Explore: Mira Variables

Mira variables /ˈmaɪrə/ (named for the prototype star Mira) are a class of pulsating stars characterized by very red colours, pulsation periods longer

variable red giant (Mira A) along with a white dwarf companion (Mira B). Mira A is a pulsating variable star and was the first non-supernova variable

semiregular variable stars, particularly the SRa and SRb sub-classes, are often grouped with the Mira variables under the long-period variable heading. In

Catalogue of Variable Stars does not define a long-period variable star type, although it does describe Mira variables as long-period variables. The term

variables are very closely related to Mira variables, possibly the only difference being pulsating in a different harmonic. Slow irregular variables These

Look up mira in Wiktionary, the free dictionary. Mira is a star in the constellation Cetus Mira may also refer to: Mira (1971 film), a Dutch-Belgian film

1×10−7 M☉/yr, close to average for a short-period Mira variable. While most short-period Mira variables reside in the Galactic halo, R Trianguli is a member

first defined in 1922 to represent a number of long-period variables (meaning Mira variables) and stars with similar peculiar spectra. Many of the absorption

likened to a Mira variable when its variations are relatively regular, although its amplitude of only 1.5 magnitudes is smaller than Mira variables. The star

variables where the partial second ionization of helium occurs. Hydrogen ionization is most likely the cause of pulsation activity in Mira variables,