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.[2]
The brightest rotating ellipsoidal variable is Spica (α Virginis).[3]
| Designation (name) | Constellation | Discovery | Apparent magnitude (Maximum) | Apparent magnitude (Minimum) | Range of magnitude | Spectral type | Comment |
|---|---|---|---|---|---|---|---|
| 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) | 0.97 | 1.04 | 0.07 | A2 V | Brightest member; binary |
| 68 Cygni (V1809 Cyg) | Cygnus | 4.98 | 5.09 | 0.11 | O7.5 IIIn((f)) | Hottest member; variability is disputable | |
| π Cassiopeiae | Cassiopeia | Paunzen & Maitzen (1998)[4] | 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)[2] | 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 |
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| Pulsating |
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| Eruptive |
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| Cataclysmic |
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| Rotating |
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| Eclipsing |
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