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Beta Cancri, also named Tarf, is the brightest star in the zodiacal constellation of Cancer. It has an apparent visual magnitude of +3.5 and an absolute magnitude of −1.2. Based on parallax measurements obtained by the Gaia spacecraft, it is approximately 323 light-years distant from the Sun. An exoplanet, designated Beta Cancri b, is believed to be orbiting the star.
Upsilon Serpentis, Latinized from υ Serpentis, is a star in the Serpens Caput section of the constellation Serpens. Based upon an annual parallax shift of 13.04 mas as seen from Earth, it is located around 250 light years from the Sun. The star is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of +5.70. It is a member of the Hyades group, a stream of stars that share a similar trajectory to the Hyades cluster.
Psi Ursae Majoris is a star in the northern circumpolar constellation of Ursa Major. It has an apparent visual magnitude of +3.01, making it a third magnitude star and one of the brighter members of the constellation. Parallax measurements place it at a distance of 140 light-years from Earth. This is sufficiently close that the magnitude of the star is only reduced by 0.05 due to extinction. In Chinese astronomy, Psi Ursae Majoris is called Tien Tsan or Ta Tsun, "Extremely Honorable". The name was possibly derived from the word 太尊, Pinyin: Tàizūn, meaning Royals, because this star stands alone as the only member of the Royals asterism within the Purple Forbidden enclosure.
Nu Ursae Majoris, formally named Alula Borealis, is a double star in the northern circumpolar constellation of Ursa Major. At an apparent visual magnitude of +3.490, it is bright enough to be seen with the naked eye. Based upon parallax measurements, the distance to ν Ursae Majoris is about 399 light-years. At such distance, its apparent brightness is diminished by 0.48 magnitudes due to interveining gas and dust.
Eta Ursae Minoris is a yellow-white hued star in the northern circumpolar constellation of Ursa Minor.
Theta Ursae Minoris, Latinized from θ Ursae Minoris, is a suspected binary star system that is visible to the naked eye in the northern circumpolar constellation of Ursa Minor. It is roughly 860 light years from Earth with an apparent visual magnitude of 5.0. The system is moving closer to the Sun with a radial velocity of −25 km/s.
Pi1 Ursae Minoris is a common proper motion binary star system in the northern circumpolar constellation of Ursa Minor. The pair have apparent visual magnitudes of +6.58 and +7.31, with a combined magnitude of 6.1. They are located about 71 light years from the Sun. The two have an angular separation of 31.4 arc seconds, which corresponds to a physical separation of about 680 AU, and orbit each other with a period of about 13,100 years.
Delta1 Canis Minoris, Latinized from δ1 Canis Minoris, is a solitary, yellow-white hued star in the constellation Canis Minor. It is faintly visible to the naked eye with an apparent visual magnitude of +5.25. Based upon an annual parallax shift of 4.29 mas as seen from Earth, this star is located roughly 760 light years from the Sun.
Delta3 Canis Minoris, Latinized from δ3 Canis Minoris, is a solitary, white-hued star in the equatorial constellation of Canis Minor. Based upon a parallax of 4.46 mas as seen from Gaia spacecraft in its repeated orbits around the Sun, just beyond the Earth. This star is about 730 light years from the Solar System. At that distance, the visual magnitude of these stars is diminished by an extinction of more than 0.15 due to interstellar dust. With an apparent visual magnitude of +5.81, it is just bright enough to be faintly visible to the naked eye.
Epsilon Canis Minoris is a suspected binary star system in the equatorial constellation of Canis Minor. It is a fifth magnitude star, which means it is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of just 3.13 mas as seen from Earth, this star is located roughly 770 light years from the Sun, give or take a 40 light year margin of error.
20 Canum Venaticorum is a single variable star in the northern constellation of Canes Venatici, located 238 light years from the Sun. This object has the variable star designation AO Canum Venaticorum; 20 Canum Venaticorum is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a baseline apparent visual magnitude of +4.72. The star is moving further from the Earth with a heliocentric radial velocity of +9 km/s. Eggen (1971) listed this star as a member of the Hyades Stream.
C3 Centauri is a suspected astrometric binary star system in the southern constellation of Centaurus. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.46. The distance to this object is approximately 342 light years based on parallax. It is a member of the Hyades Stream of co-moving stars.
39 Cygni is a binary star system near the southern border of the northern constellation of Cygnus, approximately 270 light years away from Earth. It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.43. The system is moving closer to the Sun with a heliocentric radial velocity of −15 km/s.
HD 32518 is a star with an orbiting exoplanet in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 6.42, placing it near the limit of naked eye visibility. Located 397 light years away based on parallax measurements, it is receding with a heliocentric radial velocity of −7.02 km/s.
11 Ursae Minoris is a single star located approximately 410 light years away in the northern circumpolar constellation of Ursa Minor. The star is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.15. It is moving closer to the Earth with a heliocentric radial velocity of −17.5 km/s.
Gamma Comae Berenices, Latinized from γ Comae Berenices, is a single, orange-hued star in the northern constellation of Coma Berenices. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.36. Based upon an annual parallax shift of 19.50 mas as seen from Earth, its distance can be estimated as around 167 light years from the Sun. The star is moving away from the Sun with a radial velocity of +3 km/s.
21 Camelopardalis is a star in the northern circumpolar constellation of Camelopardalis, located around 650 light years away from the Sun. It is a challenge to view with the naked eye even under excellent viewing conditions, having an apparent visual magnitude of 6.9. This is one of the fainter stars with a Flamsteed designation, one of only 220 below the magnitude cutoff for the Bright Star Catalogue. It is moving closer to the Earth with a heliocentric radial velocity of −15.5 km/s.
Eta Sagittae (η Sagittae) is solitary star in the northern constellation of Sagitta. It is faintly visible to the naked eye, having an apparent visual magnitude of +5.09. Based upon an annual parallax shift of 20.34 mas, it is approximately 160 light years distant from the Sun. There is a 61.1% chance that it is a member of the Hyades-Pleiades stream of stars that share a common motion through space.
RR Ursae Minoris, abbreviated RR UMi, is a binary star system in the northern circumpolar constellation of Ursa Minor. It can be viewed with the naked eye, typically having an apparent visual magnitude of around 4.710. Based upon an annual parallax shift of 7.1 mas as seen from Earth's orbit, it is located 460 light years away. The system is moving further from the Sun with a heliocentric radial velocity of +6 km/s.
23 Leonis Minoris is a solitary, bluish-white hued star located in the northern constellation Leo Minor. It is positioned 7° south and 11" west from β Leonis Minoris. It is rarely called 7 H. Leonis Minoris, which is its Hevelius designation.
References
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- 1 2 Stello, D.; et al. (2008), "Oscillating K Giants with the WIRE Satellite: Determination of Their Asteroseismic Masses", The Astrophysical Journal Letters, 674 (1): L53–L56, arXiv: 0801.2155 , Bibcode:2008ApJ...674L..53S, doi:10.1086/528936, S2CID 15094067.
- ↑ Lèbre, A.; et al. (May 2006), "Lithium abundances and rotational behavior for bright giant stars", Astronomy and Astrophysics, 450 (3): 1173–1179, Bibcode:2006A&A...450.1173L, doi: 10.1051/0004-6361:20053485 .
- ↑ "HD 5848". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2007-01-04.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society , 389 (2): 869–879, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x , S2CID 14878976.
