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Period Changes in the SX Phoenicis Star CY Aquarii

Published online by Cambridge University Press:  15 February 2018

Michael D. Joner  and
John M. Powell
Michael D. Joner
Affiliation:
Brigham Young University, Provo, Utah, U.S.A.
John M. Powell
Affiliation:
Brigham Young University, Provo, Utah, U.S.A.

Abstract

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CY Aquarii is a Population II dwarf Cepheid that has been observed on a regular basis since 1930. We present evidence from unpublished times of maximum light from Brigham Young University observations secured in the mid-1970s to the present that indicate that the period of CY Aqr has changed in a discontinuous manner. Furthermore, we find that the period has changed significantly since the epoch of the last published investigation (1988). Finally, contrary to some past claims, examination of our high time resolution light curves yields no indication of multi-periodic pulsation in CY Aqr.

Type
Windows on the Instability Strip
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 428
Copyright
Copyright © Cambridge University Press 1993

References

Coates, D.W., Barnes, T.G., Fernley, J.A., Frueh, M.L. & Sekiguchi, K., 1991, Delta Scuti Star Newsletter 4, 10Google Scholar
Kamper, B., 1985, IBVS, 2802Google Scholar
Percy, J.R., 1975, Astron. Astrophys. 43, 469 Google Scholar
Rolland, A., Peña, J.H., de Coca, Lopez, Peniche, R. & Gonzalez, S.F., 1986, Astron. Astrophys. 168, 125 Google Scholar