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
XZ ANT EA 9.65 – 10.7
YZ ANT EA 10.48 – 11.5
Y ANT EA 10.04 – 10.9
AL APS EA 12.7 – 13.4
BH APS EA 10.8 – 13.4
CD APS EA 11.3 – 11.8
CR APS EA 13.4 – 14.4
CY APS EA 12.9 – 14.2
DU APS EA 11.3 – 12.0
DW APS EA 7.9 – 9.1
EF APS EA 12.3 – 13.3
FF APS EA 14.5 – 15.5
FN APS EA 11.0 – 12.4
FZ APS EA 12.5 – 13.2
IO APS EA 12.3 – 13.3
KN APS EA 13.4 – 14.0
OT APS EA 7.98 – 8.3
OZ APS EA 8.59 – 8.6
PP APS EA 9.65 – 10.0
PT APS EA 12.19 – 13.3