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7. The Solar Nebula Pressure Gradient and its Effect on Planetesimal Motions

Published online by Cambridge University Press:  12 April 2016

S. J. Weidenschilling

Abstract

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In a centrally condensed solar nebula, the gas is partially supported by a pressure gradient, and rotates at less than the Keplerian velocity. Solid bodies lack this support, and spiral inward due to drag. The radial velocities developed can be significant, even in low-mass nebular models. Possible effects include fractionation of particles by size or density, rapid accumulation of planetesimals, and production of regions of anomalous (non-solar) composition in the nebula.

Type
Part IX. The Primitive Solar Nebula
Information
International Astronomical Union Colloquium , Volume 39: Comets, Asteroids, Meteorites: Interrelations, Evolution and Origins , December 1977 , pp. 541 - 544
Copyright
Copyright © A.H. Delsemme 1977

References

Cameron, A.G.W. 1973, Icarus, 18, 407.Google Scholar
Cameron, A.G.W., and Pine, M. R. 1973, Icarus, 18, 377.Google Scholar
Lewis, J. S. 1974, Science, 186, 440.Google Scholar
Whipple, F. L. 1972, in From Plasma to Planet, Elvius, A., ed. (Wiley, New York).Google Scholar
Whipple, R. L. 1973, in Evolutionary and Physical Properties of Meteoroids, NASA SP-319.Google Scholar