Cepheid variable


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Cepheid variable

(ˈsiːfɪɪd)
n
(Astronomy) astronomy any of a class of variable stars with regular cycles of variations in luminosity (most ranging from three to fifty days). There is a relationship between the periods of variation and the absolute magnitudes, which is used for measuring the distance of such stars

Ce′pheid var`iable


n.
a variable star with a short period of 1 to 50 days in which changes in brightness are due to alternations in volume.
[1900–05; Cephe (us) + -id1]
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References in periodicals archive ?
For standard candles, the team used Cepheid variable stars, which pulsate at a rate that is correlated with their brightness, and type la supernovas, whose brightness properties are well-understood.
Oscillations occur not only in mechanical systems but also in dynamic systems in virtually every area of science: for example the beating human heart, business cycles in economics, predator-prey population cycles in ecology, geothermal geysers in geology, vibrating strings in musical instruments, periodic firing of nerve cells in the brain, and the periodic swelling of Cepheid variable stars in astronomy.
Harlow Shapley became an astronomer at Mount Wilson Observatory; studied Cepheid variable pulsations.
And be sure to check in on the classic Cepheid variable we mentioned last month, Delta ([delta]) Cephei, now high in the northwest.
A Cepheid Variable is usually a population I giant yellow star, pulsing regularly by expanding and contracting, resulting in a regular oscillation of its luminosity.
Quantifying the shapes of Cepheid variable star light curves is a technique that has been in use for the past several decades.
Since the launch of NASA's Hubble Space Telescope in 1990, the team has observed 18 galaxies up to 65 million light years away and discovered almost 800 Cepheid variable stars, a special class of pulsating star used for accurate distance measurement.
By 1912 Leavitt had worked out a method for determining the luminosity of a Cepheid variable from its period.
The three variable stars are, west to east: Delta ([delta]) Cephei, the prototype of the Cepheid variable class; Omicron (o) Ceti (Mira), the prototype of long-period or Mira variables; and Beta ([beta]) Persei (Algol), the prototype of eclipsing binaries.
We present analysis of two double model Cepheid variable stars, BQ Serpens and VX Puppis.
It is one of the most luminous in the class of so-called Cepheid variable stars.