Impact disruption of gravity-dominated bodies: New simulation data and scaling

N. Movshovitz, F. Nimmo, D.G. Korycansky, E. Asphaug, J.M. Owen
2016 Icarus (New York, N.Y. 1962)  
We present results from a suite of 169 hydrocode simulations of collisions between planetary bodies with radii from 100 to 10 0 0 km. The simulation data are used to derive a simple scaling law for the threshold for catastrophic disruption, defined as a collision that leads to half the total colliding mass escaping the system post impact. For a target radius 100 ≤ R T ≤ 10 0 0km and a mass M T and a projectile radius r p ≤ R T and mass m p we find that a head-on impact with velocity magnitude v
more » ... is catastrophic if the kinetic energy of the system in the center of mass frame, , the gravitational binding energy of the system at the moment of impact; G is the gravitational constant. In all head-on collision runs we find K * = (5 . 5 ± 2 . 9 ) U. Oblique impacts are catastrophic when the fraction of kinetic energy contained in the volume of the projectile intersecting the target during impact exceeds ∼2 K * for 30 °impacts and ∼3.5 K * for 45 °impacts. We compare predictions made with this scaling to those made with existing scaling laws in the literature extrapolated from numerical studies on smaller targets. We find significant divergence between predictions where in general our results suggest a lower threshold for disruption except for highly oblique impacts with r p R T . This has implications for the efficiency of collisional grinding in the asteroid belt ( Morbidelli et al., [2009] Icarus, 204, 558-573), Kuiper belt (Greenstreet et al., [2015] Icarus, 258, 267-288), and early Solar System accretion (Chambers [2013], Icarus, 224, 43-56).
doi:10.1016/j.icarus.2016.04.018 fatcat:2ss7bmidxndw3o3ely4fftuej4