Abstract
VV Orionis is a detached eclipsing binary system consisting of stars of spectral types B1 V and B4 V with a period of 1.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 earlytype 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.
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References
Al-Naimiy, H. M.: 1978,Astrophys. Space Sci. 53, 181.
Andersen, J.: 1976,Astron. Astrophys. 47, 467.
Atkins, H. L.: 1971, M.S. Thesis, University of Georgia.
Beltrami, G. and Galeotti, P.: 1970,Mem. Soc. Astron. Ital. 41, 167.
Bolokadze, R. D.: 1953,Perem. Zvezdy 9, 379.
Budding, E. and Najim, N. N.: 1980,Astrophys. Space Sci. 72, 369.
Cester, B., Fedel, B., Giuricin, G., Mardirossian, F., and Mazzetti, M.: 1978,Astron. Astrophys. Suppl. 33, 91.
Chambliss, C. R.: 1983,Astrophys. Space Sci. 89, 15.
Chambliss, C. R. and Leung, K. C.: 1982,Astrophys. J. Suppl. 49, 531.
Daniel, Z.: 1916,Publ. Allegheny Obs. 3, 179.
Duerbeck, H. W.: 1975,Astron. Astrophys. Suppl. 22, 19.
Duerbeck, H. W.: 1976,Astron. Astrophys. 47, 471.
Eaton, J. A.: 1975,Astrophys. J. 197, 379.
Giuricin, G. Mardirossian, F., Mazzetti, M., and Chambliss, C. R.: 1983,Astron. Astrophys. Suppl. 51, 111.
Grygar, J., Cooper, M. L., and Jurkevich, I.: 1972,Bull. Astron. Inst. Czech. 23, 147.
Huffer, C. M. and Kopal, Z.: 1951,Astrophys. J. 114, 297.
Irwin, J. B.: 1947,Astrophys. J. 106, 380.
Klinglesmith, D. A. and Sobieski, S.: 1970,Astron. J. 75, 175.
Koch, R. H., Sobieski, S., and Wood, F. B.: 1963,Publ. Univ. Penna. Astron. Ser. 9, 32.
Kopal, Z. and Shapley, M. B.: 1956,Jodrell Bank Ann. 1, 141.
Russell, H. N. and Merrill, J. E.: 1952,Contr. Princeton Univ. Obs., No. 26.
Wilson, R. E. and Devinney, E. J.: 1971,Astrophys. J. 166, 304.
Wood, F. B.: 1946,Contr. Princeton Univ. Obs. 21, 25.
Wood, D. B.: 1971,Astron. J. 76, 701.
Wood, D. B.: 1972, ‘A Computer Program for Modeling Non-Spherical Eclipsing Binary Star Systems’, NASA Publ. X 110 72 473.
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Chambliss, C.R. VV Orionis: A well-behaved early-type eclipsing binary system. Astrophys Space Sci 99, 163–170 (1984). https://doi.org/10.1007/BF00650241
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DOI: https://doi.org/10.1007/BF00650241