Hostname: page-component-7bb8b95d7b-5mhkq Total loading time: 0 Render date: 2024-09-06T00:21:21.600Z Has data issue: false hasContentIssue false
  • English
  • Français

The Early Evolution of the Solar System

Published online by Cambridge University Press:  12 April 2016

A. G. W. Cameron
A. G. W. Cameron*
Affiliation:
Yeshiva University and Goddard Institute for Space Studies, NASANew York, New York

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The problems of relating collapse conditions in an interstellar cloud to a model of the primitive solar nebula are discussed. In such a nebula there is a radial force balance between gravity, the pressure gradient, and centrifugal forces due to the rotation. Approximate values are given for the combinations of temperature and density throughout the nebula, from a maximum of about 2000° K near the center to less than 200° K in the outer portion. These conditions are based upon the compression adiabats in the terminal stages of the collapse of an interstellar cloud. One general conclusion, of great importance for accumulation of bodies within the solar system, is that interstellar grains should not be completely evaporated at distances in the nebula beyond about one or two astronomical units.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 13: Evolutionary and Physical Properties of Meteoroids , June 1971 , pp. 347 - 353
Copyright
Copyright © NASA 1971

References

Cameron, A. G. W., 1970. Formation of the Earth-Moon system, EOS, Trans. Am. Geophys. Union, 51, 628–633.Google Scholar
Larson, R. B., 1969. Numerical calculations of the dynamics of a collapsing proto-star, Monthly Notices Roy. Astron. Soc, 145, 271–295.CrossRefGoogle Scholar