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Krüger 60 is a binary star system located 13.1 light-years from the Sun. These red dwarf stars orbit each other every 44.6 years.
HD 2638 is a ternary star system system in the equatorial constellation of Cetus. The pair have an angular separation of 0.53″ along a position angle of 166.7°, as of 2015. This is system too faint to be visible to the naked eye, having a combined apparent visual magnitude of 9.44; a small telescope is required. The distance to this system is 179.5 light years based on parallax, and it is drifting further away with a radial velocity of +9.6 km/s. The magnitude 7.76 star HD 2567 forms a common proper motion companion to this pair at projected separation 839″.
HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 137 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.
HD 175740 is a single star in the northern constellation of Lyra. This object has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.46. It is located at a distance of approximately 266 light years from the Sun based on parallax, and has an absolute magnitude of 0.89. The star is drifting closer with a radial velocity of −9.5 km/s, and is predicted to come as close as 31.7 light-years in around 8 million years.
HD 111232 is a star in the southern constellation of Musca. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 7.59. The distance to this star is 94.5 light years based on parallax. It is drifting away from the Sun with a radial velocity of +104 km/s, having come to within 14.1 light-years some 264,700 years ago. The absolute magnitude of this star is 5.25, indicating it would have been visible to the naked eye at that time.
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 15115 is a single star in the equatorial constellation of Cetus. It is readily visible in binoculars or a small telescope, but is considered too dim to be seen with the naked eye at an apparent visual magnitude of 6.76. The distance to this object is 160 light years based on parallax, and it is slowly drifting further away at the rate of about 1 km/s. It has been proposed as a member of the Beta Pictoris moving group or the Tucana-Horologium association of co-moving stars; there is some ambiguity as to its true membership.
HD 190984, also known as HIP 99496, is a star located in the southern circumpolar constellation Pavo, the peacock. It has an apparent magnitude of 8.76, making it readily visible in small telescopes, but not to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 486 light years away from the Solar System. It appears to be receding with a heliocentric radial velocity of 20.3 km/s.
HD 220689 is a single star in the equatorial constellation of Aquarius. It is a challenge to view with the naked eye, having an apparent visual magnitude of +7.74, but is readily viewed with a pair of binoculars. The star is located at a distance of 153 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +12 km/s. A survey in 2015 has ruled out the existence of any additional stellar companions at projected distances from 26 to 305 astronomical units.
HD 162826 is a star in the constellation Hercules. It is about 110 light-years away from Earth. With an apparent magnitude of 6.55, the star can be found with binoculars or a low-power telescope by reference to nearby Vega in the constellation Lyra.
2 Piscis Austrini, also known as HD 200763 or simply 2 PsA, is a solitary orange hued star located in the southern constellation Microscopium. It was once part of Piscis Austrinus, the southern fish. The object has an apparent magnitude of 5.2, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia satellite, it is estimated to be 354 light years away from the Solar System. However, it is receding with a poorly constrained heliocentric radial velocity of 3.1 km/s. At its current distance, 2 PsA's brightness is diminished by 0.11 magnitudes due to interstellar dust. It has an absolute magnitude of 0.19.
HD 9986 is a Sun-like star in the equatorial constellation of Pisces. With an apparent visual magnitude of 6.77, it lies below the normal limit for visibility with the naked eye. The star is located at a distance of 83 light years from the Sun as determined from parallax measurements, but it is drifting closer with a radial velocity of −21 km/s.
Kepler-21, also known as HD 179070, is a star with a closely orbiting exoplanet in the northern constellation of Lyra. At an apparent visual magnitude of 8.25 this was the brightest star observed by the Kepler spacecraft to host a validated planet until the discovery of an exoplanet orbiting HD 212657 in 2018. This system is located at a distance of 354 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −18.2 km/s.
HD 186302 is a star in the constellation of Pavo. It is 185 light-years away from Earth, with an apparent magnitude of 8.76. It was identified in November 2018 as a potential solar sibling to the Sun. Similar in spectrum and size, it was suspected to have formed in the same stellar nursery as the Sun 4.6 billion years ago. However, a common origin with the Sun was found to be unlikely in a 2019 paper, as HD 186302's galactic orbit is very different from the Sun's.
HD 193307 is the primary of a binary star located the southern constellation Telescopium. It has an apparent magnitude of 6.27, placing it near the limit for naked eye visibility, even under ideal conditions. The star is located relatively close at a distance of 102 light years based on Gaia DR3 parallax measurements, but it is receding with a heliocentric radial velocity of 16.9 km/s. At its current distance, HD 193307's brightness is diminished by 0.18 magnitudes due to extinction from interstellar dust and it has an absolute magnitude of +3.80. HD 193307 has a relatively high proper motion, moving at a rate of 437 mas/yr.
HD 42618 is a well-studied star with an exoplanetary companion in the equatorial constellation of Orion. With an apparent visual magnitude of 6.85 it is too faint to be readily visible to the naked eye. This system is located at a distance of 79.6 light years from the Sun based on parallax measurements. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.321″ per year. HD 42618 is drifting closer with a radial velocity of −53.5 km/s and is predicted to come as near as 42.6 light-years in around 297,000 years.
HD 198716, also known as HR 7987 or 33 G. Microscopii, is a solitary star located in the southern constellation Microscopium. Eggen (1993) lists it as a member of the Milky Way's old disk population.
HD 22764, also known as HR 1112, is an orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.78, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of approximately 1,770 light years based on Gaia DR3 parallax measurements but is approaching the Solar System with a heliocentric radial velocity of −12.5 km/s. At its current distance, HD 22764's brightness is diminished by 0.66 magnitudes due to interstellar dust.
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.
HD 101917, also designated as HR 4509, or rarely 34 G. Chamaeleontis, is a solitary star located in the southern circumpolar constellation Chamaeleon. It has an apparent magnitude of 6.38, placing it near the limit for naked eye visibility. The object is located relatively close at a distance of 185 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 33 km/s. At its current distance, HD 101917's brightness is diminished by 0.28 magnitudes due to interstellar dust. It has an absolute magnitude of +2.69.
References
- 1 2 Ramírez, I.; Bajkova, A. T.; et al. (June 2014). "Elemental Abundances of Solar Sibling Candidates". The Astrophysical Journal . 787 (2): 154. arXiv: 1405.1723 . Bibcode:2014ApJ...787..154R. doi:10.1088/0004-637X/787/2/154.
- ↑ Adibekyan, V.; de Laverny, P.; et al. (November 2018). "The AMBRE project: searching for the closest solar siblings". Astronomy & Astrophysics . 619: A130. arXiv: 1810.01813 . Bibcode:2018A&A...619A.130A. doi:10.1051/0004-6361/201834285.
- ↑ Martínez-Barbosa, C. A.; Brown, A. G. A.; et al. (March 2016). "The evolution of the Sun's birth cluster and the search for the solar siblings with Gaia". Monthly Notices of the Royal Astronomical Society . 457 (1): 1062–1075. arXiv: 1601.00447 . Bibcode:2016MNRAS.457.1062M. doi: 10.1093/mnras/stw006 .
- ↑ Webb, Jeremy J.; Price-Jones, Natalie; et al. (May 2020). "Searching for solar siblings in APOGEE and Gaia DR2 with N-body simulations". Monthly Notices of the Royal Astronomical Society . 494 (2): 2268–2279. arXiv: 1910.01646 . Bibcode:2020MNRAS.494.2268W. doi: 10.1093/mnras/staa788 .
- ↑ "Kepler-1974". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 11 January 2025.
- ↑ Bouma, L. G.; Kerr, R.; et al. (November 2022). "Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association". The Astronomical Journal . 164 (5): 215. arXiv: 2205.01112 . Bibcode:2022AJ....164..215B. doi: 10.3847/1538-3881/ac93ff .
- ↑ de la Fuente Marcos, C.; de la Fuente Marcos, R. (October 2019). "Comet C/2018 V1 (Machholz-Fujikawa-Iwamoto): dislodged from the Oort Cloud or coming from interstellar space?". Monthly Notices of the Royal Astronomical Society . 489 (1): 951–961. arXiv: 1908.02666 . Bibcode:2019MNRAS.489..951D. doi: 10.1093/mnras/stz2229 .