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A slow irregular variable (ascribed the GCVS types L, LB and LC) is a variable star that exhibit no or very poorly defined periodicity in their slowly changing light emissions. These stars have often been little-studied, and once more is learnt about them, they are reclassified into other categories such as semiregular variables.

Most of irregular variables are cool stars of late spectral types K and M, S stars or carbon stars. They are divided into LB:s, which are generally giants, and LC:s—supergiants exhibiting a light variation interval of about 1 magnitude.^[1]

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Variable stars Pulsating Cepheids and cepheid-like Classical Type II (BL Herculis, W Virginis) RR Lyrae Delta Scuti Rapidly oscillating Ap SX Phoenicis Blue-white with early spectra Alpha Cygni Beta Cephei Slowly pulsating B PV Telescopii Long-period and semiregular Mira Semiregular Slow irregular Other Gamma Doradus RV Tauri Solar-like oscillations White dwarf Eruptive Protostar FU Orionis Herbig Ae/Be Orion Giants and supergiants Luminous blue variable R Coronae Borealis (DY Persei) Yellow hypergiant Eruptive binary Double periodic FS Canis Majoris RS Canum Venaticorum Other Flare Gamma Cassiopeiae Lambda Eridani Wolf–Rayet Cataclysmic AM Canum Venaticorum Dwarf nova Nova Supernova Symbiotic Z Andromedae Rotating Non-spherical Rotating ellipsoidal Stellar spots BY Draconis FK Comae Berenices Magnetic fields Alpha² Canum Venaticorum Pulsar SX Arietis Eclipsing Algol Beta Lyrae Planetary transit W Ursae Majoris Star portal