Beta Lyrae variable

As a Beta Lyrae Stars ( GCVS nomenclature code: EB), a group designated by eclipsing stars, whose light curve changes continuously and its main and secondary minima are at different depths. The continuous change in brightness is due to the small distance in the close binary system in which gravitational and centripetal forces deform the stars.

The classification according to the shape of the light curve has the disadvantage that it is not a classification on the basis of physical properties and in the case of Beta Lyrae stars also is a function of the measurement accuracy. Eclipsing binaries are preferably divided based on the geometry of the Roche limit in separate, semi- separated and contact systems. The Beta Lyrae stars may belong to all three types.

In EBs, there is a dependency between the age and the period of the railway circulation. According to this, in star clusters from the mean period of 2 days at the age of some 10 million years to less than 0.5 days at the age of 10 billion years. The cause is not known and the W Ursae Majoris contact systems do not show a corresponding development. The former Beta Lyrae star V1309 Sco has developed into a star merger at a light Strengthening the Red Nova and therefore seem to lose EBs torque.

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