Formation and Evolution of W UMa Stars: Fallacies and Corrections

Details Formation and Evolution of W UMa Stars: Fallacies and Corrections Formation and Evolution of W UMa Stars: Fallacies and Corrections

2008-02-27

arxiv.org/abs/0802.3995v1

Astronomy and Astrophysics

Astrophysics

3 pages, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2008.13155.x

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.

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