Evolution of the mass-loss rate inside 80 au calculated using PLUTO+PRIZMO. Panel a: Comparison between models using the X-ray spectrum of Ercolano et al. (2021, E21) (blue; 200 orbits at 10 au) and that of Nakatani et al. (2018b, N18) (green; 150 orbits at 10 au). For comparison, we also include 50 orbits of an analogue of the Picogna et al. (2021, P21) model (which uses a ξ − T relationship derived from MOCASSIN) as the black dashed line, and the value at 1 M_⊙ from the fit to $\dot{M}(M_{\ast }$) given in Komaki et al. (2021) as the grey dotted line. Panel b: Zoom-in on the first 50 orbits (at 10 au) of our fiducial simulation with the X-ray spectrum of Ercolano et al. (2021, E21) (dark blue) compared with models where we turn off the cooling due to collisions between O and H and include negligible dust (turquoise) or turn off the cooling due to H₂ (light blue). For comparison, we again include 50 orbits of the Picogna et al. (2021, P21) analogue simulation as the black dashed line.