Hostname: page-component-7bb8b95d7b-2h6rp Total loading time: 0 Render date: 2024-09-18T02:48:08.938Z Has data issue: false hasContentIssue false
  • English
  • Français

Absolute Dimensions and Distance Modulus for HV 2226 in the SMC

Published online by Cambridge University Press:  07 August 2017

S.A. Bell ,
G. Hill ,
R.W. Hilditch ,
J.V. Clausen ,
A.P. Reynolds  and
A. Giménez
S.A. Bell
Affiliation:
Department of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY169SS, Scotland
G. Hill
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 West Saanich Road, R.R. No. 5, Victoria, B. C., Canada, V8×4M6
R.W. Hilditch
Affiliation:
Department of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY169SS, Scotland
J.V. Clausen
Affiliation:
Copenhagen University Observatory, Brorfeldevej 23, DK-4340, Tølløse, Denmark
A.P. Reynolds
Affiliation:
Department of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY169SS, Scotland
A. Giménez
Affiliation:
Laboratorio de Astrofísica Espacial y Física Fundamental, Instituto Nacional de Técnica Aerospacial, Apdo. 50727-28080 Madrid, Spain

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.

Absolute dimensions and the distance modulus have been established for the early-type eclipsing binary HV 2226 in the SMC. Analyses of the new radial velocities reported here, and CCD light curves published by Jensen et al. (1988) yield component masses of 9.3 ± 0.7 and 5.6 ± 0.5 M⊙, respectively. The radii are 5.6 ± 0.2 and 5.3 ± 0.2 R⊙ with the secondary component filling its Roche lobe which implies that HV 2226 must have evolved through a case A mass-transfer process. A distance modulus of (mv – Mv)0 = 18m.6 ± 0m.3 is derived, marginally lower than the adopted mean of 18m.9 for the SMC. The position of HV 2226, however, indicates that it is in fact situated in the near side of the SMC. In the present case, the accuracy of this estimate is limited mainly by the uncertainties of ≈ 2000 K in the effective temperatures. We point out that distance moduli with uncertainties of ± 0m.15 can be achieved from accurate radial velocities, light curves and colour indices of eclipsing binaries; such systems in the SMC and LMC are therefore promising distance indicators and work on further selected candidates is in progress.

Keywords

starsSMCbinaries: spectroscopicbinaries: eclipsingstars: masses ofstars: luminosities of
Type
Oral and Contributed Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 501 - 504
Copyright
Copyright © Kluwer 1992 

References

Balona, L. & Crampton, D.: 1974, Mon. Not. R. astr. Soc. 166, 203 CrossRefGoogle Scholar
Bell, S.A., Hill, G., Hilditch, R.W., Clausen, J.V., Reynolds, A.P. & Giménez, A.: 1991, Mon. Not. R. astr. Soc. 250, 119 Google Scholar
Böhm-Vitense, E.: 1981, Ann. Rev. Astr. Astrophys. 19, 295 CrossRefGoogle Scholar
Caldwell, J.A.R. & Coulson, I.M.: 1986, Mon. Not. R. astr. Soc. 218, 213 CrossRefGoogle Scholar
Claret, A. & Giménez, A.: 1989, Astr. Astrophys. Suppl. Ser. 81, 1 Google Scholar
Hill, G.: 1979, Publs. Dom. astrophys. Obs. 15, 297 Google Scholar
Hill, G.: 1982, Publs. Dom. astrophys. Obs. 16, 59 Google Scholar
Hill, G., Fisher, W.A. & Poeckert, R.: 1982, Publs. Dom. astrophys. Obs. 16, 43 Google Scholar
Hill, G. & Fisher, W.A.: 1986, Publs. Dom. astrophys. Obs. 16, 159 Google Scholar
Jensen, K.S., Clausen, J.V. & Giménez, A.: 1988, Astr. Astrophys. Suppl. Ser. 74, 331 Google Scholar
Norris, J.: 1971, Astrophys. J. Suppl. Ser. 23, 1934 Google Scholar
Popper, D.M.: 1980, Ann. Rev. Astr. Astrophys. 18, 115 CrossRefGoogle Scholar
Westerlund, B.F.: 1990, Astr. Astrophys. Rev. 2, 29 Google Scholar
Wilson, R.E.: 1979, Astrophys. J. 234, 1054 Google Scholar
Wilson, R.E. & Devinney, E.J.: 1971, Astrophys. J. 166, 605 Google Scholar