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Psi Sagittarii, A System with Three Evolved Components*

Published online by Cambridge University Press:  12 April 2016

F. C. Fekel
F. C. Fekel*
Affiliation:
Department of Astronomy University of Texas at Austin

Abstract

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The visual binary Psi Sagittarii (ADS 12214, HR 7292) is a spectroscopic triple system with orbital periods of 10.78 days and 20.0 years. Periastron passage in the long period crbit occurred on JD 2442410 ± 30 days. Masses derived from the parameters of the spectroscopic and visual orbits are 2.7 m⊙ for the visual primary, 2.1 m⊙ for the short period pair primary, and 1.7 m⊙ for the short period pair secondary. The distance to the system is 100 parsecs. The orbital inclination of the close pair is nearly the same numerically as that of the visual orbit. Suggested spectral classifications indicate that all three components have evolved off the main sequence. Mass exchange in the close pair has not yet occurred.

Resumen

Resumen

La binaria visual Psi Sagittarii (ADS 12214, HR7292) es en realidad un sistema triple espectroscópico con períodos orbitales de 10.78 días y 20.0 años. El paso por el periastro en la òrbita de largo período ocurrió el JD 2442410 ± 30 días. Las masas obtenidas de los parámetros orbitales espectroscópicos y visuales son: 2.7 m⊙ para la primaria visual y 2.1 m⊙ para la primaria del par de período corto y 1.7 m⊙ para la secundaria del par con período corto. La distancia al sistema es de 100 parsecs. La inclinación orbital del par cerrado es casi la misma numéricamente que la de la órbita visual. Las clasificaciones espectrales que se han sugerido indican que las tres componentes han evolucionado fuera de la secuencia principal. Aún no ha ocurrido intercambio de masa en el par cerrado.

Type
Session 3
Information
International Astronomical Union Colloquium , Volume 33: Observational Parameters and Dynamical Evolution of Multiple Stars , May 1977 , pp. 89 - 92
Copyright
Copyright © Otto G. Franz and Paris Pismis 1977

Footnotes

*

Figures 1, 2, 3 and 5 have been reproduced from Astronomical Journal, Vol. 80, p. 844 ff, published by the American Institute of Physics for the American Astronomical Society.

References

Dommanget, J., and Nys, O. 1967, Comm. Obs. R. Belgique, B15.Google Scholar
Evans, D. S. 1956, M.N.R.A.S., 116, 537.CrossRefGoogle Scholar
Evans, D. S. 1968, Quart. J.R.A.S., 9, 388.Google Scholar
Evans, D. S. 1969, M.N.R.A.S., 142, 523.CrossRefGoogle Scholar
Finsen, W. S., and Worley, C. E. 1970, Republ. Obs. Johannesb. Circ, 7, N» 129.Google Scholar
Harris, D. L., Strand, K. Aa., and Worley, C. E. 1963, Basic Astronomical Data, ed. Strand, K. Aa. (Chicago: University of Chicago Press), 273.Google Scholar
Heintze, J. R. W. 1973, IAU Symposium N° 54, eds. Hauck, B. and Westerlund, B. E. (Dordrecht: D. Reidel), 231.Google Scholar
Iben, I. 1967a, Ap. J., 147, 624.CrossRefGoogle Scholar
Iben, I. 1967b, Ap. J., 147, 650.Google Scholar
Pésurname>trie, R. M., and Batten, A. H. 1970, Pub. D.A.O., 13, 383.trie,+R.+M.,+and+Batten,+A.+H.+1970,+Pub.+D.A.O.,+13,+383.>Google Scholar
Pétrie, R. M., and Laidler, D. M. 1952, Pub. D.A.O., 9, 181.Google Scholar
van den Bos, W. H. 1957, Union Obs. Circ, 116, 291.Google Scholar
van Flandern, T. C. 1975, private communication.Google Scholar