2008/02/27 by Z. Eker, O. Demircan, S. Bilir · 3 citations
Physics and Astronomy · #Angular momentum #Astro and Planetary Science #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Binary star #Classical mechanics #Contact binary #Eclipse #Physics #Sky #Stars #Stellar evolution #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.13155.x
3 pages, accepted for publication in MNRAS
arxiv created 2008/02/27 · openalex publication_date 2008/04/16 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Period histograms of eclipsing binaries generated with data from the All-Sky Automated Survey cannot be interpreted only using orbital evolution. Eclipse probabilities, selection effects and space distributions in the solar neighbourhood should be considered before any interpretations are made. Depending upon the physical dimensions (the total mass and the period) of the progenitor stars and the efficiency of the angular momentum loss mechanism, a newly formed W Ursa Majoris type binary can be at any age up to several Gyr. Also, the evolution in the contact stage is controlled not only by angular momentum and mass loss but also by mass transfer between the component stars. Thus, the mean life of the contact stages should be about 1.6 Gyr. A different time-scale would cause inconsistencies.