2006/11/30 by Theodor Pribulla, Slavek M. Rucinski, George Conidis +5 · 68 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Binary number #Binary star #Binary system #Contact binary #Orbital elements #Radial velocity #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/512772
published in The Astronomical Journal 133(5), 1977-1987 (Institute of Physics) · submitted to AJ, revised version Jan 7, 2007, 6 figures, 4 tables
arxiv created 2007/01/07 · openalex publication_date 2007/03/23 · arxiv updated 2009/12/01 · openalex created_date 2019/06/27 · openalex updated_date 2026/08/05
Radial velocity measurements and sine-curve fits to the orbital radial velocity variations are presented for 10 close binary systems: OO Aql, CC Com, V345 Gem, XY Leo, AM Leo, V1010 Oph, V2612 Oph, XX Sex, W UMa, and XY UMa. Most of these binaries have been observed spectroscopically before, but our data are of higher quality and consistency than in the previous studies. While most of the studied eclipsing pairs are contact binaries, V1010 Oph is probably a detached or semidetached double-lined binary, and XY UMa is a detached, chromospherically active system whose broadening functions clearly show well-defined and localized dark spots on the primary component. A particularly interesting case is XY Leo, which is a member of visually unresolved quadruple system composed of a contact binary and a detached, noneclipsing, active binary with an 0.805 day orbital period. V345 Gem and AM Leo are known members of visual binaries. We found faint visual companions at about 2''-3'' from XX Sex and XY UMa.