Impact disruption of gravitydominated bodies: New simulation data and scaling
We present results from a suite of 169 hydrocode simulations of collisions between planetary bodies with radii from 100 to 1000 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} ≤ 1000km and a mass M _{T} and a projectile radius r _{p} ≤ R _{T} and mass mp we find that a headon impact with velocity magnitude v is catastrophic if the kinetic energy of the system in the center of mass frame, K=0.5 M _{T}m _{p}v ^{2}/(M _{T}+m _{p}) exceeds a threshold value K* that is a few times U= (3/5) GM$$2\atop{T}$$/RT+ (3/5) Gm$$2\atop{p}$$/r _{p} + GM _{T}m _{p}/(R _{T}+r _{p}), the gravitational binding energy of the system at the moment of impact; G is the gravitational constant. In all headon 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 rp << RT. Lastly, 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).
 Authors:

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 Univ. of California, Santa Cruz, CA (United States). Dept. of Earth and Planetary Sciences
 Arizona State Univ., Tempe, AZ (United States). School of Earth and Space Exploration
 Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
 Publication Date:
 Report Number(s):
 LLNLJRNL734522
Journal ID: ISSN 00191035; 886074
 Grant/Contract Number:
 AC5207NA27344
 Type:
 Accepted Manuscript
 Journal Name:
 Icarus
 Additional Journal Information:
 Journal Volume: 275; Journal Issue: C; Journal ID: ISSN 00191035
 Publisher:
 Elsevier
 Research Org:
 Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
 Sponsoring Org:
 USDOE National Nuclear Security Administration (NNSA)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 79 ASTRONOMY AND ASTROPHYSICS; 58 GEOSCIENCES; Collisional physics; Planetesimals; Planetary formation
 OSTI Identifier:
 1466931
Movshovitz, N., Nimmo, F., Korycansky, D. G., Asphaug, E., and Owen, J. M.. Impact disruption of gravitydominated bodies: New simulation data and scaling. United States: N. p.,
Web. doi:10.1016/j.icarus.2016.04.018.
Movshovitz, N., Nimmo, F., Korycansky, D. G., Asphaug, E., & Owen, J. M.. Impact disruption of gravitydominated bodies: New simulation data and scaling. United States. doi:10.1016/j.icarus.2016.04.018.
Movshovitz, N., Nimmo, F., Korycansky, D. G., Asphaug, E., and Owen, J. M.. 2016.
"Impact disruption of gravitydominated bodies: New simulation data and scaling". United States.
doi:10.1016/j.icarus.2016.04.018. https://www.osti.gov/servlets/purl/1466931.
@article{osti_1466931,
title = {Impact disruption of gravitydominated bodies: New simulation data and scaling},
author = {Movshovitz, N. and Nimmo, F. and Korycansky, D. G. and Asphaug, E. and Owen, J. M.},
abstractNote = {We present results from a suite of 169 hydrocode simulations of collisions between planetary bodies with radii from 100 to 1000 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 ≤ RT ≤ 1000km and a mass MT and a projectile radius rp ≤ RT and mass mp we find that a headon impact with velocity magnitude v is catastrophic if the kinetic energy of the system in the center of mass frame, K=0.5 MTmpv2/(MT+mp) exceeds a threshold value K* that is a few times U= (3/5) GM$2\atop{T}$/RT+ (3/5) Gm$2\atop{p}$/rp + GMTmp/(RT+rp), the gravitational binding energy of the system at the moment of impact; G is the gravitational constant. In all headon 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 rp << RT. Lastly, 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},
journal = {Icarus},
number = C,
volume = 275,
place = {United States},
year = {2016},
month = {4}
}