Observational studies of early-type binary stars: VV Orionis

New and previously published observations of the bright eclipsing binary VV Orionis are analyzed. We present new radial velocities and interstellar reddening measurements from high-resolution spectra of this detached, short-period (P= 1.48 d) binary. We discuss the validity of prior claims for the existence of a third body and show that our new velocities and light-curve solution cast doubt on them. The components of VV Ori are shown to be a B1 V primary with a mass M 1= 10.9 ± 0.1 M⊙ and a radius R 1= 4.98 ± 0.02 R⊙ and a B4.5 V secondary with a mass M 2= 4.09 ± 0.05 M⊙ and a radius R 2= 2.41 ± 0.01 R⊙.