Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-26T03:17:01.907Z Has data issue: false hasContentIssue false
  • English
  • Français

Fundamental Mode and First Overtone Mode Cepheids in the Small Magellanic Cloud

Published online by Cambridge University Press:  15 February 2018

H.A. Smith ,
N.A. Silbermann ,
S.R. Baird  and
J.A. Graham
H.A. Smith
Affiliation:
Dept. of Physics and Astronomy, Michigan State University, USA
N.A. Silbermann
Affiliation:
Dept. of Physics and Astronomy, Michigan State University, USA
S.R. Baird
Affiliation:
Dept. of Physics and Astronomy, Benedictine College and the University of Kansas, USA
J.A. Graham
Affiliation:
Dept. of Terrestrial Magnetism, Carnegie Institution of Washington, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We report results of a new photographic survey of variable stars in a 1 x 1.3 degree region near the Northeast Arm of the Small Magellanic Cloud. We have discovered 133 new variable stars in this field and have determined periods and B lightcurves for 78 new and 72 previously known variables. At periods shorter than about 3 days, the Cepheid period-luminosity relation splits into two sequences. The brighter sequence is believed to be populated by stars pulsating in the first overtone radial mode, wherecis the fainter sequence is populated by fundamental mode pulsators. The peak in the Cepheid period-frequency distribution occurs near a period of 1.8 days. The surface density of RR Lyrae stars in this field is comparable to that in an outlying SMC field near NGC 121.

Type
Windows on the Instability Strip
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 349 - 356
Copyright
Copyright © Cambridge University Press 1993

References

Arp, H., 1960, Astron. J, 65, 404.Google Scholar
Da Costa, G.S. & Mould, J.R., 1986, ApJ 305, 214.Google Scholar
Dessy, J.L., 1959, 71, 435.Google Scholar
Graham, J.A., 1975, PASP, 87, 641.Google Scholar
Graham, J.A., 1977, PASP 89, 425.Google Scholar
Harris, W.E., 1982, Ap.J. Suppl. 50, 573.Google Scholar
Hazen, M.L. & Nemec, J.M., 1992, Astron. J. 104, 111.Google Scholar
Nemec, J.M., 1989, IAU Colloq. No. III, The Use of Pulsating Stars in Fundamental Problems of Astronomy, ed. Schmidt, E.G., Cambridge University Press, Cambridge, p. 215.Google Scholar
Nemec, J.L., Wehlau, A., & Mendes de Oliveira, C. 1988, Astron. J. 96, 528.Google Scholar
Payne-Gaposchkin, C. & Gaposchkin, S. 1966, Smith. Contr. Ap. 9, 1.Google Scholar
Pickering, E.C., 1912, Harvard Coll. Obs. Circ. No. 173, 3.Google Scholar
Walker, A.R. 1991, IAU Symp. 148, The Magellanic Clouds, ed. Haynes, R. and Milne, D., Kluwer, Dordrecht, p. 307.Google Scholar
Wesselink, A.J., & Shuttleworth, M., 1965, MNRAS 130, 443.Google Scholar