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HD 69863 is a binary star system in the southern constellation of Carina. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.16. The system is located at a distance of about255 light years from the Sun based on parallax. The dual nature of this system was announced in 1832 by German astronomer Carl Rümker. As of 2015, the pair had an angular separation of 4.10″ along a position angle of 70°.
HR 4177, also called t2 Carinae, is a double star in the southern constellation of Carina. It is faintly visible to the naked eye with a combined apparent visual magnitude of +4.77. The two components are HD 92397 and HD 92398. The primary component is located at a distance of approximately 1,600 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +11 km/s. It has a peculiar velocity of 24.3+9.9
−16.1 km/s and may be a runaway star. The star is a member of the BH 99 cluster.
V376 Carinae is a binary star system in the southern constellation of Carina. It has the Bayer designation b1 Carinae; V376 Carinae is the variable star designation. The system is visible to the naked eye as a faint point of light with a combined apparent magnitude of +4.69. The distance to this system from the Sun is approximately 650 light years based on parallax. It is drifting further away with a radial velocity of +27 km/s.
HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.
HD 111597 is a suspected astrometric binary star system in the southern constellation of Centaurus. It has the Bayer designation p Centauri, while HD 111597 is the star's identifier from the Henry Draper catalogue. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.90. It is located at a distance of approximately 380 light years from the Sun based on parallax, and has an absolute magnitude of −0.53. The system is a probable member of the Sco OB2 association of co-moving stars. The visible component is a B-type main-sequence star with a stellar classification of B9V.
Omega Fornacis, which is Latinized from ω Fornacis, is a wide binary star system in the southern constellation of Fornax. It has a blue-white hue and is faintly visible to the naked eye as a fifth-magnitude star. The system lies at a distance of approximately 470 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s.
HD 41534 is a binary star system in the southern constellation of Columba. It is dimply visible to the naked eye with a combined apparent visual magnitude of 5.65. The distance to this system is approximately 950 light-years based on parallax, and it is receding from the Sun with a radial velocity of +93 km/s. This is a runaway star system with an unusually high peculiar velocity of 187.6+12.2
−13.8 km/s. It is thought to have been ejected from the OB association Sco OB 1 approximately 14 million years ago.
ι Crucis, Latinized as Iota Crucis, is a wide double star in the southern constellation of Crux. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4m.69. This object is located 125 light-years from the Sun, based on parallax, and is drifting further away with a radial velocity of +7.5 km/s.
HD 172044 is a triple star system in the northern constellation of Lyra. It has a blue-white hue and is visible to the naked eye with an apparent visual magnitude of 5.41. The distance to the primary component is approximately 535 light years based on parallax. It is drifting closer with a radial velocity of −32.5 km/s, and is predicted to come as near as 77.3 light-years to the Sun some 4.5 million years from now.
HD 196050 is a triple star system located in the southern constellation of Pavo. This system has an apparent magnitude of 7.50 and the absolute magnitude is 4.01. It is located at a distance of 165 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +61 km/s. It is also called by the Hipparcos designation HIP 101806.
HD 222093 is a double star in the equatorial constellation of Aquarius. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 5.68. The system is located at a distance of approximately 293 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −13 km/s.
27 Hydrae is a triple star system system in the equatorial constellation of Hydra, located 222 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with a combined apparent visual magnitude of 4.82. The system is moving further from the Earth with a heliocentric radial velocity of +25.6 km/s.
HD 102350 is a single star in the constellation Centaurus. It has a yellow hue and is visible to the naked eye with an apparent visual magnitude of 4.11. The distance to this star is approximately 390 light years based on parallax, but it is drifting closer with a radial velocity of −3 km/s. It has an absolute magnitude of −1.51.
HD 216446 is a binary star system in the northern circumpolar constellation of Cepheus. It is faintly visible to the naked eye with a combined apparent visual magnitude of 4.77. The system is located at a distance of approximately 319 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −32 km/s. It is predicted to come to within 188.7 light-years in around 1.876 million years. The system has an absolute magnitude of −0.14.
HD 211073 is a triple star system in the northern constellation Lacerta, located around 580 light years from the Sun. It is visible to the naked eye as a faint orange-hued star with a baseline apparent visual magnitude of 4.50. The system is moving closer to the Earth with a heliocentric radial velocity of −11.7 km/s.
λ Coronae Australis, Latinized as Lambda Coronae Australis is a binary star system located in the southern constellation of Corona Australis. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 5.11. The system is located at a distance of 205 light-years, based on parallax, and is drifting further away with a radial velocity of −26 km/s.
HD 34968 is a binary star system in the southern constellation Lepus. The combined apparent visual magnitude of 4.69 is bright enough to be visible to the naked eye. The distance to HD 34968 can be estimated from its annual parallax shift of 8.7 mas, yielding a range of 374 light years. It is moving further away from the Earth with a heliocentric radial velocity of 31 km/s, having come within 118.6 ly some 3,686,000 years ago.
74 Ophiuchi is a suspected binary star in the equatorial constellation of Ophiuchus, near the border with Serpens Cauda. It is visible to the naked eye as a faint, yellow-hued point of light with a combined apparent visual magnitude of 4.85. The system is located at a distance of 238 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +4.4 km/s.
HR 4180 is a double star with components HD 92449 and HD 92463 in the southern constellation of Vela. They are probably members of a binary star system. HR 4180 can be viewed with the naked eye, having an apparent visual magnitude of 4.29. Based upon the annual parallax shift of the two stars it is located approximately 780 light years from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of +20 km/s.
HR 5401 is a possible astrometric binary star system in the southern constellation of Lupus. With an apparent visual magnitude of 5.83, it is just visible to the naked eye under good seeing conditions. The distance to HR 5401 can be estimated from its annual parallax shift of 15.9 mas, yielding a range of 205 light years. It is moving closer to Earth with a heliocentric radial velocity of −30 km/s, and is expected to come within 161 ly in ~524,000 years.
References
- 1 2 3 4 5 6 7 8 9 10 11 12 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 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 Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x , S2CID 14878976.
- 1 2 Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1975mcts.book.....H.
- ↑ "HD 73389". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-07-11.
- ↑ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi: 10.1086/323920 , retrieved 2015-07-22
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