Abstract
The observations of VV Ori inUBV and inuvby obtained by Chambliss in 1975–79 have been re-analyzed with the use of an updated version of the WINK program of Wood. Several solutions were obtained using the normal points (ca. 80 per light curve). These establish fairly reliable values for the linear limb-darkening coefficient of VV Ori A and approximate values for the luminosity of the third component of this system. Attempts to determine non-linear coefficients of limb darkening for the primary component, however, proved to be unsuccessful. Solutions were also obtained using all observations (ca. 620 per light curve). Very close agreement was found between the values of the geometric elements determined from these solutions and those determined by use of the normal points only. The solutions based on all observations produced reliable values foru 1, the limb darkening coefficient of VV Ori A, (typically, 0.30±-0.04). These results are in good agreement with theoretical limb darkening coefficients derived from model atmospheres calculations. The contribution of VV Ori C to the light of the system was also ascertained, and it was found that this could be best interpreted, if this component has a spectral type of A3V. The other orbital elements of VV Ori were also discussed, and the differences between the various solutions were noted. Since VV Ori A is one of the very few early-type stars for which reliable limb-darkening coefficients can be empirically determined, this system is viewed as being of considerable importance.
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References
Al-Naimiy, H. A.: 1978,Astrophys. Space Sci. 53, 181.
Andersen, J.: 1976,Astron. Astrophys. 47, 467.
Beltrami, G. and Galeotti, P.: 1970,Mem. Soc. Astron. Italy 41, 167.
Budding, E. and Najim, N. N.: 1980,Astrophys. Space Sci. 72, 369.
Carbon, D. F. and Gingerich, O.: 1969, inTheory and Observations of Normal Stellar Atmospheres, MIT Press, p. 377.
Chambliss, C. R. and Leung, K. C.: 1982,Astrophys. J., Suppl. 49, 531.
Cester, B., Fedel, B., Giuricin, G., and Mazzetti, M.: 1978:Astron. Astrophys. Suppl. 33, 91.
Crawford, D. L. and Barnes, J. V.: 1970,Astron. J. 75, 978.
Daniel, Z.: 1916,Publ. Allegheny Obs. 3, 179.
Duerbeck, H. W.: 1975,Publ. Allegheny. Suppl. 22, 19.
Duerbeck H. W.: 1976,Astron. Astrophys. 47, 471.
Eaton, J. A.: 1975,Astrophys. J. 197, 379.
Fitz Gerald, M. P.: 1970,Astron. Astrophys. 4, 234.
Flower, P. J.: 1977,Astron. Astrophys. 54, 31.
Giuricin, G., Mardirossian, F., Mazzetti, M., and Chambliss, C. R.: 1982,Astron. Astrophys. Suppl., in press.
Grygar, J., Cooper, M. L., and Jurkevich, I.: 1972,Bull. Astron. Inst. Czech. 23, 147.
Heintze, J. R. W. and Grygar, J.: 1970,Bull. Astron. Inst. Czech.,21, 77.
Hosokawa, Y.: 1957,Sci. Rep. Tohoku Univ. Ser. I 40, 208.
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.: 1949,Harvard Obs. Circ., No. 454.
Kopal, Z.: 1959,Close Binary Systems, Chapman and Hall Ltd., London.
Kopal, Z. and Shapley, M. B.: 1956,Jodrell Bank Annals 1, 141.
Kurucz, R. L.: 1979,Astrophys. J. Suppl. 40, 1.
Merrill, J. E.: 1950,Contrib. Princeton Univ. Obs., No. 23.
Morton, D. C. and Adams, T. F.: 1968,Astrophys J. 151, 611.
Münch, G. and Chandrasekhar, S.: 1949,Harvard Obs. Circular, No. 453.
Popper, D. M.: 1980,Ann. Rev. Astron. Astrophys. 18, 115.
Popper, D. M.: 1981,Astrophys. J. Suppl. 47, 339.
Russell, H. N. and Merrill, J. E.: 1952,contrib. Princeton Univ. Obs., No. 26.
Russell, H. N. and Shapley, H.: 1912,Astrophys. J. 36, 239, 285.
Schul'berg, A. M.: 1973,Soviet Astron. 17, 622.
Twigg, L. W. and Rafert, J. B.: 1980,Monthly Notices Roy. Astron. Soc. 193, 775.
Wesselink, A. J.: 1941,Leiden Ann. 17, No. 3.
Wilson, R. E. and Devinney, E. J.: 1971,Astrophys. J. 166 304.
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, Greenbelt, Maryland, U.S.A.
Wood, D. B.: 1978, private communication.
Wood, D. B. and Etzel, P. B.: 1982, private communication.
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Visiting Astronomer, Kitt Peak National Observatory, which is operated by AURA Inc., under contract with the National Science Foundation
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Chambliss, C.R. A re-analysis of the eclipsing binary system VV Orionis. Astrophys Space Sci 89, 15–32 (1983). https://doi.org/10.1007/BF01008382
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DOI: https://doi.org/10.1007/BF01008382