Observational studies of early-type binary stars: VV Orionis


E-mail: terrell@boulder.swri.edu (DT); ulisse.munari@oapd.inaf.it (UM); siviero@pd.astro.it (AS)


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 M1= 10.9 ± 0.1 M and a radius R1= 4.98 ± 0.02 R and a B4.5 V secondary with a mass M2= 4.09 ± 0.05 M and a radius R2= 2.41 ± 0.01 R.