Rotating ellipsoidal variables are a class of close binary variable star systems whose components are ellipsoidal. They are not eclipsing, but fluctuations in apparent magnitude occur due to changes in the amount of light emitting area visible to the observer. Typical brightness fluctuations do not exceed 0.1 magnitudes.
The brightest rotating ellipsoidal variable is Spica (α Virginis).
List of variables + List of Rotating ellipsoidal variablesDesignation (name)ConstellationDiscoveryApparent magnitude (Maximum)Apparent magnitude (Minimum)Range of magnitudeSpectral typeComment Spica (α Virginis) Virgo Ruban et al. (2006) 0.97 1.04 0.07 B1 III-IV + B2 V Brightest member; binary α Trianguli (Mothallah) Triangulum Ruban et al. (2006) 3.52 (Hp) 3.53 (Hp) 0.01 F5 III + M π5 Orionis Orion Ruban et al. (2006) 3.66 3.73 0.07 B2 III + B6 V b Persei Perseus Ruban et al. (2006) 4.52 4.68 0.07 A2 V 68 Cygni (V1809 Cyg) Cygnus 4.98 5.09 0.11 O7.5 IIIn((f)) Variability is disputable π Cassiopeiae Cassiopeia Paunzen & Maitzen (1998) 4.95 4.97 0.02 A5 V + A5 V 31 Crateris (TY Corvi) Corvus 5.19 5.23 0.04 B1.5 V Unknown companion 14 Cephei (LZ Cephei) Cepheus Morris (1985) 4.67 4.71 0.04 O9 III + O9.5 V HZ Canis Majoris Canis Major 5.28 5.34 0.06 A0 EuCrSr Long 6.4 year period;binary
References
External links OGLE Atlas of Variable Star Light Curves - Ellipsoidal variables