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]

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

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