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Physical Properties of Cepheids and RR Lyrae Stars

Published online by Cambridge University Press:  14 August 2015

J. W. Pel  and
J. Lub
J. W. Pel
Affiliation:
Max-Planck-Institut für Astronomie, Heidelberg
J. Lub
Affiliation:
European Southern Observatory, Genéve

Extract

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At the Leiden Southern Station a large program on galactic pulsating variables has been carried out with the Walraven five-channel photometer. For 170 Cepheids and 100 RR Lyrae stars south of δ =+15° there are now available 30000 VBLUW measurements (Walraven et al., 1964; Pel, 1976; Lub, 1977b). These data are used to derive physical properties of the variables. A general discussion of the VBLUW system and its calibration for A-G stars by means of the theoretical fluxes of Kurucz (1975) has been given by Lub and Pel (1977). Following this calibration, reddening and blanketing corrections, as well as effective temperatures, gravities, and their cyclical variations were determined, and luminosity and radius curves were derived (Cepheids: Pel, 1977; RR Lyrae stars: Lub, 1977a). We will present here some interesting results that have been obtained from these data. A more detailed discussion is in preparation.

Type
Part V: HR Diagrams, Horizontal Branch
Information
Symposium - International Astronomical Union , Volume 80: The HR Diagram , 1978 , pp. 229 - 236
Copyright
Copyright © Reidel 1978 

References

Albada, T.S. van and Baker, N.H. (1971). Astrophys. J. 169, 311.Google Scholar
Albada, T.S. van and Baker, N.H. (1973). Astrophys. J. 185, 477.CrossRefGoogle Scholar
Albada, T.S. van and Boer, K.S. de (1975). Astron. Astrophys. 39, 83.Google Scholar
Böhm-Vitense, E., Skody, P., Wallerstein, G. and Iben, I. (1974). Astrophys. J. 194, 125.Google Scholar
Breger, M. (1970). Astron. J. 75, 239.Google Scholar
Butler, C.J. (1976a). Astron. Astrophys. Suppl. 24, 299.Google Scholar
Butler, C.J. (1976b). Roy. Obs. Bull. 182, 159.Google Scholar
Butler, C.J. (1977). preprint.Google Scholar
Cox, A.N., Deupress, R.G., King, D.S. and Hodson, S.W. (1977). Astrophys. J. 214, L127.CrossRefGoogle Scholar
Fricke, K., Stobie, R.S. and Strittmatter, P.A. (1972). Astrophys. J. 171, 593.Google Scholar
Heck, A. (1977). preprint.Google Scholar
Hemenway, M.K. (1975). Astron. J. 80, 199.Google Scholar
Iben, I. and Tuggle, R.S. (1975). Astrophys. J. 197, 39.Google Scholar
Jones, D.H.P. (1973). Astrophys. J. Suppl. 25, 487.Google Scholar
King, D.S., Hansen, C.J., Ross, R.R. and Cox, J.P. (1975). Astrophys. J. 195, 467.Google Scholar
Kraft, R.P. (1960). Astrophys. J. 132, 404.Google Scholar
Kurucz, R.L. (1975). In Multicolor Photometry and The Theoretical HR Diagram, Philip, A.G.D. and Hayes, D.S., eds., Dudley Obs. Report 9, 271.Google Scholar
Lub, J. (1977a). , University of Leiden.Google Scholar
Lub, J. (1977b). Astron. Astrophys. Suppl. 29, 345.Google Scholar
Lub, J. and Pel, J.W. (1977). Astron. Astrophys. 54, 137.Google Scholar
Madore, B.F. (1976). Roy. Obs. Bull. 182, 151.Google Scholar
Pel, J.W. (1976). Astron. Astrophys. Suppl. 24, 413.Google Scholar
Pel, J.W. (1977). Astron. Astrophys. (in press).Google Scholar
Petersen, J.O. (1973). Astron. Astrophys. 27, 89.Google Scholar
Preston, G.W. (1959). Astrophys. J. 130, 507.Google Scholar
Sandage, A.R. and Tammann, G.A. (1971). Astrophys. J. 167, 293.Google Scholar
Stellingwerf, R.F. (1975a). Astrophys. J. 195, 441.Google Scholar
Stellingwerf, R.F. (1975b). Astrophys. J. 199, 705.CrossRefGoogle Scholar
Sturch, C. (1966). Astrophys. J. 143, 774.Google Scholar
Sweigart, A.V. and Gross, P.G. (1976). Astrophys. J. Suppl. 32, 367.CrossRefGoogle Scholar
Tuggle, R.S. and Iben, I. (1972). Astrophys. J. 178, 455.Google Scholar
Walraven, J.H., Tinbergen, J. and Walraven, Th. (1964). Bull. Astr. Inst. Neth. 17, 520.Google Scholar