Hostname: page-component-586b7cd67f-dsjbd Total loading time: 0 Render date: 2024-11-29T21:42:07.552Z Has data issue: false hasContentIssue false
  • English
  • Français

An overtone Cepheid variable in an LMC eclipsing binary

Published online by Cambridge University Press:  12 April 2016

D. Lepischak  and
D.L. Welch
D. Lepischak
Affiliation:
Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M2, Canada
D.L. Welch
Affiliation:
Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M2, Canada

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.

Eclipsing binary systems potentially allow the direct and precise determination of the important properties of their component stars. An eclipsing binary containing a Cepheid variable which is also a double-lined spectroscopic binary would allow, for the first time, the direct measurement of the absolute luminosity and mass of the Cepheid. The MACHO Project LMC database contains five systems whose light curves show variations due to both eclipses and pulsation but only one has been clearly identified as an intermediate-mass, Population I object. This object, MACHO 81.8997.87 (= OGLELMC_SC16 119952) is a 2.035-d overtone Cepheid in an 800.4-d binary system with an M-type companion. Here we present the results of the analysis of the light curve of this system, the implications for its evolutionary history and discuss the prospects for future observations.

Type
Part 6. Binary stars and pulsation
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 372 - 376
Copyright
Copyright © Astronomical Society of the Pacific 2004

References

Alcock, C., et al. 2002, ApJ, 573, 338 Google Scholar
Allen, C.W. 1973 Astrophysical Quantities (London: Athlone)Google Scholar
Groenewegen, M.A.T. 2000, A&A, 363, 901 Google Scholar
Udalski, A., et al. 1999, Acta Astron., 49, 223 Google Scholar