2008/10/09 by Theodor Pribulla, Slavek M. Rucinski, Heide DeBond +8 · 47 citations
Physics and Astronomy · Social Sciences · #Amplitude #Astronomy and Astrophysical Research #Binary number #Binary star #Binary system #Contact binary #Educational Leadership and Practices #Orbital elements #Radial velocity #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1088/0004-6256/137/3/3646
published in The Astronomical Journal 137(3), 3646-3654 (Institute of Physics) · 5 figures, submitted to AJ
arxiv created 2008/10/09 · openalex publication_date 2009/02/25 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
Radial velocity (RV) measurements and sine curve fits to the orbital RV variations are presented for 10 close binary systems: TZ Boo, VW Boo, EL Boo, VZ CVn, GK Cep, RW Com, V2610 Oph, V1387 Ori, AU Ser, and FT UMa. Our spectroscopy revealed two quadruple systems, TZ Boo and V2610 Oph, while three stars showing small photometric amplitudes, EL Boo, V1387 Ori, and FT UMa, were found to be triple systems. GK Cep is a close binary with a faint third component. While most of the studied eclipsing systems are contact binaries, VZ CVn and GK Cep are detached or semidetached double-lined binaries, and EL Boo, V1387 Ori, and FT UMa are close binaries of uncertain binary type. The large fraction of triple and quadruple systems found in this sample supports the hypothesis of formation of close binaries in multiple stellar systems; it also demonstrates that low photometric amplitude binaries are a fertile ground for further discoveries of multiple systems.