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Xi Sculptoris, Latinized from ξ Sculptoris, is a solitary orange-hued star in the southern constellation of Sculptor, near the southern constellation boundary with Phoenix. It is just visible to the naked eye as a dim point of light with an apparent visual magnitude of 5.59. The distance to Xi Sculptoris is approximately 489 light years based on parallax, while it is drifting closer with a radial velocity of −31 km/s. It has an absolute magnitude of −0.39.
Beta Tucanae, Latinized from β Tucanae, is a group of six stars which appear to be at least loosely bound into a system in the constellation Tucana. Three of the stars are luminous and distinct enough to have been given their own Bayer designations, β1 Tucanae through β3 Tucanae. The system is approximately 140 light years from Earth.
Lambda1 Tucanae is the Bayer designation for one member of a pair of stars sharing a common proper motion through space, which lie within the southern constellation of Tucana. As of 2013, the pair had an angular separation of 20.0 arc seconds along a position angle of 82°. Together, they are barely visible to the naked eye with a combined apparent visual magnitude of 6.21. Based upon an annual parallax shift for both stars of approximately 16.5 mas as seen from Earth, this system is located roughly 198 light years from the Sun.
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.
10 Boötis is a suspected astrometric binary star system in the northern constellation of Boötes, located around 528 light years away from the Sun. It is visible to the naked eye under suitable viewing conditions as a dim, white-hued star with an apparent visual magnitude of 5.76. Its magnitude is diminished by an extinction of 0.17 due to interstellar dust. This system is moving away from the Earth with a heliocentric radial velocity of +6 km/s.
D Centauri is a double star in the southern constellation of Centaurus. The system is faintly visible to the naked eye as a point of light with a combined apparent magnitude of +5.31; the two components are of magnitude 5.78 and 6.98, respectively. It is located at a distance of approximately 610 light years from the Sun based on parallax, and is drifting further away with a radial velocity of ~10 km/s.
3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.
HD 75710 is a single star in the constellation of Vela. It has an apparent visual magnitude of approximately 4.94, which is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of 2.7 mas, it is located about 1,200 light-years from the Sun.
HD 7853 is a double star in the constellation Andromeda. With an apparent magnitude of 6.46, it can barely be seen with the naked eye even on the best of nights. The system is located approximately 130 parsecs (420 ly) distant, and the brighter star is an Am star, meaning that it has unusual metallic absorption lines. The spectral classification of kA5hF1mF2 means that it would have a spectral class of A5 if it were based solely on the calcium K line, F2 if based on the lines of other metals, and F1 if based on the hydrogen absorption lines. The two components are six arc-seconds apart and the secondary is three magnitudes fainter than the primary.
HD 29573 is a binary star system in the constellation Eridanus. It has a combined apparent visual magnitude of 4.99, making it visible to the naked eye. Based upon an annual parallax shift of 15 mas, it is located 217 light years from the Sun. The system is moving further away from Earth with a heliocentric radial velocity of +3 km/s.
Theta Sagittae (θ Sagittae) is a double star in the northern constellation of Sagitta. With a combined apparent visual magnitude of +6, it is near the limit of stars that can be seen with the naked eye. According to the Bortle scale the star is visible in dark suburban/rural skies. Based upon an annual parallax shift of 22.15 mas as seen from Earth, it is located roughly 147 light years from the Sun.
Chi1 Hydrae is a binary star in the equatorial constellation of Hydra. It originally received the Flamsteed designation of 9 Crateris before being placed in the Hydra constellation. Based upon an annual parallax shift of 22.8 mas as seen from Earth, it is located about 143 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of 4.94.
Tau1 Hydrae is a triple star system in the equatorial constellation of Hydra. Based upon the annual parallax shift of the two visible components as seen from Earth, they are located about 18 parsecs (59 ly) from the Sun. The system has a combined apparent visual magnitude of +4.59, which is bright enough to be visible to the naked eye at night.
Phi1 Hydrae, Latinized from φ1 Hydrae, is a yellow-hued star in the constellation Hydra. Its apparent magnitude is 7.61, making it too faint to be seen with the naked eye. Based upon an annual parallax shift of 12.3 mas as seen from Earth, it is located about 266 light years from the Sun. It forms a triangle with the brighter φ2 Hydrae and φ3 Hydrae, between μ Hydrae and ν Hydrae.
23 Orionis is a double star located around 1,200 light-years away from the Sun in the equatorial constellation of Orion. It is visible to the naked eye as a dim, blue-white-hued point of light with a combined apparent visual magnitude of 4.99. The pair are moving away from the Earth with a heliocentric radial velocity of +18 km/s, and they are members of the Orion OB1 association, subgroup 1a.
ξ Pavonis, Latinised as Xi Pavonis, is a triple star system in the southern constellation of Pavo. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 4.35 The system is located approximately 440 light-years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s.
ι1 Muscae, Latinised as Iota1 Muscae, is a solitary star in the southern constellation of Musca, near the southern constellation border with Chamaeleon. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude is 5.05. The star is located around 222 light-years distant from the Sun based on parallax, and is drifting further away with a radial velocity of 27.5 km/s.
53 Ophiuchi is a multiple star system in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 5.80. Located around 370 light years distant from the Sun based on parallax, it is moving closer to the Earth with a heliocentric radial velocity of −14 km/s. As of 2011, the visible components had an angular separation of 41.28″ along a position angle of 190°. The primary may itself be a close binary system with a separation of 0.3692″ and a magnitude difference of 3.97 at an infrared wavelength of 562 nm.
Delta Mensae, Latinized from δ Mensae, is a binary star system in the southern constellation of Mensa. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.69. Based upon an annual parallax shift of 7.70 mas as seen from the Earth, it is 420 light years from the Sun.
HD 111456 is a yellow-white hued star in the northern circumpolar constellation of Ursa Major. It is dimly visible to the naked eye, having an apparent visual magnitude of 5.85. Based upon an annual parallax shift of 38.2 mas as seen from Earth, it is located about 85 light years from the Sun. The star is moving closer to the Sun with a radial velocity of −18 km/s. HD 111456 is a nucleus cluster member of the Ursa Major Moving Group, a set of stars that are moving through space with a similar heading and velocity. Six other stars in the nucleus of the group are prominent members of the Big Dipper asterism.
References
- 1 2 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
- 1 2 3 4 5 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
- 1 2 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
- 1 2 3 4 Struve, Otto; Franklin, K. L. (1955). "Spectrographic Observations of Visual Double Stars". The Astrophysical Journal. 121: 337. Bibcode:1955ApJ...121..337S. doi:10.1086/145993.
- 1 2 Fabricius, C.; Høg, E.; Makarov, V. V.; Mason, B. D.; Wycoff, G. L.; Urban, S. E. (2002). "The Tycho double star catalogue". Astronomy and Astrophysics. 384: 180–189. Bibcode:2002A&A...384..180F. doi: 10.1051/0004-6361:20011822 .
- ↑ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048 , Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- 1 2 3 4 van Leeuwen, F. (November 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 Tokovinin, Andrei (2014). "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal. 147 (4): 14. arXiv: 1401.6827 . Bibcode:2014AJ....147...87T. doi:10.1088/0004-6256/147/4/87. S2CID 56066740. 87.
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- 1 2 Soubiran, Caroline; et al. (2016), "The PASTEL catalogue: 2016 version", Astronomy & Astrophysics, 591: A118, arXiv: 1605.07384 , Bibcode:2016A&A...591A.118S, doi:10.1051/0004-6361/201628497, S2CID 119258214.
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