Mu Cephei, also known as Herschel's Garnet Star, Erakis, or HD 206936, is a red supergiant or hypergiant star in the constellation Cepheus. It appears garnet red and is located at the edge of the IC 1396 nebula. Since 1943, the spectrum of this star has served as a spectral standard by which other stars are classified.
U Antliae is a variable star in the constellation Antlia. It is a carbon star surrounded by two thin shells of dust.
R Horologii is a red giant star approximately 1,000 light-years away in the southern constellation of Horologium. It is a Mira variable with a period of 404.83 days, ranging from apparent magnitude 4.7 to 14.3—one of the largest ranges in brightness known of stars in the night sky visible to the unaided eye. The star is losing mass at the rate of 5.9×10−7 M☉·y−1.
R Cassiopeiae is a variable star in the northern constellation of Cassiopeia. It is located approximately 574 light years distant from the Sun, but is drifting closer with a radial velocity of −23 km/s. This is a pulsating Mira-type variable star with a brightness varies from magnitude +4.4 down to +13.5 with a period of 433.6 days. At its maximum, R Cassiopeiae is visible to the naked eye as a faint, red-hued star.
R Centauri is a Mira variable star in the constellation Centaurus.
Zeta Cephei is a star in the constellation of Cepheus. Zeta Cephei marks the left shoulder of Cepheus, the King of Joppa (Ethiopia). It is one of the fundamental stars of the MK spectral sequence, defined as type K1.5 Ib.
W Cephei is a spectroscopic binary and variable star located in the constellation Cepheus. It is thought to be a member of the Cep OB1 stellar association at about 8,000 light years. The supergiant primary star is one of the largest known stars and as well as one of the most luminous red supergiants.
R Reticuli, also listed under the duplicate variable star designation S Reticuli, is a Mira variable star in the southern constellation Reticulum. It is an aging red giant star on the asymptotic giant branch with a stellar classification that varies between M4e to M7.5e, being hottest near maximum visual magnitude. The brightness of the star varies between apparent visual magnitudes 6.35 and 14.2 with an average period of 281.08±0.58 d. The mean maximum magnitude is 7.57 and the mean minimum magnitude 13.80.
R Boötis is a variable star in the northern constellation of Boötes. Typically the star is too faint to be readily visible to the naked eye, with a brightness that fluctuates between apparent visual magnitudes of 9.98. The distance to this star is approximately 2,150 light years based on parallax measurements. It is drifting closer with a radial velocity of about −58 km/s.
TX Camelopardalis is a Mira-type variable star in the constellation Camelopardalis. It is a classical long period variable star with pulsational period of 558.7 days. Water masers have been observed around the star.
V Cephei is a white main sequence star in the constellation Cepheus. It only varies slightly by 0.03 of a magnitude. It was suspected of being variable by American astronomer Seth Carlo Chandler noting in 1890 that it varied by 0.7 magnitude but that it needed more confirmation. Subsequent observers were divided in whether they noted variability or not. A subsequent study with photoelectric photometry showed no variability.
R Equulei is a class M Mira variable star in the constellation Equuleus. Its brightness varies between a minimum magnitude of 15.0 to a maximum of 8.7 with an average period of 261 days.
9 Cephei, also known as V337 Cephei, is a variable star in the constellation Cepheus.
S Canis Minoris is a variable star in the equatorial constellation Canis Minor. It has a peak apparent visual magnitude of 7.63±0.37, which lies below the minimum brightness that is normally visible to the naked eye. The star is located at a distance of approximately 1,600 light-years from the Sun based on stellar parallax, and is drifting further away with a radial velocity of about +68 km/s.
QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.
S Boötis is a Mira variable in the constellation Boötes. It ranges between magnitudes 7.8 and 13.8 over a period of approximately 270 days. It is too faint to be seen with the naked eye, however when it is near maximum brightness it can be seen with binoculars.
W Aquilae is a variable star in the constellation of Aquila. It is a type of evolved star known as an S-type star. Due to its relatively close distance of 1,200 light-years and equatorial location, it is easy to observe and heavily studied.
S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.
R Fornacis is a Mira variable and carbon star located in the constellation Fornax. It is around 1,800 light years away based on parallax measurements.
R Volantis is a single variable star in the southern circumpolar constellation Volans. It has an average apparent magnitude of 8.7, making it readily visible in amateur telescopes but not to the naked eye. The object is relatively far at a distance of about 2,300 light years but is drifting closer with a radial velocity of −5 km/s.
