Linked from

The 15 pages that link to Mira variable, each with the reason it gives.

• Hubble tensionRelated: Mira-based distance measurements offer another independent check on local expansion.

• Standard candleBroader topic: Its period–luminosity relation enables distance estimates in nearby galaxies.

• Asymptotic giant branchBroader topic: Many branch stars show large-amplitude pulsations that identify them as Mira variables.

• RR Lyrae variableCompared with: Its cool giant structure and long cycle contrast with RR Lyrae stars’ shorter pulsations.

• Period–luminosity relationCompared with: Mira stars have their own period–luminosity behavior, separate from Cepheid calibrations.

• Stellar pulsationBroader topic: Mira stars illustrate how pulsation in an expanded giant can drive strong brightness and radius changes.

• Carbon starRelated: Some carbon stars are Mira variables, linking carbon enrichment with large-amplitude pulsation.

• Circumstellar envelopeBroader topic: Mira variables often lose mass through dense winds that form extended envelopes.

• Helium flashRelated: Such stars descend from low-mass stars whose core helium burning began after a flash.

• MiraBroader topic: Mira gives this subgroup of long-period variables its name.

• Instability stripCompared with: Mira stars pulsate far from the classical strip and arise at a later evolutionary stage.

• Kappa mechanismBroader topic: Opacity-related pulsation physics helps explain its repeated expansion and contraction.

• Type II CepheidCompared with: Mira variables also pulsate, but their giant-star structure and variability differ from Type II Cepheids.

• AlgolCompared with: Mira changes intrinsically, unlike Algol’s recurring eclipse-driven dimming.

• CW LeonisRelated: CW Leonis varies in brightness as its extended atmosphere pulsates.