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The LongTerm Behaviour of Two Pulsating Variables in M56

Published online by Cambridge University Press:  12 April 2016

Amelia Wehlau ,
Philip Rice ,
Marcia Wehlau  and
Helen Sawyer Hogg
Amelia Wehlau
Affiliation:
Department of Astronomy, The University of Western Ontario
Philip Rice
Affiliation:
Department of Astronomy, The University of Western Ontario
Marcia Wehlau
Affiliation:
Department of Astronomy, The University of Western Ontario
Helen Sawyer Hogg
Affiliation:
David Dunlap Observatory, University of Toronto

Extract

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Of twelve variables known in Messier 56 in Lyra, two, V1 and V6 are the subject of this paper. VI was discovered by Shapley (1920) and first determined by Sawyer Hogg (1942) to be a Cepheid with a period of 1.5 days. V6 was discovered by Sawyer Hogg (1940) from her early plates at the David Dunlap Observatory. Later Sawyer Hogg (1949) showed it to be an RV Tauri type with a period of 90.02 days, one of the first such to be identified in a globular cluster. A.H.Joy (1949) determined spectral type and radial velocity for both of these variables.

Type
Part IV. Population II Cepheids
Information
International Astronomical Union Colloquium , Volume 82: Cepheids: Theory and Observations , 1985 , pp. 284 - 287
Copyright
Copyright © Cambridge University Press 1985

References

Carson, T. R., and Stothers, R. 1976, Astrophys. J., 204, 461.10.1086/154190CrossRefGoogle Scholar
Clement, C., Sawyer Hogg, H. and Lake, K. 1984a, in IAU Colloquium 82, Cepheids: Observation and Theory, edited by Madore, Barry F. (University of Cambridge, Cambridge), p·260.Google Scholar
Clement, C., Sawyer Hogg, H. and Wells, T. 1984b, in IAU Colloquium 82, Cepheids: Observation and Theory, edited by Madore, Barry F. (University of Cambridge, Cambridge), p. 262.Google Scholar
Davis, C. G. 1982, in Pulsations in Classical and Cataclysmic Variable Stars, edited by Cox, J. P. and Hansen, C. J. (University of Colorado, Boulder), p.232.Google Scholar
Davis, C. G., Moffett, T. J. and Barnes, T. G. 1981, Astrophys.J., 246, 914.10.1086/158984CrossRefGoogle Scholar
Harris, H. C., Olszewski, E. W. and Schommer, R. A. 1981, private communication.Google Scholar
Joy, A. H. 1949, Astrophys.J., 110, 105.10.1086/145190CrossRefGoogle Scholar
Rosino, L. 1944, Pub.Oss.Astr.Bologna, 4 No.7.Google Scholar
Rosino, L. 1949, Pub.Oss.Astr.Bologna 5, No.12.Google Scholar
Sawyer, H. B. 1940, D.D.O. Pub.1, No.5.Google Scholar
Sawyer, H. B. 1942, Pub.A.A.S., 10, 233.Google Scholar
Sawyer, H. B. 1949, J.Roy.Astr.Soc.Can., 43, 38.Google Scholar
Shapley, H. 1920, Astrophys.J., 52, 73.10.1086/142560CrossRefGoogle Scholar
Wehlau, A. and Bohlender, D. 1982, Astron.J., 87, 780.10.1086/113156CrossRefGoogle Scholar