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Chi Scorpii, Latinized from χ Scorpii, is a single star in the zodiac constellation of Scorpius. It has an orange hue and can be faintly seen with the naked eye with an apparent visual magnitude of 5.24. Based upon parallax measurements, this star is around 448 light years from the Sun. The star is drifting closer with a radial velocity of −23.6 km/s.
Psi Virginis is a suspected binary star system in the zodiac constellation of Virgo. It can be seen with the naked eye and has an apparent visual magnitude of about 4.8. Based upon the annual parallax shift of 5.99 milliarcseconds, the distance to this star is roughly 540 light years. The angular size of Psi Virginis was measured on December 26, 1975 during an occultation by the Moon, yielding the estimate 6.5±0.3 mas.
Omega Virginis is a solitary star in the zodiac constellation Virgo. It has an apparent visual magnitude of +5.2, which is bright enough to be faintly visible to the naked eye. Based upon an annual stellar parallax shift of 6.56 milliarcseconds, it is located about 500 light years from the Sun.
Eta Volantis, Latinized from η Volantis, is a single star in the southern constellation of Volans. It has an apparent visual magnitude of 5.28, which is bright enough to be seen with the naked eye as a dim, white-hued star. Based upon parallax measurements, it is approximately 387 light years from the Sun. The star is moving further away from the Sun with a radial velocity of 20 km/s.
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.
HD 180262 is a wide double star in the equatorial constellation of Aquila. The pair have an angular separation of 89.823″.
HD 36678 is single star in the northern constellation of Auriga. This star is dimly visible to the naked eye with an apparent visual magnitude of 5.83. It is located at a distance of approximately 840 light years from the Sun based on parallax.
Beta Equulei, Latinized from β Equulei, is the Bayer designation for a solitary star in the northern constellation of Equuleus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.16. The annual parallax shift is 11.27 mas, indicating a separation of around 289 light years from the Sun. It is drifting closer with a radial velocity of −11 km/s.
HD 118508 is a suspected variable star in the northern constellation of Boötes. Its apparent magnitude may vary with an amplitude of 0.04, discovered during a search for small-amplitude red variables. It is a red giant about 552 light years away.
HD 112028 is an evolved star in the northern constellation of Camelopardalis. It has spectral peculiarities that have been interpreted as a shell, and also relatively weak magnesium and silicon lines. Its spectral class has been variously assigned between B9 and A2, and its luminosity class between a subgiant and bright giant.
HD 30442 is a solitary star in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye with an apparent magnitude of 5.47 and is estimated to be 403 light years away from the Solar System. The object has a heliocentric radial velocity of −37 km/s, indicating that it is drifting closer.
56 Ceti is a single star located in the equatorial constellation of Cetus. Not found in the original Bayer catalogue, it was given the Bayer-like designation Upsilon1 Ceti by Flamsteed to distinguish it from Bayer's Upsilon Ceti, which Flamsteed designated Upsilon2 or 59 Ceti. In 1801, J. E. Bode included this designation in his Uranographia, but the superscripted designations Upsilon1 and Upsilon2 are not in general use today. 56 Ceti is the Flamsteed designation for this star.
χ Eridani is a binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.70. The distance to this system, as determined using the parallax method, is around 58 light years. The pair had an angular separation of 5.0 arcseconds as of 1994. This corresponds to a projected separation of around 128 AU.
54 Eridani is a suspected astrometric binary star system located around 400 light years from the Sun in the equatorial constellation of Eridanus. It is visible to the naked eye as a faint, reddish hued star with a baseline apparent visual magnitude of 4.32. The object is moving closer to the Earth with a heliocentric radial velocity of −33 km/s.
45 Eridani is a single star located around 700 light years away from the Sun in the equatorial constellation of Eridanus. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.91. This body is moving away from the Earth with a heliocentric radial velocity of +15 km/s.
Pi Leonis, Latinised from π Leonis, is a single star in the zodiac constellation Leo. It is a red-hued star that is visible to the naked eye with an apparent visual magnitude of 4.70. This object is located at a distance of some 410 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s. Because the star lies near the ecliptic it is subject to occultations by the Moon.
59 Serpentis, also known as d Serpentis, is a multiple star in the constellation Serpens. The system shows irregular variations in brightness between magnitudes 5.17 and 5.29.
77 Ceti is a single, orange-hued star located 489 light years away in the equatorial constellation of Cetus. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.7. This is an evolved giant star with a stellar classification of K2 III. It is radiating 187 times the Sun's luminosity from its photosphere at an effective temperature of 4,206 K.
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 4222, also known as HR 196, is the primary of a binary star located in the northern constellation Cassiopeia. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.41. Gaia DR3 parallax measurements imply a distance of 353 light-years and it is drifting closer with a heliocentric radial velocity of −8.5 km/s. At its current distance, HD 4222's brightness is diminished by an interstellar extinction of 0.13 magnitudes and it has an absolute magnitude of +0.44.
References
- 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID 244398875. Gaia DR3 record for this source at VizieR.
- 1 2 3 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. SIMBAD. Bibcode:1986EgUBV........0M.
- 1 2 3 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.
- 1 2 Abt, Helmut A. (2008). "Visual Multiples. IX. MK Spectral Types". The Astrophysical Journal Supplement Series. 176 (1): 216–217. Bibcode:2008ApJS..176..216A. doi: 10.1086/525529 .
- 1 2 3 Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal. 158 (1): 20. arXiv: 1905.03744 . Bibcode:2019AJ....158...20M. doi: 10.3847/1538-3881/ab1cbd . S2CID 148571616.
- ↑ "HD 24480". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-01-25.
{{cite web}}: CS1 maint: postscript (link) - 1 2 Parsons, Sidney B. (May 2004). "New and Confirmed Triple Systems with Luminous Cool Primaries and Hot Companions". The Astronomical Journal. 127 (5): 2915–2930. Bibcode:2004AJ....127.2915P. doi: 10.1086/383546 .
