2007MNRAS.376.1671S

HR 6046 has long been known as a single-lined binary system, for which preliminary orbital solutions were given in the 1930s, but the nature of the secondary star in the system has to date appeared puzzling. The rather large masses which the component stars were once believed to possess caused much speculation that the secondary was a `collapsed star', and the large mass function that was originally published encouraged determined, but unsuccessful, efforts to be made to resolve the system by optical interferometry. We have observed the system as a double-lined binary, and now present the orbit. We are unable to specify the exact nature of the secondary star, whose mass is only slightly less than that of the primary, but comparison with late-type standard spectra suggests that it is an evolved star, while the primary is a giant somewhat cooler than the published spectral type indicates. The Hipparcos parallax is consistent with such a model for the system, but it is possible that it is vitiated by the photocentric motion. Our new orbital elements and their improved level of precision show conclusively that the system is by no means as exotic as was once thought.