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Chi1 Sagittarii (χ1 Sagittarii) is a binary star system in the zodiac constellation of Sagittarius. The pair have a combined apparent visual magnitude of +5.03, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 12.95 mas as seen from Earth, it is located around 252 light years from the Sun. It is advancing through space in the general direction of the Earth with a radial velocity of −43.4 km/s.
24 Cancri is a triple star system in the constellation Cancer. The system is located about 260 light-years away, based on its parallax. The system has a combined apparent magnitude of 6.91.
Theta Pictoris is a star in the Pictor constellation.
HD 72108 is a star system in the constellation Vela. It is approximately 1640 light years from Earth.
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 31093 is a binary star system in the constellation Caelum. With a radial velocity of 23 km/s, it's drifting away from the Solar System. HD 31093 is roughly 268 light years distant based on parallax.
28 Aquarii is a single star located about 560 light years away from the Sun in the zodiac constellation of Aquarius. 28 Aquarii is the Flamsteed designation. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.6. This object is moving further from the Earth with a heliocentric radial velocity of +8.1 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.
HD 72561 is a star in the constellation Hydra. Its apparent magnitude is 5.867. Based on parallax shift, it is located about 1,600 light-years away.
ADS 48 is a multiple star system in the constellation of Andromeda consisting of 7 stars. The components, in order from A to G, have apparent visual magnitudes of 8.826, 8.995, 13.30, 12.53, 11.68, 9.949, and 13.00.
HD 120987 is a star system located in the constellation Centaurus. HD 120987 is a quintuple star system located 50 pc from the Sun. The system has an apparent magnitude of 5.565. Based on the system's parallax, it is located some 172 light-years away.
x2 Centauri is a star located in the constellation Centaurus. It is also known by its designations HD 108114 and HR 4724. The apparent magnitude of the star is about 5.7, meaning it is only visible to the naked eye under excellent viewing conditions. Its distance is about 440 light-years, based on its parallax measured by the Hipparcos astrometry satellite.
Pi Chamaeleontis, its name Latinized from π Chamaeleontis, is a binary star system located in the southern circumpolar constellation of Chamaeleon. It is dimly visible to the naked eye with an apparent visual magnitude of 5.64. Parallax measurements by Hipparcos put the system approximately 135 light-years away. It is drifting closer with a radial velocity of −10 km/s.
LS Canis Majoris is an eclipsing binary star located around 1018 light years from Earth in the constellation Canis Major. The apparent magnitude ranges from 5.57 to 5.6. The orbital period of binary pair and the period of light variation is 70.048 days. The component stars are blue-white giant stars of spectral types B2III or IV and B3III or IV respectively.
Psi1 Piscium is a binary star in the constellation Pisces. It is approximately 280 light years from Earth, based on its parallax.
HD 96819 is a single star in the equatorial constellation of Hydra. It was formerly known by its designation 10 Crateris, but that name fell into disuse after constellations were redrawn and the star was no longer in Crater. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.43. Parallax measurements put it at a distance of 182 light years away from the Sun. This is most likely a member of the TW Hydrae association.
Mu2 Octantis (μ2 Oct) is a binary star system of two G-type main-sequence stars. It shares the designation μ with μ1 Octantis, from which it is separated by 50 arcminutes.
57 Persei, or m Persei, is a suspected triple star system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08. The annual parallax shift of 16.90 mas provides a distance estimate of about 193 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).
Gliese 251, also known as HIP 33226 or HD 265866, is a star located about 18 light years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.
References
- 1 2 3 4 5 6 7 8 9 10 Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
- 1 2 3 "HD 99922". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 20 February 2017.
- ↑ Nicolet, B. (1964). "Catalogue of homogeneous data in the UBV photoelectric photometric system". Astronomy and Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N.
- ↑ Kharchenko, N. V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv: 0705.0878 . Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. S2CID 119323941.
- ↑ van Leeuwen, F. (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.
- ↑ "HD 99922A". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 20 February 2017.
- 1 2 "HD 99922B". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 20 February 2017.
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