The Astrometric-Spectroscopic Binary System HIP 50796: An Overmassive Companion

Abstract

We report spectroscopic observations of the star HIP 50796, previously considered (but later rejected) as a candidate member of the TW Hya association. Our measurements reveal it to be a single-lined binary with an orbital period of 570 days and an eccentricity of e = 0.61. The astrometric signature of this orbit was previously detected by the HIPPARCOS satellite in the form of curvature in the proper motion components, although the period was unknown at the time. By combining our radial velocity measurements with the HIPPARCOS intermediate data (abscissae residuals) we are able to derive the full three-dimensional orbit, and determine the dynamical mass of the unseen companion as well as a revised trigonometric parallax that accounts for the orbital motion. Given our primary mass estimate of 0.73 solar masses (mid-K dwarf), the companion mass is determined to be 0.89 solar masses, or about 20% larger than the primary. The likely explanation for the larger mass without any apparent contribution to the light is that the companion is itself a closer binary composed of M dwarfs. The near-infrared excess and X-ray emission displayed by HIP 50796 support this. Our photometric modeling of the excess leads to a lower limit to the mass ratio of the close binary of about q = 0.8, and individual masses of 0.44-0.48 solar masses and 0.41-0.44 solar masses. The new parallax (20.6 +/- 1.9 mas) is significantly smaller than the original HIPPARCOS value, and more precise.