A procedure for the automatic classification of eclipsing binaries is presented. The procedure is based on the data from 1029 classified systems and allows for the classification of a given system based on a set of observational parameters, even if the set is incomplete. The procedure is applied to six large surveys of eclipsing variables. About 5300 systems were classified for the first time and can be used for the determination of the astrophysical parameters of their components.
We have developed a procedure for the classification of eclipsing binaries from their light-curve parameters and spectral type. The procedure was tested on more than 1000 systems with known classification, and its efficiency was estimated for every evolutionary status we use. The procedure was applied to about 4700 binaries with no classification, and the vast majority of them was classified successfully. Systems of relatively rare evolutionary classes were detected in that process, as well as systems with unusual and/or contradictory parameters. Also, for 50 previously unclassified cluster binaries evolutionary classes were identified. These stars can serve as tracers for age and distance estimation of their parent stellar systems. The procedure proved itself as fast, flexible and effective enough to be applied to large ground based and space born surveys, containing tens of thousands of eclipsing binaries.
Abstract. We present the results of Monte Carlo simulation aiming to estimate the frequency of semi-detached Algol-type binaries among the stars observed as single. When an account is taken of various detection biases (mostly due to inclination of orbits), the fraction of Algols among the Galactic disk stars appears to be 0.1-0.2%. However, this number should be regarded as a lower limit only, since there are still unaccounted-for selection effects and other types of photometrically unresolved binaries. Hidden binarity appears to be an important phenomenon that should be taken into account when considering stellar statistics and constructing the fundamental relations between stellar parameters.
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