Multicolor photometry of the eclipsing binary system VV Orionis

Details Multicolor photometry of the eclipsing binary system VV Orionis Multicolor photometry of the eclipsing binary system VV Orionis

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apjs...49..531c&link_type=abstract

Astrophysical Journal Supplement Series, vol. 49, Aug. 1982, p. 531-544. Research supported by the Kutztown State College, Amer

Astronomy and Astrophysics

Astrophysics

13

B Stars, Eclipsing Binary Stars, Stellar Color, Stellar Spectrophotometry, Ubv Spectra, Astrometry, Astronomical Catalogs, Ephemerides, Light Curve, Orbital Elements, Periodic Variations, Spectrum Analysis, Stellar Spectra

Scientific paper

VV Orionis is an eclipsing binary consisting of two B-type components with a period of 1.485378 day. Over 4200 observations of this system were obtained in UBV and uvby during the 1975-1979 seasons. All seven light curves were analyzed simultaneously using the Wilson-Devinney method. The contribution of light from the much fainter third component of the system was taken into consideration, but it was found that this star had a negligible effect on the light curves of the eclipsing pair. Consistent solutions were found, but the residuals for both of the ultraviolet light curves proved to be fairly large. Thus, VV Ori appears to be somewhat more complicated than might be expected for a detached system of this type. The larger component appears to be normal for a star of spectral type B1 V and is found to lie fairly close to the ZAMS. The secondary component, however, appears to be unusually small for its mass.

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