Left: temporal variation due to PR drag of the semimajor axis (a) and eccentricity (b) of olivine-type particles with β = 0.3 starting with initial a = 70 au and e = 0.4 (blue lines) and β = 0.4 with initial a = 120 au and e = 0.7 (red). These initial conditions were motivated by the peak of the a and e distributions as illustrated in Figure 4. The shaded regions show the range of their radial motion a(1 − e) ≤ r ≤ a(1 + e). Right: temporal variation over 2 Myr of the semimajor axis (c), eccentricity (d) dotted lines, and radius (d) bottom solid lines of 1 (blue line) and 5 μm (red) photo-sputtered ice particles, launched with an initial semimajor axis a = 45 au and eccentricity e = 0.1. Small ice grains continuously gain energy and drift outwards out of the solar system, while bigger particles initially drift inward until their mass loss results in a large enough β to reverse the direction of their drift and eventually also leave the solar system.