The property of a celestial source whose observed flux or brightness changes over time.Variability in astronomy refers to the observed change in brightness or flux of a celestial object over time. This can range from periodic pulsations of stars, like Cepheid variables, to erratic flares from active galactic nuclei, and even to the subtle flickering caused by exoplanets transiting their host star. The study of variability is fundamental because it provides a dynamic view of the universe, revealing processes that are otherwise hidden in static snapshots.
The first recorded variable star, Mira, was identified in the 16th century by David Fabricius. The systematic study of variable stars began in earnest in the 19th century with the advent of photography, allowing for the detection and classification of thousands of such objects.
The mechanisms behind variability are diverse. Intrinsic variability arises from changes within the source itself, such as stellar pulsations, eruptions, or the accretion of matter onto a compact object. Extrinsic variability is caused by external factors, like the eclipse of a star by a companion or the gravitational lensing of light by an intervening mass. By measuring the amplitude, period, and wavelength dependence of the variability, astronomers can infer physical properties like the size, mass, and energy output of the source.
Variable stars, particularly Cepheids and RR Lyrae stars, serve as standard candles for measuring cosmic distances, which is essential for determining the scale and expansion rate of the universe.
The brightness of the Sun varies by only about 0.1% over its 11-year solar cycle, making it an exceptionally stable star compared to many of its variable counterparts.





