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On the Formation of Planetesimals

Published online by Cambridge University Press:  25 April 2016

K. Hourigan  and
A. J. R. Prentice
K. Hourigan
Affiliation:
Department of Mathematics, Monash University
A. J. R. Prentice
Affiliation:
Department of Mathematics, Monash University
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Extract

The past and present existence of smaller bodies in our solar system manifests itself in various ways through the appearance of asteroids, minor moons, planetary rings, surface cratering, etc. The occurrence of these planetesimals appears to be an integral intermediary step in the formation of the larger bodies from the initial grain state. In order to account for the discreteness and order of the planetary orbits and regular satellite systems, Prentice (1977, 1978) has suggested that the accumulation of this planetesimal material took place in a series of well defined orbits corresponding to the positions of a system of gaseous Laplacian rings that were shed by the primitive contracting parent cloud. Alfvén and Arrhenius (1975) have also drawn attention to the fact that planetesimal formation occurs far more effectively if the accumulation takes place along well defined ‘jet streams’. Hourigan (1977) has previously demonstrated how such concentrated rock/ice streams or ‘jet-streams’ naturally form on the mean Keplerian orbit of gaseous rings that are present in the Prentice-Laplace model.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 3 , Issue 6 , 1979 , pp. 389 - 390
Copyright
Copyright © Astronomical Society of Australia 1979

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References

Alfven, H., and Arrhenius, G., ‘Structure and Evolutionary History of the Solar System’, Reidel, D. Publishing Company, Holland (1975).CrossRefGoogle Scholar
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Hourigah, K., Proc. Aslron. Soc. Aust., 3, 169 (1977).CrossRefGoogle Scholar
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Prentice, A.J.R., in ‘The Origin of the Solar System’ (Ed. Dermott, S.F.) p.p. 111–161, John Wiley and Sons, London (1978).Google Scholar