Type of variability: EA

Algol (Beta Persei)-type eclipsing systems.

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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

33

stars

0

observed in last month


Name Type Brightness
EPS AUR EA 2.92 – 3.8
WW AUR EA 5.86 – 6.5
ZET AUR EA 3.7 – 3.9
ZZ BOO EA 6.79 – 7.4
V0470 CAM EA 14.1 – 14.7
RZ CAS EA 6.18 – 7.7
TV CAS EA 7.22 – 8.2
EK CEP EA 7.99 – 9.3
U CEP EA 6.75 – 9.2
VV CEP EA 4.8 – 5.3
R CMA EA 5.7 – 6.3
U CRB EA 7.66 – 8.7
MY CYG EA 8.3 – 9.0
Y CYG EA 7.3 – 7.9
W DEL EA 9.69 – 12.3
AI DRA EA 7.05 – 8.0
S EQU EA 8.0 – 10.0
TX HER EA 8.54 – 9.3
KW HYA EA 6.11 – 6.5
AR LAC EA 6.08 – 6.7