Hostname: page-component-848d4c4894-8kt4b Total loading time: 0 Render date: 2024-06-23T06:01:17.675Z Has data issue: false hasContentIssue false
  • English
  • Français

VV Orionis: A Well-Behaved Early-Type Eclipsing Binary System*

Published online by Cambridge University Press:  12 April 2016

Carlson R. Chambliss
Carlson R. Chambliss*
Affiliation:
Kutztown University, Kutztown, Pennsylvania, U.S.A.

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.

VV Orionis is a detached eclipsing binary system consisting of stars of spectral types BI V and B4 V with a period of l.d4854. There is also a third component whose orbital period about the eclipsing pair is about 120 days. In recent years there have been several new photoelectric and spectroscopic investigations of this system, and the results of these are compared. Both the geometric and photometric orbital elements appear to be well determined. VV Ori A appears to be of normal size and mass for its spectral class, but VV Ori B seems to be somewhat smaller than would be expected for a normal B4 V star. Linear limb-darkening coefficients are derived for VV Ori A, and these are in good agreement with theory. This system is of particular importance, because it is only one of very few early-type systems for which reliable limb-darkening coefficients can be expected to be obtained. The contribution of the light of the third component to the system has also been determined, and it appears most likely that VV Ori C is a star of spectral type A3 V.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 80: Double Stars, Physical Properties and Generic Relations , 1984 , pp. 163 - 170
Copyright
Copyright © Reidel 1984

Footnotes

*

Paper presented at the Lembang-Bamberg IAU Colloquium No. 80 on ‘Double Stars: Physical Properties and Generic Relations', held at Bandung, Indonesia, 3-7 June, 1983.

References

Al-Naimiy, H. M.: 1978, Astrophys. Space Sci. 53, 181.CrossRefGoogle Scholar
Andersen, J.: 1976, Astron. Astrophys. 47, 467.Google Scholar
Atkins, H. L.: 1971, M.S. Thesis, University of Georgia.Google Scholar
Beltrami, G. and Galeotti, P.: 1970, Mem. Soc. Astron. Ital. 41, 167.Google Scholar
Bolokadze, R. D.: 1953, Perem. Zvezdy 9, 379.Google Scholar
Budding, E. and Najim, N. N.: 1980, Astrophys. Space Sci. 72, 369.Google Scholar
Cester, B., Fedel, B., Giuricin, G., Mardirossian, F., and Mazzetti, M.: 1978, Astron. Astrophys. Suppl. 33, 91. Google Scholar
Chambliss, C. R.: 1983, Astrophys. Space Sci. 89, 15.Google Scholar
Chambliss, C. R. and Leung, K. C.: 1982, Astrophys. J. Suppl. 49, 531.CrossRefGoogle Scholar
Daniel, Z.: 1916, Pubi. Allegheny Obs. 3, 179.Google Scholar
Duerbeck, H. W.: 1975, Astron. Astrophys. Suppl. 22, 19.Google Scholar
Duerbeck, H. W.: 1976, Astron. Astrophys. 47, 471.Google Scholar
Eaton, J. A.: 1975, Astrophys. J. 197, 379.Google Scholar
Giuricin, G. Mardirossian, F., Mazzetti, M., and Chambliss, C. R.: 1983, Astron. Astrophys. Suppl. 51, 111.Google Scholar
Grygar, J., Cooper, M. L., and Jurkevich, I.: 1972, Bull. Astron. Inst. Czech. 23, 147.Google Scholar
Huffer, C. M. and Kopal, Z.: 1951, Astrophys. J. 114, 297.Google Scholar
Irwin, J. B.: 1947, Astrophys. J. 106, 380.CrossRefGoogle Scholar
Klinglesmith, D. A. and Sobieski, S.: 1970, Astron. J. 75, 175.CrossRefGoogle Scholar
Koch, R. H., Sobieski, S., and Wood, F. B.: 1963, Pubi. Univ. Penna. Astron. Ser. 9, 32.Google Scholar
Kopal, Z. and Shapley, M. B.: 1956, Jodrell Bank Ann. 1, 141.Google Scholar
Russell, H. N. and Merrill, J. E.: 1952, Contr. Princeton Univ. Obs., No. 26.Google Scholar
Wilson, R. E. and Devinney, E. J.: 1971, Astrophys. J. 166, 304.Google Scholar
Wood, F. B.: 1946, Contr. Princeton Univ. Obs. 21, 25.Google Scholar
Wood, D. B.: 1971, Astron. J. 76, 701.Google Scholar
Wood, D. B.: 1972, ‘A Computer Program for Modeling Non-Spherical Eclipsing Binary Star Systems', NASA Pubi. X 11072473.Google Scholar