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Collision and impact simulations including porosity

Published online by Cambridge University Press:  01 August 2006

Willy Benz  and
Martin Jutzi
Willy Benz
Affiliation:
Physikalisches Institut, University of Bern, Siedlerstrasse 5, 3012 Bern, Switzerland email: willy.benz@space.unibe.ch
Martin Jutzi
Affiliation:
Physikalisches Institut, University of Bern, Siedlerstrasse 5, 3012 Bern, Switzerland email: willy.benz@space.unibe.ch
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Abstract

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The Smooth Particle Hydrodynamics (SPH) impact code (Benz & Asphaug 1994) has been developed for the simulation of impacts and collisions involving brittle solids in the strength-and gravity-dominated regime. In the latter regime, the gravitational overburden is used to increase the fracture threshold. In this paper, we extend our numerical approach to include the effect of porosity at a sub-resolution scale by adapting the so-called P -α model (Herrman 1969). Using our extended 3D SPH impact code, we investigated collisions between porous bodies to examine the sensitivity of collisional outcomes to the degree of porosity. Two applications that illustrate the capabilities of our approach are shown: 1) the modeling of a Deep Impact-like impact and 2) the computation of the amount of momentum transferred to an asteroid following the impact of a high velocity projectile.

Keywords

Hydrodynamicsshock waveequation of state
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S236: Near Earth Objects, our Celestial Neighbors: Opportunity and Risk , August 2006 , pp. 223 - 231
Copyright
Copyright © International Astronomical Union 2007

References

Benz, W. 1992, in: Büchler, J.R. (eds.), The numerical modelling of nonlinear stellar pulsations: Problems and prospects (Springer: Berlin), p. 269.Google Scholar
Benz, W. & Asphaugh, E. 1994, Icarus 107, 98CrossRefGoogle Scholar
Benz, W. & Asphaugh, E. 1995, Comp. Phys. Comm. 87, 253CrossRefGoogle Scholar
Britt, D. T., Consolmagno, G. J. & Merline, W. J. 2006, 37th Annual Lunar and Planetary Science Conference, 2214Google Scholar
Carroll, M. M. & Holt, A. C. 1972, J. Appl. Phys. 43, 759Google Scholar
Herrmann, W. 1969, J. Appl. Phys. 40, 2490CrossRefGoogle Scholar
Housen, K. R. & Holsapple, K. A. 2003, Icarus 163, 102CrossRefGoogle Scholar
Jutzi, M. 2004, Diploma thesis, University of BernGoogle Scholar
Libersky, L. D. & Petschek, A. G. 1990, in Lecture Notes in Physics 395, 248CrossRefGoogle Scholar
Melosh, H. J. 1989, Impact cratering: A geologic process (Oxford: Oxford University Press)Google Scholar
Monaghan, J. J. 1992, Annu. Rev. Astron. Astrophys. 30, 543CrossRefGoogle Scholar
Wuennemann, K., Collins, G. S. & Melosh, H. J. 2006, Icarus 180, 514CrossRefGoogle Scholar
Wurm, G., Paraskov, G. & Krauss, O. 2005, Icarus 178, 253CrossRefGoogle Scholar