2008/05/30 by Slavek M. Rucinski, Theodor Pribulla · 52 citations
Physics and Astronomy · #Amplitude #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Binary number #Binary star #Contact binary #Globular cluster #Orbit (dynamics) #Orbital period #Period (music) #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.13508.x
published in Monthly Notices of the Royal Astronomical Society 388(4), 1831-1835 (Oxford University Press) · to appear in MNRAS
arxiv created 2008/05/30 · openalex publication_date 2008/07/06 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract Photometric and spectroscopic results for the contact binary GSC 01387–00475 (ASAS 083128+1953.1) are presented. The existence of this binary with the orbital period of P= 0.2178 d strengthens the argument that the cut-off of the period distribution for contact binaries – until now defined by CC Comae – is very sharp. The only case of a still shorter period is known in a globular cluster where more compact contact configurations are in fact expected. While the spectroscopic orbit of GSC 01387–00475 is well defined, the low orbital inclination of the binary and the presence of a spectroscopic companion contributing about 1/3 of the total light conspire to reduce the photometric variability to ≃0.09 mag. The photometric data are currently inadequate to identify the source of the small amplitude (0.02–0.03 mag) intrinsic variability of the system.