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Porosity models for pre-planetesimals: modified P-α like models and the effect of dissipated energy

Published online by Cambridge University Press:  10 November 2011

Serena E. Arena  and
Roland Speith
Serena E. Arena
Affiliation:
Université de Lyon, Lyon, F-69003, France; Université Lyon 1, Villeurbanne, F-69622, France; CNRS, UMR 5574, Centre de Recherche Astrophysique de Lyon; École normale supérieure de Lyon, 46, allée d'Italie, F-69364 Lyon cedex 07, France email: serena.arena@ens-lyon.fr
Roland Speith
Affiliation:
Physikalisches Institut, Universität Tübingen, Auf der Morgenstelle 14, D-72076 Tübingen, Germany email: speith@pit.physik.uni-tuebingen.de
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Abstract

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The outcome of collisions between pre-planetesimals is important in the theory of planetesimal formation by collisional growth and strongly depends on their internal structure. Since pre-planetesimals are highly porous, reaching 90% porosity, they could show the so called anomalous behaviour (decrease of density during shock compression, e.g. Bolkhovitinov & Khvostov 1978). Due to involved sizes (>dm), laboratory experiments are unfeasible therefore numerical simulations equipped with adequate porosity models are necessary.

Here we focus on the P-α model and its variations. We found that they are suitable for applications in the high porosity range only after a modification of the basic equations, that avoids an inconsistency and takes into account the effect of dissipated energy, is performed.

Keywords

equation of stateshock wavesinterplanetary medium
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 395 - 396
Copyright
Copyright © International Astronomical Union 2011

References

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