Collisional Family Formation and Scaling Laws: Effects of Porosity and Explicit Formation of Spinning Aggregates

Details Collisional Family Formation and Scaling Laws: Effects of Porosity and Explicit Formation of Spinning Aggregates Collisional Family Formation and Scaling Laws: Effects of Porosity and Explicit Formation of Spinning Aggregates

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5509m&link_type=abstract

American Astronomical Society, DPS meeting #40, #55.09; Bulletin of the American Astronomical Society, Vol. 40, p.499

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Main belt asteroid families are the products of impact events. In recent years, we have been able for the first time to simulate the formation of families and reproduce their main properties. The fragmentation of the asteroid was computed using a 3D SPH hydrocode and the mutual gravitational interaction of the generated fragments was computed with a parallel N-body code (pkdgrav). In our previous simulations, all fragments during the gravitational phase were treated as spheres. We have improved our model by implementing a semi-rigid body approximation. The shapes and spins of the aggregates are preserved as clumps reaccumulate. We will present simulations of asteroid family formation including this explicit formation of spinning aggregates. Our model can provide some clues regarding the likely physical structure (surface, internal) of small bodies resulting from reaccumulation.
Our earlier model of fragmentation was adapted to brittle materials with no porosity at microscales, limiting it to the study of families of S taxonomic type, believed to be composed of such material. Dark (C) type asteroids, Kuiper Belt objects and comets are believed to contain microporosity. We have extended our hydrocode to include the effect of porosity at a sub-resolution scale by adapting the so-called P-alpha model. A first validation at laboratory scale has been performed. We will show its application to dark-type family formation and to the characterization of the impact energy threshold for disruption (Q*D) of porous bodies as a function of their size.
This work is supported by the ESA Advanced Concept Team (Ariadna study "NEO Encounter 2029"), the French Programme National de Planétologie, the Swiss National Science Foundation, NASA under Grant NNX08AM39G issued through the Office of Space Science, the NSF under Grant AST0708110, the cooperation program CNRS-JSPS 2008. We also thank the Mésocentre de Calcul-SIGAMM (Observatoire de la Côte d'Azur, France).

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