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
MY VUL EA 14.9 – 16.0
NP VUL EA 14.3 – 15.5
NV VUL EA 13.5 – 15.5
QS VUL EA 5.15 – 5.25
RR VUL EA 10.0 – 11.4
RS VUL EA 6.79 – 7.8
SY VUL EA 13.0 – 16.0
V0399 VUL EA 7.01 – 7.1
V0400 VUL EA 6.76 – 6.8
V0456 VUL EA 12.14 – 12.8
V0472 VUL EA 14.5 – 16.6
V0487 VUL EA 10.76 – 10.76
V0491 VUL EA 9.94 – 10.3
V0495 VUL EA 9.76 – 10.1
V0499 VUL EA 11.19 – 11.6
V0500 VUL EA 12.44 – 13.0
V0502 VUL EA 10.39 – 11.0
V0512 VUL EA 12.2 – 13.0
VV VUL EA 12.0 – 13.9
WZ VUL EA 14.5 – 16.1