Studies of multiple stellar systems — IV. The triple-lined spectroscopic system Gliese 644

• Published in: Monthly notices of the Royal Astronomical Society 2001-07, Vol.325 (1), p.343-357
• Main Authors: Mazeh, Tsevi, Latham, David W., Goldberg, Elad, Torres, Guillermo, Stefanik, Robert P., Henry, Todd J., Zucker, Shay, Gnat, Orly, Ofek, Eran O.
• Format: Article
• Language: English
• Subjects: binaries: spectroscopic; binaries: visual; stars: individual: Gliese 644; techniques: radial velocities
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1046/j.1365-8711.2001.04419.x

We present a radial velocity study of the triple-lined system Gliese 644 and derive spectroscopic elements for the inner and outer orbits with periods of 2.965 5 and 627 d. We also utilize old visual data, as well as modern speckle and adaptive optics observations, to derive a new astrometric solution for the outer orbit. These two orbits together allow us to derive masses for each of the three components in the system: MA = 0.410±0.028 (6.9 per cent), MBa = 0.336±0.016 (4.7 per cent), and MBb = 0.304±0.014 (4.7 per cent) M⊙. We suggest that the relative inclination of the two orbits is very small. Our individual masses and spectroscopic light ratios for the three M stars in the Gliese 644 system provide three points for the mass–luminosity relation near the bottom of the main sequence, where the relation is poorly determined. These three points agree well with theoretical models for solar metallicity and an age of 5 Gyr. Our radial velocities for Gliese 643 and vB 8, two common proper motion companions of Gliese 644, support the interpretation that all five M stars are moving together in a physically bound group. We discuss possible scenarios for the formation and evolution of this configuration, such as the formation of all five stars in a sequence of fragmentation events leading directly to the hierarchical configuration now observed, versus formation in a small N cluster with subsequent dynamical evolution into the present hierarchical configuration.