semiregular variable star

It is a semiregular variable star with a period of around 940 days.

It is classified as a semiregular variable star and its brightness varies from magnitude 2.99 to 3.33.

It is classified as a semiregular variable star and is undergoing strong mass loss.

It is suspected of being a semiregular variable star whose apparent visual magnitude varies from +2.01 to +2.10.

It is the second brightest star in Orion, and is a semiregular variable star.

V810 Centauri is a semiregular variable star.

It is also considered to be a semiregular variable star, as its minimum and maximum magnitude are themselves variable over a period of decades.

It is a semiregular variable star with a minimum magnitude of 5.1 and a maximum magnitude of 3.4.

Distinctly reddish, it is a semiregular variable star whose apparent magnitude varies between 0.2 and 1.2, the widest range of any first-magnitude star.

BM Scorpii, is classed as a semiregular variable star, its brightness varying from magnitude +5.5 to magnitude +7.0.

Semiregular variable stars are giants or supergiants of intermediate and late spectral type showing considerable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities.

Betelgeuse is classified as a semiregular variable star of subgroup SRc; these are pulsating red supergiants with low-amplitude variations and periods of stable brightness.

VZ Camelopardalis (VZ Cam) is a Semiregular variable star in the constellation Camelopardalis.

Another, VV Cephei, like Mu Cephei, is a red supergiant and a semiregular variable star, located at least 2000 light-years from Earth.

He has contributed more than 32 000 observations of long-period and semiregular variable stars and dwarf novae to the American Association of Variable Star Observers and in 1976 was the most prolific observer of that year.