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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.
106 Aquarii, abbreviated 106 Aqr, is a single star in the equatorial constellation of Aquarius. 106 Aquarii is the Flamsteed designation, and it also bears the Bayer designation i1 Aquarii. It has an apparent visual magnitude of +5.2, making it bright enough to be viewed from the suburbs according to the Bortle Dark-Sky Scale. An annual parallax shift of 8.61 milliarcseconds yields an estimated distance of around 380 light-years from Earth.
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°.
HD 125288 is a single star in the southern constellation of Centaurus. It has the Bayer designation v Centauri ; while HD 125288 is the star's identifier in the Henry Draper catalogue. The object has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.30. Based on parallax measurements, it is located at a distance of approximately 1,230 light years from the Sun. This is a candidate runaway star that is moving to the west and falling back into the Galactic plane. It has an absolute magnitude of −3.56.
HD 19275 is a single star in the northern constellation of Cassiopeia. It has a white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.85. The distance to HD 19275 is 163 light years as determined using parallax measurements. It is drifting further away from the Sun with a radial velocity of around 12 km/s.
HD 130458 is a double star in the southern circumpolar constellation of Apus. The pair has a combined apparent magnitude of 5.8, making it faintly visible to the naked eye under ideal conditions. Parallax measurements place the system 310-24 light years away and it is receding with a heliocentric radial velocity of 31.4 km/s.
HD 189276 is a single star in the northern constellation Cygnus, positioned near the northern constellation border with Draco. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.98. The star is located at a distance of approximately 820 light years from the Sun based on parallax, and it has an absolute magnitude of −2.25. It is drifting further away with a radial velocity of +4 km/s. The star has a high peculiar velocity of 38.5+1.8
−2.2 km/s and thus is a probable runaway star.
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 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.
Sigma Ophiuchi, Latinized from σ Ophiuchi, is a single, orange-hued star in the equatorial constellation Ophiuchus. Its apparent visual magnitude is 4.31, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of 3.62 mas as seen from Earth provides a distance estimate of roughly 900 light years. It is moving closer to the Sun with a radial velocity of −28 km/s.
θ Normae, Latinised as Theta Normae, is a binary star system in the constellation Norma. It has an apparent visual magnitude of 5.13 and is visible to the naked eye as a faint, blue-white-hued point of light. Based upon an annual parallax shift of 9.27 mas as seen from Earth, this system is located about 352 light-years from the Sun. At that distance, the visual magnitude of these stars is diminished by an extinction of 0.45 due to interstellar dust.
HD 57197, also known as M Puppis or HR 2789, is a suspected astrometric binary located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 5.84, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia satellite, the system is estimated to be 629 light years away from the Solar System. The value is poorly constrained, but it appears to be receding with a heliocentric radial velocity of 13 km/s. At its current distance, HD 57197's brightness is diminished by 0.3 magnitudes due to interstellar dust. It has an absolute magnitude of -0.43.
Alruba, a name derived from Arabic for "the foal", is a suspected astrometric binary star system in the northern circumpolar constellation of Draco. It is just barely visible to the naked eye as a dim point of light with an apparent visual magnitude of 5.76. Based on parallax measurements obtained during the Gaia mission, it is located at a distance of about 457 light-years from the Sun. The system is drifting closer with a radial velocity of −2 km/s.
Pi2 Octantis, Latinized from π2 Octantis, is a solitary star situated in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.64, allowing it to be faintly visible to the naked eye under ideal conditions. Located 1,570 light years away, the star is approaching the Sun with a heliocentric radial velocity of −13.8 km/s.
HD 222806 is a suspected astrometric binary in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.74, allowing it to be faintly seen with the naked eye. Parallax measurements place the system at a distance of 565 light years and it is currently receding with a heliocentric radial velocity of 21 km/s.
HD 46815 is a solitary star in the southern constellation Columba. It is faintly visible to the naked eye with an apparent magnitude of 5.4 and is estimated to be 408 light years away. However, it is receding with a heliocentric radial velocity of 32.2 km/s.
HD 194612 is a solitary orange hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.9, making it visible to the naked eye under ideal conditions. Parallax measurements place it at a distance of 760 light years and it has a low heliocentric radial velocity of 0.3 km/s.
HD 58425, also known as HR 2830, is an astrometric binary located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye as an orang point of light at an apparent magnitude of 5.64. Based on parallax measurements from Gaia DR3, the system is estimated to be 470 light years away from Earth. It appears to be rapidly receding from the Sun, having a heliocentric radial velocity of 58.6 km/s. HD 58425 is listed as 54 Ursae Majoris in Johann Hevelius' catalogue, but this was dropped after the official IAU's official constellation borders were drawn.
HD 40091, also known as HR 2082, is a solitary star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.54, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 501 light years distant. However, it is rapidly receding with a high heliocentric radial velocity of 114 km/s.
HD 168592, also designated as HR 6862 or rarely 7 G. Coronae Australis, is a solitary star located in the southern constellation Corona Australis. It is faintly visible to the naked eye as an orange-hued star with an apparent magnitude of 5.07. Gaia DR3 parallax measurements place it at a distance of 490 light years and is currently receding with a heliocentric radial velocity of 18 km/s. At its current distance, HD 168592's brightness is diminished by 0.38 magnitudes due to interstellar dust. It has an absolute magnitude of −0.76.
References
- 1 2 3 4 5 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 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.
- ↑ 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.
- 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 Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv: 1007.4883 , Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873
- ↑ Pasinetti Fracassini, L. E.; et al. (2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy & Astrophysics (Third ed.), 367 (2): 521–24, arXiv: astro-ph/0012289 , Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- 1 2 3 4 5 Gullikson, Kevin; Kraus, Adam; Dodson-Robinson, Sarah (2016), "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars", The Astronomical Journal, 152 (2): 40, arXiv: 1604.06456 , Bibcode:2016AJ....152...40G, doi: 10.3847/0004-6256/152/2/40 , S2CID 119179065.
- 1 2 Paunzen, E.; et al. (2005), "An empirical temperature calibration for the Δa photometric system . I. The B-type stars", Astronomy and Astrophysics, 444 (3): 941–946, arXiv: astro-ph/0509049 , Bibcode:2005A&A...444..941P, doi:10.1051/0004-6361:20053546, S2CID 119436374.
- ↑ "HD 73390". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-01-08.
- ↑ Mannings, Vincent; Barlow, Michael J. (April 1998), "Candidate Main-Sequence Stars with Debris Disks: A New Sample of Vega-like Sources", The Astrophysical Journal, 497 (1): 330–341, Bibcode:1998ApJ...497..330M, doi: 10.1086/305432 .
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