Timescale diagnostics for saving viscous and MHD-wind-driven dusty discs from external photoevaporation

Open Access

Fig. B.2

Results for a setup including (dashed lines) and not including (continuous lines) dust radial drift. The top three rows plot the same quantities as in Fig. 3, with different columns corresponding to different ψ_DW = α_DW/α_SS. We add the mass accretion rates as a bottom row (see Fig. 1).

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