Close Binary Eclipsing Systems

Abstract

Within the GCVS you will find over 6000 eclipsing binary variable stars. The Algol-type eclipsing binary stars are the most numerous; however, over one thousand eclipsing stars have not been well studied and as a result have not been categorized within the three major groups (i.e. EA, EB, or EW). One thousand ill-defined eclipsing binaries, classified as “E:”, can certainly be described as a target-rich environment for any observer!

We adopt a triple system of classifying eclipsing binary systems: according to the shape of the combined light curve, as well as to physical and evolutionary characteristics of their components. The classification based on light curves is simple, traditional, and suits the observers; the second and third classification methods take into account positions of the binary-system components in the (Mv, B-V) diagram and the degree of inner Roche lobe filling. Estimates are made by applying the simple criteria proposed by Svechnikov and Istomin (1979).

GCVS