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tokens: in denser environments, for example, star clusters ( Varri et al. 2018 ) or the Galactic bulge, where thousands of NSs may be present (e.g. Fragione et al. 2018 ). The encounter velocities originating from SN kicks will be significantly higher than the virialised velocities that have been used in published simulations (e.g. Wang et al. 2020 ). In fact, they are closer to what would be expected for a high-velocity star in the Solar neighbourhood ( Laughlin Adams 2000 ). An estimate of the gravitational capture distance, assuming that the intruder can be bound in the centre of mass frame, is given by . This scales as where ‘I’ represents the impactor. For reference, the value for the lowest velocities in our simulations is r grav, BH ≈ 10 −3 pc and r grav, NS ≈ 2 × 10 −4 pc. For b BH, NS ≲ r grav , we found alterations in both the inclination and eccentricity of virtually all retained planets regardless of the incidence angle and encounter velocity (see Appendices B and C ). The most efficient captures for both scenarios occurred in the range 60° ≲ θ BH, NS ≲ 120°, with up to eight planets for b BH, NS ≲ 10 −5 pc and the lowest impact velocity (see f cap in Figs. 2 and 3 ). Eccentricities of the captured planetary orbits, e cap , were very high – around 0.8 for the BH and 0.65 for the NS. Fig. 3. Outcomes of the NS scenario for v NS = 10 km s −1 . For each impact parameter (coded by colours and symbols) and incidence angle (columns), we plotted the final distribution of semi-major axes, eccentricities, and inclinations of planets that were either retained by the Sun or captured by the NS ( top six rows , for each planet from Mercury ☿ to Neptune ♆). Bottom two rows : fraction of retained and captured planets. Each variation in the initial parameters was averaged over nine pre-evolved states of the SS, see Sect. 2 . Detailed plots for all v NS and θ NS are in Figs. C.1 – C.8 . There was a difference between the prograde ( θ BH, NS = 0°) and retrograde ( θ BH, NS = 180°) encounters with the SS in both scenarios. A low-velocity NS showed no directional preferences for planetary capture, but it was most destructive for a retrograde fly-by with b NS ≲ 10 −5 pc; in 60% of the cases, the SS did not survive and in the remaining 40% the Sun was left with only one terrestrial planet (see f ret and f cap in Fig. 3 ). In contrast, a low-velocity BH was generally more disruptive and also more efficient in capturing planets for a prograde encounter (see f ret and f cap in Fig. 2 ). The greatest difference between the NS and BH case was found in the change of the orbital inclinations of the retained planets, i ret , as the BH is more likely to completely flip the orbits of even massive planets. Based on the positions of the planets during the encounter, both intruders were able to capture planets on prograde, retrograde, or 90° orbits while approaching from θ BH, NS = 0° (see i cap ). It was, however, impossible for the NS to capture a retrograde planet