Type of variability: EA

Algol (Beta Persei)-type eclipsing systems.

Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes.

General Catalog of Variable Stars

4842

stars

0

observed in last month


Name Type Brightness
V0662 AND EA 10.65 – 11.0
V0665 AND EA 12.7 – 13.3
V0674 AND EA 10.65 – 10.9
V0683 AND EA 10.45 – 10.9
V0706 AND EA 11.8 – 13.0
V0707 AND EA 9.93 – 10.4
V0714 AND EA 12.0 – 12.4
WW AND EA 10.92 – 11.52
WX AND EA 12.1 – 13.8
XZ AND EA 9.91 – 12.4
BV ANT EA 11.52 – 12.2
BY ANT EA 9.21 – 9.2
CC ANT EA 7.68 – 7.8
CD ANT EA 10.33 – 10.6
CF ANT EA 10.12 – 10.4
UU ANT EA 11.94 – 12.4
VV ANT EA 12.6 – 13.6
WX ANT EA 11.25 – 12.9
XX ANT EA 8.6 – 9.2
XY ANT EA 9.95 – 10.6