Rotating ellipsoidal variable

A light curve for Spica, adapted from Tkachenko *et al.* (2016)^[1]

Rotating ellipsoidal variables are a class of variable star. They are close binary 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).

References

Morris, S.L. "The Ellipsoidal Variable Stars", ApJ 295: 143–152, 1985 August 1

Samus N.N., Durlevich O.V., et al. Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.)

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^ Tkachenko, A.; et al. (May 2016), "Stellar modelling of Spica, a high-mass spectroscopic binary with a β Cep variable primary component", Monthly Notices of the Royal Astronomical Society, 458 (2): 1964–1976, arXiv:1601.08069, Bibcode:2016MNRAS.458.1964T, doi:10.1093/mnras/stw255, S2CID 26945389{{citation}}: CS1 maint: unflagged free DOI (link)

[Tkachenko2016-1] Tkachenko, A.; et al. (May 2016), "Stellar modelling of Spica, a high-mass spectroscopic binary with a β Cep variable primary component", Monthly Notices of the Royal Astronomical Society, 458 (2): 1964–1976, arXiv:1601.08069, Bibcode:2016MNRAS.458.1964T, doi:10.1093/mnras/stw255, S2CID 26945389{{citation}}: CS1 maint: unflagged free DOI (link)

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