A Cepheid is a member of a class of pulsating variable stars. The relationship between a Cepheid variable's luminosity and pulsation period is quite precise, securing Cepheids as viable standard candles and the foundation of the Extragalactic Distance Scale.
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CEPHEID (CPHD) had its IPO in 2000.
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Cepheid variables
The Cepheid phase is a stage in the life cycle of a star where the star pulsates in a predictable manner, changing in brightness over a fixed period of time. This pulsation is used by astronomers to accurately measure the distance to Cepheid variable stars and other celestial objects.
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The brightness of a Cepheid star is determined by its period-luminosity relationship, which is a relationship between the star's variability period and its intrinsic luminosity. By measuring the period of a Cepheid star, astronomers can use the period-luminosity relationship to calculate its luminosity, and from there determine its apparent brightness as observed from Earth.
No, not all red giants are Cepheid variables. Cepheid variables are a specific type of variable star that pulsates regularly, making them useful for measuring cosmic distances. Red giants, on the other hand, encompass a broad class of stars in the later stages of their evolution, which may or may not exhibit variability in their brightness.
The pulsation period of a Cepheid star typically ranges from a few days to a few months. This period is directly related to the star's intrinsic brightness, making Cepheids useful for measuring astronomical distances.
seh-fee-id or see-fee-id (most common pronunciations I think:) 'seh' as in seven or 'see' as in 'sea' Important variable star for distance calculations.
Cepheid variables are a type of pulsating star whose brightness varies in a regular pattern. The key relationship used in distance measurement is the period-luminosity relation, which states that the longer the pulsation period of a Cepheid, the more luminous it is. By measuring the period of a Cepheid's brightness fluctuations, astronomers can determine its absolute brightness and compare it to its observed brightness to calculate the distance using the inverse square law of light. This method allows for accurate distance measurements to nearby galaxies and helps establish the scale of the universe.
A Cepheid variable or a nova depending on what you are trying to observe.