Alpha Coronae Borealis, officially named Alphecca, is an eclipsing binary star in the constellation of Corona Borealis. It is located about 75 light years from the Sun and contains two main sequence stars, one class A and one class G.
ν Tauri, Latinized as Nu Tauri, is a single star in the zodiac constellation of Taurus. It is a white-hued star and is visible to the naked eye with an apparent visual magnitude of +3.91. This object is located 117 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −6 km/s. It is predicted to come to within roughly 18.4 ly of the Sun in around five million years.
Kappa Tauri is a double star in the constellation Taurus, the two components κ1 Tauri and κ2 Tauri both members of the Hyades open cluster. The pair are approximately 150 light years from Earth and are separated from each other by about six light years.
Tau Tauri, Latinized from τ Tauri, is a quadruple star system in the constellation Taurus. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.33. The distance to this system is approximately about 400 light years based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +14.6 km/s, and it is a member of the Taurion OB association, located between Orion and Taurus. It is located 0.7 degree north of the ecliptic, and thus is subject to lunar occultations.
Celaeno, designated 16 Tauri, is a star in the constellation of Taurus and a member of the Pleiades open star cluster (M45) of stars.
Beta Comae Berenices is a main sequence dwarf star in the northern constellation of Coma Berenices. It is located at a distance of about 29.95 light-years from Earth. The Greek letter beta (β) usually indicates that the star has the second highest visual magnitude in the constellation. However, with an apparent visual magnitude of 4.3, this star is actually slightly brighter than α Comae Berenices. It can be seen with the naked eye, but may be too dim to be viewed from a built-up urban area.
Delta2 Canis Minoris is a main-sequence star in the constellation Canis Minor, about 141 ly away.
Gamma Gruis or γ Gruis, formally named Aldhanab, is a star in the southern constellation of Grus. With an apparent visual magnitude of 3.0, it is the third-brightest star in Grus. Based upon parallax measurements, this star is located at a distance of roughly 211 light-years from the Sun.
Theta2 Crucis, Latinized from θ2 Crucis, is a spectroscopic binary star in the constellation Crux. This pair of stars complete an orbit every 3.4280 days and they have a low orbital eccentricity that is close to 0.0. Theta2 Crucis is located at about 690 light-years from the Sun.
HD 127304 is a double star in the northern constellation of Boötes. The brighter component is a sixth magnitude A-type main sequence star with a stellar classification of A0Vs It has a faint magnitude 10.62 companion at an angular separation of 25.6″ along a position angle of 256°.
5 Camelopardalis is a binary star system in the northern circumpolar constellation of Camelopardalis, located about 770 light years away from the Sun as determined using parallax. With an apparent magnitude of 5.5, it can be seen with the naked eye as a faint, blue-white hued star. The system is moving further from the Earth with a heliocentric radial velocity of +2.4 km/s.
RU Lupi is a star in the constellation of Lupus, located in the young Lupus Star Forming Region. Based on parallax measurements, the distance to this star is about 514 light-years (158 pc). The apparent visual magnitude is 10.5, so viewing it would require a telescope with an aperture of 6 cm (2 in), but preferably larger.
26 Draconis is a triple star system in the constellation Draco, located 46 light years from the Sun. Two of the system components, A and B, form a spectroscopic binary that completes an orbit every 76 years. The composite spectral classification of the AB pair is G0V, which decomposes to individual spectral types F9V and K3V. A 1962 study estimated the masses of these two stars as 1.30 and 0.83 times the mass of the Sun, respectively. The stars are considered moderately metal-poor compared to the Sun, which means they have a lower proportion of elements other than hydrogen or helium.
111 Tauri is a wide binary star system in the constellation Taurus. It is located at a distance of 48 light years from the Sun. Primary component A is a main sequence star with a stellar classification of F8V. The secondary component B is a K-type main sequence star. The primary is larger and more luminous than the Sun, with about 130% of the Sun's radius and 185% of the Sun's luminosity. The apparent magnitude of 5.0 indicates it is a faint star that can be viewed by the naked eye under good, dark-sky conditions.
6 Equulei is a probable astrometric binary star system in the northern constellation of Equuleus, located 380 light years from the Sun. It is barely visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 6.07. The system is moving further away from the Earth with a heliocentric radial velocity of +6.9 km/s. It forms a wide optical double with γ Equulei, at an angular separation of 336 arcseconds in 2011.
Kappa2 Coronae Australis, Latinized from κ2 Coronae Australis, is the primary of a probable binary system located in the southern constellation Corona Australis. It is visible to the naked eye as a bluish-white hued star with an apparent visual magnitude of 5.59. The distance to this star is roughly 710 light years based on Gaia DR3 parallax measurements. The radial velocity is poorly constrained, but the star appears to be moving closer with a radial velocity of around −15 km/s. At its current distance, Kappa2 CrA's brightness is diminished by 0.45 magnitudes due to interstellar dust.
ι Phoenicis, Latinized as Iota Phoenicis, is a binary star system in the southern constellation of Phoenix, near the constellation border with Grus. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude that fluctuates around 4.71. This system lies approximately 254 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +19.4 km/s.
υ Gruis, Latinised as Upsilon Gruis, is a double star in the southern constellation of Grus. The apparent magnitude is 5.61, which is bright enough to be viewed with the naked eye. Located around 87 parsecs (280 ly) distant, the white-hued primary is an A-type main-sequence star of spectral type A1V, a star that is currently fusing its core hydrogen. it is spinning rapidly with a projected rotational velocity of 320 km/s. The companion is a magnitude 8.24 star at an angular separation of 0.90″ from the primary along a position angle of 205°, as of 2009.
T Coronae Australis, is a young star in the constellation Corona Australis. It is a member of the Corona Australis star-forming region, which is located about 502 light-years (154.0 pc) from the Sun. It has a spectral type of F0e and is surrounded by a circumstellar disk, seen edge-on.
41 Tauri is a single-lined spectroscopic binary system in the zodiacal constellation of Taurus; 41 Tauri is its Flamsteed designation. The star has a visual magnitude of 5.19, making it visible to the naked eye from brighter suburban skies. Parallax measurements put it at a distance of roughly 404 light years from the Sun.
