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Fourier analysis of Beat Cepheids

Published online by Cambridge University Press:  25 April 2016

D. J. Faulkner*
Affiliation:
Mount Stromlo and Siding Spring Observatory, Australian National University

Extract

The double-mode or beat Cepheids form a group of some 10 variables at the short period end of the classical Cepheid period range, which exhibit two (or three) simultaneous pulsations with remarkably constant period ratio (see Table I). If, as seems likely, the two periods (P0 and P1,) are to be identified with fundamental and first-overtone radial oscillations, linear pulsation theory may be used to yield a mass and a radius estimate for each beat Cepheid (Mbear and Rbeat) based on period observations alone. The masses so obtained may be compared with two other Cepheid mass estimates: the pulsation mass, Mpuls, is derived by the application of pulsation theory to one observed stellar period (usually P0) and a radius calculated from the stellar luminosity and temperature; the evolutionary mass, Mevol, is inferred from the stellar luminosity by the application of stellar evolution results (without mass loss) for Population I stars in the core helium-burning phase. If a Cepheid is a member of a cluster or association whose distance and reddening have been determined, the Cepheid luminosity and temperature may be obtained observationally, yielding Mpuls, and Mevol estimates directly. For other Cepheids, only indirect estimates may be made, based on the period-luminosity-colour relationship calibrated using the Cepheids with cluster membership.

Type
Contributions
Copyright
Copyright © Astronomical Society of Australia 1977

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References

Cogan, B.C., private communication (1977).Google Scholar
Cox, A. N., King, D. S.,Hodson, S. W., and Henden, A. A., Astrophys. J., 212, 451 (1977).CrossRefGoogle Scholar
Cox, J. P., King, D. S., and Stellingwerf, R. F., Astrophys. J., 171, 93 (1972).CrossRefGoogle Scholar
Efremov, Yu. N., and Kholopov, P. N., Inf. Bull, Var. Stars, No. 1073 (1975a).Google Scholar
Efremov, Yu. N., and Kholopov, P. N., Perem. Zvezdy, 20, 133 (1975b).Google Scholar
Faulkner, D. J., Astrophys. J., in press (1977a).Google Scholar
Faulkner, D. J., Astrophys. J., in press (1977b).Google Scholar
Fitch, W. S., and Szeidl, B., Astrophys. J., 203, 616 (1976).Google Scholar
Gordon, K. C, and Kron, G. E., Astrophys. J., 106, 318, (1974).Google Scholar
Hanson, R. B., Astron. J., 80, 379 (1975).CrossRefGoogle Scholar
Iben, I. Jr., and Tuggle, R. S., Astrophys. J., 173, 135 (1972).Google Scholar
Irwin, J. B., Astrophys. J. Suppl., 6, 253 (1961).Google Scholar
Jansen, A. G., Bull. Astron. Inst. Netherlands, 16, 141 (1962).Google Scholar
Jerzykiewicz, M., and Wenzel, W., Acta Astron., 27, 35 (1977).Google Scholar
Kholopov, P. N., and Efremov, Yu. N., Astron. Tsirk., No. 437, 5 (1967).Google Scholar
King, D. S., Cox, J. P., Eilers, D. D., and Davey, W. R., Astrophys. J., 182 859 (1973).Google Scholar
King, D. S., Hansen, C. J., Ross, R. R., and Cox, J. P., Astrophys, J., 195, 467 (1975).Google Scholar
Kobayashi, E., Saio, H., and Takeuti, M., Sci. Rep. Tohoku Univ., 59 67 (1976).Google Scholar
Landau, L. D., and Lifshitz, E. M., Mechanics (Oxford: Pergamon Press), (1976).Google Scholar
Leotta-Janin, C., Bull. Astron. Inst. Netherlands, 19, 169 (1967).Google Scholar
Madore, B. F., and van den Bergh, S., Astrophys. J., 197, 55 (1975).Google Scholar
Mitchell, R. I., Iriarte, B., Steinmetz, D., and Johnson, H. L., Bol Tonantzintla y Tacubaya, 3, 153 (1964).Google Scholar
Oosterhoff, P. Th., Bull. Astron. Inst. Netherlands, 13, 317 (1957a).Google Scholar
Oosterhoff, P. Th., Bull. Astron. Inst. Netherlands, 13, 320 (1957b).Google Scholar
Oosterhoff, P. Th., Bull. Astron. Inst. Netherlands, 15, 199 (1960).Google Scholar
Oosterhoff, P. Th., Bull. Astron. Inst. Netherlands, 17, 448 (1964).Google Scholar
Pel, J. W., Astron. Astrophys. Suppl., 24, 413 (1976).Google Scholar
Preston, G. W., Astrophys. J., 130, 507 (1959).Google Scholar
Roslund, C., and Pretorius, W., Ark. f. Astron., 3, 201 (1963).Google Scholar
Stellingwerf, R. F., Astrophys, J., 199, 705 (1975).Google Scholar
Stobie, R. S., Observatory, 90, 20 (1970).Google Scholar
Stocie, R. S., Mon. Not. R. Astron. Soc, 157, 167 (1972).Google Scholar
Stobie, R. S., Inf. Bull. Var. Stars, No. 1209 (1976).Google Scholar
Stobie, R. S., preprint (1977).Google Scholar
Stobie, R. S., and Hawarden, T., Mon. Not. R. Astron. Soc, 157, 157 (1972).Google Scholar
Szabados, L., IAU Colloquium No. 29, in press (1976).Google Scholar
Tammann, G. A., Astron. Astrophys., 3, 308 (1969).Google Scholar
The, P.-S., and Roslund, C., Contr. Bosscha Obs., No. 19 (1963).Google Scholar
Walraven, Th., Muller, A. B., and Oosterhoff, P. Th., Bull. Astron. Inst. Netherlands, 14, 81 (1958).Google Scholar
Weaver, H., Steinmetz, D., and Mitchell, R., Lowell Obs. Bull, 5, 30 (1960).Google Scholar
Wenzel, W., Mitt. Ver. Sterne, 4, 25 (1966).Google Scholar
Wenzel, W., IAU Colloquium No. 29, in press (1976).Google Scholar
Worley, C. E., and Eggen, O. J., Astron. J., 62, 104 (1957).Google Scholar
Zajceva, G. V., Astron. Tsirk., No. 502, 7 (1969).Google Scholar