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4 Cassiopeiae is a red giant in the northern constellation of Cassiopeia, located approximately 790 light-years away from the Sun. It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96. At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust. This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.
HD 5789 and HD 5788 is a pair of stars comprising a binary star system in the northern constellation of Andromeda. Located approximately 151 parsecs (490 ly) away, the primary is a hot, massive blue star with an apparent magnitude of 6.06 while the secondary is slightly smaller and cooler, with an apparent magnitude of 6.76. Both stars are main-sequence stars, meaning that they are currently fusing hydrogen into helium in their cores. As of 2016, the pair had an angular separation of 7.90″ along a position angle of 195°. While both have a similar proper motion and parallax, there's still no proof that the pair is gravitationally bound.
HD 131551 is a solitary star in the southern constellation Apus. It has an apparent magnitude of 6.19, allowing it to be faintly seen with the naked eye under ideal conditions. Located 526 light years away, the object is approaching the Sun with a heliocentric radial velocity of 7.6 km/s.
40 Aquarii is a star in the equatorial constellation of Aquarius. 40 Aquarii is its Flamsteed designation; it was too faint to be included in the Bright Star Catalogue. The brightness of this star is below the normal limit for visibility with the naked eye, having an apparent visual magnitude of 6.93. Based upon parallax measurements, it is located about 726 light-years away from the Sun. It is moving closer to the Earth with a heliocentric radial velocity of -3 km/s. 40 Aquarii is positioned near the ecliptic and thus is subject to lunar occultations.
Psi1 Piscium is a binary star in the constellation Pisces. It is approximately 280 light years from Earth, based on its parallax.
46 Ceti is a single star in the equatorial constellation of Cetus. It is visible to the naked eye with an apparent visual magnitude of 4.9. The distance to this star, as determined from an annual parallax shift of 11.9 mas, is about 273 light years. It is moving closer to the Earth with a heliocentric radial velocity of −23 km/s, and is expected to come as close as 184 light-years in 2.2 million years.
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.
Epsilon Microscopii, Latinized from ε Microscopii, is a single, white-hued star in the southern constellationof Microscopium. It is faintly visible to the naked eye with an apparent visual magnitude of 4.71. The annual parallax shift of the star is 19.7054 mas as measured from Earth, which yields a distance estimate of around 166 light years. It is moving further from the Sun with a radial velocity of +7 km/s.
3 Monocerotis is a binary star system in the equatorial constellation of Monoceros, located approximately 780 light years away from the Sun based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.92. The system is moving further from the Earth with a heliocentric radial velocity of +39 km/s.
θ Octantis, Latinized as Theta Octantis, is a single star in the southern circumpolar constellation of Octans, near the constellation border with Hydrus. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.78. The star is located approximately 217 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +22.5 km/s.
HD 44131 is a star in the equatorial constellation of Orion, positioned near the eastern constellation border with Monoceros. It has a reddish hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.91. The star is located at a distance of approximately 465 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +48.6 km/s. Based on radial velocity variations, it is a candidate spectroscopic binary system and a preliminary orbital solution was published in 1991 with a period of 9.29 yr. However, these velocity variations may be due to other causes.
Eta Pavonis, a name latinized from η Pavonis, is a single star in the southern constellation of Pavo, positioned near the western constellation border next to Ara. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 3.61. Based on parallax, this object is located at a distance of approximately 350 light-years (108 pc) from the Sun. It has an absolute magnitude of −1.56, and is drifting closer with a radial velocity of −7.6 km/s.
Gamma Pictoris, Latinised from γ Pictoris, is a single, orange-hued star in the southern constellation of Pictor. It is a faintly visible to the naked eye with an apparent visual magnitude of 4.50. Based upon an annual parallax shift of 18.45 mas as seen from Earth, this star is located about 177 light-years from the Sun. It is moving away from the Sun with a radial velocity of +15.7 km/s.
31 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a dim, blue-white hued point of light with an apparent visual magnitude of 5.05. This star is located around 172 parsecs (560 ly) away from the Sun, and it is drifting closer with a radial velocity of −1.6 km/s. It is likely a member of the Alpha Persei Cluster.
Gamma1 Octantis, Latinized from γ1 Octantis, is a single, yellow-hued star in the constellation which includes the southern celestial pole, Octans. Its apparent visual magnitude is 5.10, meaning that in good conditions it is bright enough to be faintly visible to the naked eye.
HD 33266 is a solitary star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 6.17, making it faintly visible to the naked eye. Located 481 light years away, it is approaching the Sun with a heliocentric radial velocity of −4.4 km/s.
HD 166006, also known as HR 6778, is a solitary orange-hued star located in the southern constellation Telescopium. It has an apparent magnitude of 6.07, making it barely visible to the naked eye. Based on Gaia DR2 parallax measurements, the object is located 582 light years away. It is currently approaching the Solar System with a somewhat constrained heliocentric radial velocity of −15 km/s.
5 Trianguli is a solitary star located in the northern constellation Triangulum. With an apparent magnitude of 6.23, it’s barely visible to the naked eye under ideal conditions. The star is located 399 light years away from the Solar System, but is drifting away with a radial velocity of 7.7 km/s.
HD 191829 is a solitary star located in the southern constellation Telescopium. It has an apparent magnitude of 5.632, making it faintly visible to the naked eye if viewed under ideal conditions. The star is situated at a distance of 710 light years but is receding with a heliocentric radial velocity of 14 km/s.
Mu1 Octantis, Latinized from μ1 Octantis, is a solitary star in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.98, allowing it to be faintly visible to the naked eye under ideal conditions. Located 335 light years away, it is approaching the Sun with a heliocentric radial velocity of −36 km/s.
References
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- ↑ Gontcharov, G. A. (2006). "Pulkovo compilation of radial velocities for 35495 stars in a common system". Astronomy Letters . 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
- 1 2 3 4 Gaia Collaboration (2022). "VizieR Online Data Catalog: Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)". Astronomy and Astrophysics. Bibcode:2022yCat.1355....0G.
- ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 255204555.
- 1 2 3 4 Paegert, Martin; Stassun, Keivan G.; Collins, Karen A.; Pepper, Joshua; Torres, Guillermo; Jenkins, Jon; Twicken, Joseph D.; Latham, David W. (2021). "TESS Input Catalog versions 8.1 and 8.2: Phantoms in the 8.0 Catalog and How to Handle Them". arXiv: 2108.04778 [astro-ph.EP].