Rotating ellipsoidal variables are a class of closebinaryvariable star systems whose components areellipsoidal. They are not eclipsing, but fluctuations inapparent 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 isSpica (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) | 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] | 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 |
| Pulsating |
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|---|---|---|---|---|---|---|---|---|---|
| Eruptive |
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| Cataclysmic | |||||||||
| Rotating |
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| Eclipsing | |||||||||
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