Cepheid variable

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A Cepheid variable is a member of a particular class of variable stars, notable for a fairly tight correlation between their period of variability and absolute stellar luminosity.

Because of this correlation (discovered by Henrietta Swan Leavitt in 1912), Cepheid variables can be used as a standard candle to determine the distance to their host globular clusters or galaxies. Since the period-luminosity relation can be calibrated with great precision using the nearest Cepheid stars, the distances found with this method are among the most accurate available.

Description

A Cepheid is usually a population I giant yellow star, pulsing regularly by expanding and contracting, resulting in a regular oscillation of its luminosity. The luminosity of cepheid stars range from 103 to 104 times that of the Sun.

Use as a "Standard Candle"

The relationship between a Cepheid variable's luminosity and variability period is quite precise, and has been used a standard candle for more than a century. A three-day period Cepheid has a luminosity of about 800 times the Sun. A thirty-day period Cepheid is 10,000 times as bright as the Sun. The scale has been calibrated using nearby Cepheid stars, for which the distance was already known. This high luminosity, and the precision with which their distance can be estimated, makes Cepheid stars the ideal standard candle to measure the distance of globular clusters and external galaxies. Of course, a small error will be present because we do not know the precise location of the Cepheid variable within the cluster or galaxy. This error is typically small enough to be irrelevant in these kinds of measurements. Cepheid stars are visible from great distances. Edwin Hubble first identified some Cepheids in the Andromeda galaxy, thus proving its extragalactic nature (not known at that time). More recently, the Hubble Space Telescope succeeded in identifying some Cepheid stars in the Virgo cluster, at a distance of 60 million light years.

Notes

Missing image
HRDiagram_InsStrip.png
Hertzsprung-Russell diagram adapted from Powell. (http://anzwers.org/free/universe/hr.html) The instability strip is shown and contains the Cepheid variable region (in red) and the RR Lyrae region (in blue).


  • Some Cepheid stars (for example Polaris), have shown a decrease in their oscillation over a period of few tens of years, and now are virtually constant.
  • Cepheid stars are sometimes divided into two types, type I Cepheid and type II Cepheid. The latter type, composed of Population II stars, are now usually called W Virginis variables, and show a similar behaviour.

See also: RR Lyrae variable, Hubble Constantca:Cefeida de:Cepheiden fr:Cphide io:Cepheid-varianti it:Variabile Cefeide nl:Cephede ja:セファイド変光星 pl:Cefeida ru:Цефеида

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