VV Orionis: a well-behaved early-type eclipsing binary system

• Published in: Astrophysics and space science Vol. 99; no. 1-2; pp. 163 - 170
• Main Author: CHAMBLISS, C. R
• Format: Journal Article
• Language: English
• Published: Dordrecht Kluwer 01.02.1984
• Subjects: Astronomy; Binary and multiple stars; Earth, ocean, space; Eclipsing binaries; Exact sciences and technology; Stars; First type star; Orbital element; Photoelectric observation; Triple star; Spectroscopical observation; Eclipsing binary
• ISSN: 0004-640X; 1572-946X
• DOI: 10.1007/BF00650241

VV Orionis is a detached eclipsing binary system consisting of stars of spectral types B1 V and B4 V with a period of 1.4854 d. There is also a third component whose orbital period about the eclipsing pair is about 120 days. Recently, there have been several new photoelectric and spectroscopic investigations of this system, and the results of these are compared. 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 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.