W Virginis variable

Lightcurve of the W Virginis (Type II Cepheid) variable κ Pavonis recorded by NASA's Transiting Exoplanet Survey Satellite (TESS).

W Virginis variables are a subclass of Type II Cepheids which exhibit pulsation periods between 10–20 days,^[1] and are of spectral class F6 – K2.^[2][3]

They were first recognized as being distinct from classical Cepheids by Walter Baade in 1942, in a study of Cepheids in the Andromeda Galaxy that proposed that stars in that galaxy were of two populations.^[4]

See also

• Low-dimensional chaos in stellar pulsations

References

1. Wallerstein, G. (2002). "The Cepheids of Population II and Related Stars". Publications of the Astronomical Society of the Pacific. 114 (797): 689–699. Bibcode:2002PASP..114..689W. doi:10.1086/341698.
2. Strohmeier, W. (1972). Variable Stars. Oxford, New York: Pergamon Press. Bibcode:1972vast.book.....S.
3. Soszyński, I.; Udalski, A.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Wyrzykowski, Ł.; Szewczyk, O.; Ulaczyk, K.; Poleski, R. (2008). "The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. II.Type II Cepheids and Anomalous Cepheids in the Large Magellanic Cloud". Acta Astronomica. 58: 293. arXiv:0811.3636. Bibcode:2008AcA....58..293S.
4. Webb, Stephen (1999). Measuring the Universe: The Cosmological Distance Ladder. Springer.

External links

• AAVSO Variable Star of the Month. W Virginis: Spring 2003 PDF / HTML
• OGLE Atlas of Variable Star Light Curves - W Virginis stars