scenarios are distinguished to high confidence when at least $N_{\mathrm{c}\mathrm{r}\mathrm{i}\mathrm{t}}\gtrsim 250$ stars have values measured for $\mathcal{R}$. Newly developed lightcurve analysis methods enable measuring $\mathcal{R}$ for enough stars to distinguish the spin-down scenarios in the course of upcoming observing campaigns.