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On the Detection of Binary Be Stars

Published online by Cambridge University Press:  14 August 2015

R. S. Polidan
R. S. Polidan*
Affiliation:
Dept. of Astronomy, University of California, Los Angeles, Calif., U.S.A.

Abstract

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Possible methods for detecting the presence of a cool companion to a Be star are discussed. Photometric observations are shown to be incapable of detecting companions in all but the most extreme cases. Spectroscopic investigation is also unlikely to yield many new discoveries. It, however, remains the most promising method for the detection of binary Be stars. The four known binary Be stars are also discussed.

Infrared calcium triplet emission in Be stars is discussed in detail. The lines are shown to originate in a region of large optical thickness and low temperature (T ~ 5000 K). The possible connection between the presence of calcium triplet emission and binary nature is briefly discussed.

Type
Part VI: Single Versus Binary Stars
Information
Symposium - International Astronomical Union , Volume 70: Be and Shell Stars , 1976 , pp. 401 - 415
Copyright
Copyright © Reidel 1976 

References

Allen, D. A.: 1973, Monthly Notices Roy. Astron. Soc. 161, 145.CrossRefGoogle Scholar
Andrillat, Y. and Houziaux, L.: 1967, J. Observ. 50, 107.Google Scholar
Cowley, A. P.: 1964, Astrophys. J. 139, 817.CrossRefGoogle Scholar
Cowley, A. P.: 1967, Astrophys. J. 147, 609.CrossRefGoogle Scholar
Doazan, V. and Peton, A.: 1970, Astron. Astophys. 9, 245.Google Scholar
Gehrz, R. D., Hackwell, J. A., and Jones, T. W.: 1975, Astrophys. J. 191, 675.CrossRefGoogle Scholar
Herbig, G. H.: 1952, Astrophys. J. 116, 369.CrossRefGoogle Scholar
Hill, G. and Hutchings, J. B.: 1970, Astrophys. J. 162, 265.CrossRefGoogle Scholar
Hiltner, W. A.: 1947, Astrophys. J. 105, 212.CrossRefGoogle Scholar
Houziaux, L.: 1962, Publ. Astron. Soc. Pacific 74, 250.CrossRefGoogle Scholar
Johnson, H. L., Mitchell, R. I., Iriarte, B., and Wisniewski, W. Z.: 1966, Comm. Lunar Planetary Laboratory 4, 99.Google Scholar
Kraft, R. P.: 1957, Astrophys. J. 125, 336.CrossRefGoogle Scholar
Kríz, S. and Harmanec, P.: 1975, Bull. Astron. Inst. Czech. 26, 65.Google Scholar
Lockwood, G. W., Dyck, H. M., and Ridgway, S. T.: 1975, Astrophys. J. 195, 385.CrossRefGoogle Scholar
Merrill, P. W.: 1934, Astrophys. J. 79, 183.CrossRefGoogle Scholar
Pagel, B. E. J.: 1960, Vistas in Astronomy 3, 203.CrossRefGoogle Scholar
Peters, G. J.: 1972, Publ. Astron. Soc. Pacific 84, 498.Google Scholar
Peton, A.: 1974, Astrophys. Space Sci. 30, 481.CrossRefGoogle Scholar
Plaskett, J. S., Harper, W. E., Young, R. K., and Plaskett, H. H.: 1920, Publ. Dominion Astrophys. Obs. 1, 163.Google Scholar
Slettebak, A.: 1950, Astrophys. J. 112, 559.CrossRefGoogle Scholar
Swings, J. P.: 1973, Astron. Astrophys. 26, 443.Google Scholar
Wellman, P.: 1951, Z. Astrophys. 30, 71.Google Scholar
Wyse, A. B.: 1941, Publ. Astron. Soc. Pacific 53, 184.CrossRefGoogle Scholar