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On the Origin of the Algol Systems

Published online by Cambridge University Press:  30 March 2016

M. Plavec

Extract

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The 4th edition of the Finding List for Observers of Eclipsing Variables (Koch et al, 1963) contains 145 sufficiently well-observed eclipsing binaries brighter than 8·5m at maximum light. Among them, 59 binaries, or 41%, are systems with both components on the main sequence. The second largest group, 52 binaries or 36% of all systems, are systems similar to Algol. These can be characterized as follows:

  1. (1) The primary (more massive) components are main-sequence stars, fitting well into the mass-luminosity relation defined by visual binaries and by eclipsing binaries with both components on the main sequence (detached systems).

  2. (2) The secondary components are of later spectral type than the primaries, and can be best characterized as subgiants. They are overluminous for their mass as well as for their spectral class.

  3. (3) As a rule, the secondary components fill their respective critical Roche lobes (innermost Lagrangian surfaces).

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 1: Highlights of Astronomy. As presented at the XIIIth General Assembly of the IAU, 1967 , 1968 , pp. 396 - 408
Copyright
Copyright © Reidel 1968

References

Crawford, J.A. (1955) Astrophys. J., 121,71.Google Scholar
Giannone, P., Kohl, K., Weigert, A. (1968) Z. Astrophys., 68, 107.Google Scholar
Henyey, L.G., Forbes, J.E., Gould, N.L. (1964) Astrophys. J., 139,306.CrossRefGoogle Scholar
Iben, I. (1966) Astrophys.J., 143, 483.Google Scholar
Kippenhahn, R., Weigert, A. (1967) Z. Astrophys., 65, 251.Google Scholar
Kippenhahn, R., Kohl, K., Weigert, A. (1967) Z. Astrophys., 66, 58.Google Scholar
Koch, R.H., Sobieski, S., Wood, F.B. (1963) Publ. Univ. Pa. astr. ser., 9.Google Scholar
Kopal, Z. (1954) Jodrell Bank Ann., 1,37.Google Scholar
Morton, D.C. (1960) Astrophys. J., 132, 146.CrossRefGoogle Scholar
Paczyński, B. (1966) Acta astr., 16, 231.Google Scholar
Paczyński, B. (1967) Acta astr., 17,1.Google Scholar
Paczyński, B., Ziólkowski, J. (1967) Acta astr., 17, 7.Google Scholar
Plavec, M. (1967a) Bull. astr. Inst. Csl., 18, 253.Google Scholar
Plavec, M. (1967b) Bull. astr. Inst. Csl., 18, 334.Google Scholar
Plavec, M. (1968a) Adv. Astr. Astrophys., 6, 201.CrossRefGoogle Scholar
Plavec, M. (1968b) Bull. astr. Inst. Csl., 19, in press.Google Scholar
Plavec, M., Kratochvíl, P. (1964) Bull. astr. Inst. Csl., 15, 165.Google Scholar
Plavec, M., Kříž, S., Harmanec, P., Horn, J. (1968a) Bull. astr. Inst. Csl., 19, 24.Google Scholar
Plavec, M., Kříž, S., Harmanec, P., Horn, J. (1968b) Bull. astr. Inst. Csl., 19, in press.Google Scholar
Roxburgh, I.W. (1966) Astr. J., 71, 133.Google Scholar
Smak, J. (1962) Acta astr., 12, 28.Google Scholar