W Virginis variable
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] The Type II Cepheids are now split into three sub-groups, with the W Virginis group being asymptotic giant branch stars which have temporarily increased in temperature due to a helium shell flash and crossed the instability strip. The prototype is W Virginis.[1]
See also
[edit]References
[edit]- 1 2 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.
- ↑ Strohmeier, W. (1972). Variable Stars. Oxford, New York: Pergamon Press. Bibcode:1972vast.book.....S.
- ↑ 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.
- ↑ Webb, Stephen (1999). Measuring the Universe: The Cosmological Distance Ladder. Springer.
External links
[edit]- AAVSO Variable Star of the Month. W Virginis: Spring 2003 PDF / HTML
- OGLE Atlas of Variable Star Light Curves - W Virginis stars
| Pulsating |
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| Eruptive |
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| Cataclysmic | |||||||||
| Rotating |
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| Eclipsing | |||||||||
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