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The Instability of Sub-Giants in Close Binary Systems

Published online by Cambridge University Press:  14 August 2015

Zdeněk Kopal
Zdeněk Kopal*
Affiliation:
Department of Astronomy, University of Manchester, Manchester, England

Extract

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I should like to open my subject by attempting to answer the following question: how many parameters are necessary and sufficient for a complete specification of the form of both components in close binary systems? Their shape should, in principle, be specified by the nature of forces acting on their surfaces, and (provided that the free period non-radial oscillations of both components are short in comparison with that of their orbits) their distortion should be governed by the equilibrium theory of tides. The level surfaces of constant density then coincide with those of constant potential, and the boundary of zero density becomes a particular case of such equipotentials.

Type
V. Phenomena of Instability in Binary Systems
Information
Symposium - International Astronomical Union , Volume 3: Non-Stable Stars , 1957 , pp. 123 - 137
Copyright
Copyright © Cambridge University Press 1957 

References

1. For their tabulation cf. Kopal, Z., Jodrell Bank Ann. 1, 37 (1954) (Table V, col. 2).Google Scholar
2. Details of this process are being postponed for subsequent publication.Google Scholar
3. The material at the basis of this study is summarized in Table V of the Draft Report prepared by the writer on behalf of Commission 42 of the I.A.U. for the 9th General Assembly in Dublin, and will be published in the I.A.U. Transactions, vol. 9.Google Scholar
4. Cf. Kopal, Z., Jodrell Bank Ann. 1, 37 (1954) (Table I, col. 7).Google Scholar
5. This conclusion, announced by the writer at the sixth International Astrophysical Colloquium at Liège in July 1954 (cf. Communications presentées au sixième Colloque International d'Astrophysique, Liège, 1955, pp. 684–5), was independently arrived at by Crawford, J. A. [Ap.J. 121, 71 (1955)] on the basis of a statistical study of completely different material.Google Scholar
6. For fuller details cf., e.g., Moulton, F. R., An Introduction to Celestial Mechanics (6th ed., New York, 1939) chapter VIII, sec. 154.Google Scholar
7. These angles have been tabulated for different mass-ratios by Kopal in Jodrell Bank Ann. 1, 37 (1954) (Table III).Google Scholar
8. Struve, O., Ann. d'Ap. 11, 117 (1948); also Harvard Centennial Symposia (Harv. Obs. Mono. No. 7, Cambridge, 1948), pp. 211–30.Google Scholar