Fragment properties from large-scale asteroid collisions: I: Results from SPH/N-body simulations using porous parent bodies and improved material models

Abstract

Understanding the collisional fragmentation and subsequent reaccumulation of fragments is crucial for studies of the formation and evolution of the small-body populations. Using an SPH / N-body approach, we investigate the size-frequency distributions (SFDs) resulting from the disruption of 100 km-diameter targets consisting of porous material, including the effects of pore-crushing as well as friction. Overall, the porous targets have a significantly higher impact strength (Q*D) than the rubble-pile parent bodies investigated previously (Benavidez et al., 2012) and show a behavior more similar to non-porous monolithic targets (Durda et al., 2007). Our results also confirm that for a given specific impact energy, the SFDs resulting from a parent body disruption are strongly dependent on the size scale.

26 pages, 12 figures; accepted for publication in Icarus

References in corpus (7)

• Numerical simulations of impacts involving porous bodies: I. Implementing sub-resolution porosity in a 3D SPH Hydrocode
• SPH calculations of asteroid disruptions: The role of pressure dependent failure models
• Effects of friction and plastic deformation in shock-comminuted damaged rocks on impact heating
• Resolution Dependence of Disruptive Collisions between Planetesimals in the Gravity Regime
• Impact Erosion Model for Gravity-Dominated Planetesimals
• SPH/N-body simulations of small (D = 10 km) asteroidal breakups and improved parametric relations for Monte-Carlo collisional models
• Collisional Disruption of Planetesimals in the Gravity Regime with iSALE Code: Comparison with SPH code for Purely Hydrodynamic Bodies

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