Formation and Evolution of W UMa Stars: Fallacies and Corrections
arXiv:0802.3995 · doi:10.1111/j.1365-2966.2008.13155.x
Abstract
The period histograms of eclipsing binaries generated with ASAS data cannot only be interpreted by orbital evolution. The eclipse probabilities, selection effects and space distributions in the solar neighborhood should be considered before any interpretations are made. Depending upon physical dimensions (total mass and period) of the progenitor stars and the efficiency of angular momentum loss (AML) mechanism, a newly formed W UMa type binary can be at any age up to several Gyr, and 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, mean life of contact stages should be about 1.6 Gyr. A different time scale would cause inconsistencies.
3 pages, accepted for publication in MNRAS
References in corpus (5)
- Eclipsing binaries in ASAS catalog
- Dynamical evolution of active detached binaries on log Jo - log M diagram and contact binary formation
- Kinematics of W UMa-type binaries and evidences on the two types of formation
- Kinematics of the chromospherically active binaries and evidence of an orbital period decrease in binary evolution
- Mass loss and orbital period decrease in detached chromospherically active binaries
Cited by in corpus (9)
- Fast radio bursts may originate from nearby flaring stars
- A catalog of chromospherically active binary stars (third edition)
- Physical Properties and Evolutionary States of EA-type Eclipsing Binaries Observed by LAMOST
- Origin of W UMa-type contact binaries - age and orbital evolution
- Fast radio bursts: the observational case for a Galactic origin
- The detached-binary channel for the formation of contact binaries
- Observations and light curve solutions of ultrashort-period eclipsing binaries
- Photometric observations and light curve solutions of the W UMa stars NSVS 2244206, NSVS 908513, CSS J004004.7+385531 and VSX J062624.4+570907
- Photometric analysis and evolutionary stages of the contact binary V2790 Ori