Long-term dust and pebble disk mass evolution (top), as well as dust mass ejected due to radiation pressure (middle) and accreted onto the star (bottom). All models start with a low v_frag of 1 × 10⁻² cm s⁻¹ and do not include the effect of dust entrainment in photoevaporative winds. The thick gray line denotes the model without Poynting–Robertson drag but with direct ejection of the smallest grains due to radiation pressure. The inverted assumptions are shown with a green line. The nominal model (dotted black line) includes both effects and is equivalent to the low-v_ftag case shown in the top row of Fig. 5.