Radial accelerations on the equatorial surface at heights of H = 1 cm, for the corresponding particle radius r_a with respect to longitude. The net radial radiative accelerations () are shown.The black horizontal lines show the gravity and the effective gravity as in Fig. 4. a, c) olivine; b, d) magnetite. Panels a and b are calculated for fiducial perpendicular (solid) and aspect 45° (dashed) model asteroids (D = 1 km) at the heliocentric distance r_h = 0.2 au for given particle radii r_a in the legend. For the perpendicular model, the 25% ambiguity inthe thermal inertia (Γ = 200 ± 50 tiu) is expressed as shading. Panels c and d are calculated for Phaethon using the nominal physical parameter values (Table 1) at the perihelion. The shading signifies the uncertainty range in the thermal inertia (Γ = 600 ± 200 tiu, Hanuš et al. 2018) of Phaethon. From these figures, it is obvious that most of ≲ 10μm-sized particles areaccelerated outwards from the AR.