description W Virginis Overview
W Virginis is the prototype of the W Virginis variables, a class of pulsating variable stars also known as Type II Cepheids. These stars are Population II objects, meaning they are older and more metal-poor than classical Cepheid variables. W Virginis stars follow a period-luminosity relationship distinct from classical Cepheids and are typically found in globular clusters and the galactic halo. They are less luminous than classical Cepheids at equivalent pulsation periods.
insights Ranking position
W Virginis ranks #64 of 212 in the Star ranking, behind Shaula, ahead of Gacrux.
help W Virginis FAQ
Why is W Virginis important in variable-star astronomy?
W Virginis is the prototype of the W Virginis subclass of Type II Cepheids. Its name therefore identifies a family of old, low-mass pulsating stars used in studies of stellar evolution and astronomical distances.
How long does W Virginis take to complete one brightness cycle?
Its principal pulsation period is about 17.3 days. Long-term observations also reveal modest cycle-to-cycle differences and additional pulsation behavior.
How is a W Virginis star different from a classical Cepheid?
W Virginis variables belong to the older Population II and are less luminous than classical Cepheids at the same pulsation period. Astronomers must use the correct period-luminosity relation or they will derive an incorrect distance.
Can W Virginis be seen with the naked eye?
No. The star varies roughly between ninth and eleventh magnitude in the constellation Virgo, placing it below naked-eye visibility. Amateur observers can monitor it with a telescope, a camera, and comparison-star charts.
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