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Psi Velorum, Latinized from ψ Velorum, is a binary star system in the southern constellation of Vela. Based upon an annual parallax shift of 53.15 mas as seen from Earth, it is located 61.4 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of +3.58. The motion of this system through space makes it a candidate member of the Castor stellar kinematic group.
12 Boötis is a spectroscopic binary in the constellation Boötes. It is approximately 122 light years from Earth.
Upsilon2 Centauri is a binary star system in the southern constellation Centaurus. It is visible to the naked eye with an apparent visual magnitude of +4.33. Based upon an annual parallax shift of just 2.57 mas as seen from Earth, this star is located roughly 1,300 light years from the Sun. Relative to its neighbors, the system has a peculiar velocity of 39.2+8.8
−15.2 km/s and it may form a runaway star system.
Theta Pictoris is a star in the Pictor constellation.
HR 9038 is a triple star system located thirty-five light-years away, in the constellation Cepheus. Component A is a spectroscopic binary system with an orbital period of 7.753 days and a combined stellar classification of K3 V. Component B is a red dwarf star that orbits the primary pair every 290 years.
HD 87822 is a triple star in the northern constellation of Leo Minor. The inner pair orbit each other with a period of about 18 years.
HD 222109 is a binary star system located in the northern constellation of Andromeda. It has a combined apparent visual magnitude of 5.80, which allows it to be visible to the naked eye as a single star. The system has a combined spectral classification of B8V. It is situated at a distance of approximately 800 light years from the Solar System, and the two stars orbit each other with a period of 351.22 years. They are separated by a distance of 0.41″ and have an orbital eccentricity of 0.39. Individually, the stars have apparent magnitudes of 6.08 and 7.38, respectively.
HD 224635 and HD 224636 is a pair of stars comprising a binary star system in the constellation Andromeda. They are located approximately 94 light years away and they orbit each other every 717 years.
HD 216718 is a binary star system in the equatorial constellation of Aquarius.
HD 200375 is a binary star system in the equatorial constellation of Aquarius. Their orbit does not yet have a unique solution available.
HD 188405 is a binary star in the equatorial constellation of Aquila. The pair have an orbital period of roughly 425 years and an angular separation of 1.085″.
HD 153370 is binary star in the southern constellation of Ara.
HD 118889 is a binary star system in the northern constellation of Boötes. It is faintly visible to the naked eye as a point of light with an apparent visual magnitude of 5.57. The system is located at a distance of approximately 196 light years from the Sun based on stellar parallax, but is drifting closer with a radial velocity of −26 km/s.
HD 127726 is a binary star system in the northern constellation of Boötes. The pair consist of a rapidly-rotating A-type main-sequence star and a fainter F-type companion, orbiting each other with a period of 29.93 years and an orbital eccentricity (ovalness) of 0.16. They have a combined apparent visual magnitude of 5.88, which is bright enough to be dimly visible to the naked eye. The system is located at a distance of approximately 240 light years from the Sun.
Iota Coronae Borealis, Latinized from ι Coronae Borealis, is a binary star system in the constellation Corona Borealis. It is visible to the naked eye with a combined apparent visual magnitude of is 4.96. Based upon an annual parallax shift of 10.46 mas as seen from the Earth, it is located about 312 light years from the Sun.
Psi Pegasi, which is Latinized from ψ Pegasi, is a binary star system within the great square in the northern constellation of Pegasus. It has a red hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.66. This object is located at a distance of approximately 476 light-years away from the Sun based on parallax, but is drifting closer with a radial velocity of −6.6 km/s.
Eta Horologii is a binary star system in the southern constellation of Horologium. It is visible to the naked eye with a combined apparent visual magnitude of 5.31. Based upon an annual parallax shift of 21.95 mas as seen from Earth, it is located around 149 light years from the Sun.
HD 3322 is a binary star system in the northern constellation of Andromeda. With an apparent visual magnitude of 6.51, it lies below the nominal brightness limit for visibility with the normal naked eye, but it is still possible to see the star with excellent vision under ideal seeing conditions. An annual parallax shift of 4.59±0.65 mas provides a distance estimate of roughly 700 light years.
λ Librae is the Bayer designation for a binary star system in the zodiac constellation of Libra. It can be faintly seen with the naked eye, having an apparent visual magnitude of 5.03. With an annual parallax shift of 10.54 mas, it is roughly 310 light years from the Sun. At that distance, the visual magnitude of this system is diminished by an extinction factor of 0.22 due to interstellar dust. It is 0.1 degree north of the ecliptic.
Psi Crateris, Latinized from ψ Crateris, is the Bayer designation for a visual binary star system in the southern constellation of Crater. It is faintly visible to the naked eye with an apparent visual magnitude of 6.13. According to the Bortle scale, it requires dark suburban or rural skies to view. Based upon an annual parallax shift of 6.5 mas, the system is located approximately 500 light years away from the Sun.
References
- 1 2 3 4 5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
- 1 2 3 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N
- ↑ Malkov, O. Yu.; et al. (2012), "Dynamical Masses of a Selected Sample of Orbital Binaries", Astronomy & Astrophysics, 546: 5, Bibcode:2012A&A...546A..69M, doi: 10.1051/0004-6361/201219774 , A69
- ↑ Abt, H. A. (September 1985), "Visual multiples. VIII - 1000 MK types", Astrophysical Journal Supplement Series, 59: 95–112, Bibcode:1985ApJS...59...95A, doi: 10.1086/191064
- 1 2 3 Olevic, D.; Cvetkovic, Z. (2004), "Orbits of 6 Binaries", Serbian Astronomical Journal, 168 (168): 25–36, Bibcode:2004SerAJ.168...25O, doi: 10.2298/saj0468025o
- 1 2 Soubiran, C.; et al. (March 2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics, 480 (1): 91–101, arXiv: 0712.1370 , Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788, S2CID 16602121
- ↑ Muñoz Bermejo, J.; et al. (May 2013), "A PCA approach to stellar effective temperatures", Astronomy and Astrophysics, 453: A95, arXiv: 1303.7218 , Bibcode:2013A&A...553A..95M, doi:10.1051/0004-6361/201220961, S2CID 67752733.
