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...veness in the [[Irregular variable|irregular]] variables. The [[W Virginis variables]] are at the interface; the short period ones are regular and the longer pe ...ators, which have smaller fluctuations in brightness than those of regular variables used as standard candles.<ref>{{cite journal|bibcode=2010ApJ...713L.192G|ti ...

...'' is a relationship linking the [[bolometric luminosity|luminosity]] of [[pulsating variable star]]s with their pulsation period. ...n between the periods and the brightness of a sample of 25 of the Cepheids variables in the Small Magellanic Cloud, published in 1912.<ref name="Leavitt1912">{{ ...

...surface from deep inside the star. It is also a Mira variable, a type of pulsating [[giant star]] which varies by several [[apparent magnitude]]s with a perio [[Category:Mira variables]] ...

...rm Variability of Evolved Massive Stars with TESS II: A New Class of Cool, Pulsating Supergiants|journal=The Astrophysical Journal|year=2020|volume=902|issue=1| [[Category:Slow irregular variables]] ...

...s:1998129|title=Hipparcos photometry of 24 variable massive stars (α Cygni variables)|journal=Astronomy and Astrophysics Supplement Series|volume=128|pages=117– ...em |first6=K. Azalee |date=2023-01-01 |title=The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants |journal=America ...

...s '''Population I Cepheids''', '''Type I Cepheids''', and '''Delta Cepheid variables'''. ...}</ref> [[Hubble Space Telescope]] (HST) observations of classical Cepheid variables have enabled firmer constraints on [[Hubble's law]], which describes the ex ...

...[Scutum (constellation)|Scutum]]. It is a yellow [[supergiant]] and is a [[pulsating variable]] known as an [[RV Tauri variable]]. It was discovered in 1795 by RV Tauri variables often have somewhat irregular light curves, both in amplitude and period, b ...

In 2013 the luminosity of Mira variables, based on [[Hipparcos]] parallaxes, was used to calibrate a [[Period-lumino ...Kjeldsen |first6=H. |title=Long-term photometry and periods for 261 nearby pulsating M giants |journal=Monthly Notices of the Royal Astronomical Society |date=D ...

...h><x^2></math> denotes the [[variance]] of the [[Dependent and independent variables|dependent variable]] <math>x_k</math>. |author1=C. Schoenaers |author2=A. E. Lynas-Gray | title = A new slowly pulsating subdwarf-B star: HD 4539 ...

...rs thickness, totaling 4 × 10¹⁰ stars. [[Cephid variable]]s are pulsating stars that have a [[period-luminosity relation]], exploited by [[Harlow Sha ...