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A Monte Carlo Simulation of the Mass Distribution in an Accreting System of Dust Particles

Published online by Cambridge University Press:  14 August 2015

Paul A. Daniels  and
David W. Hughes
Paul A. Daniels
Affiliation:
Department of Physics, The University, Sheffield, UK.
David W. Hughes
Affiliation:
Department of Physics, The University, Sheffield, UK.

Extract

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This paper investigates the way in which the mass distribution index, s, of the particles in a dust cloud varies as a function of time and particle mass, assuming that accretion, and only accretion, takes place after interparticle collisions. The approach is an extension of one first put forward by Napier and Dodd (1974). Two cases are considered. In the first the cloud starts with 500 particles of unit mass and as accretion takes place, more unit mass particles are added to keep that number constant at 500. This simulates a constant source feeding the low mass end of the distribution. In the second case the cloud starts with 5000 particles of unit mass and no additions are made. This corresponds to accretion in a closed system.

Type
III: The Interplanetary Dust Complex 1. Sources, Evolution, and Dynamics
Information
Symposium - International Astronomical Union , Volume 90: Solid Particles in the Solar System , 1980 , pp. 325 - 328
Copyright
Copyright © Reidel 1980 

References

Napier, W. McD., and Dodd, R. J. 1974, Mon. Not. R. astr. Soc. 166, p.469.CrossRefGoogle Scholar
Hughes, D. W. 1972, Planet, and Space Sci., 20, p. 1949.CrossRefGoogle Scholar