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This is a list of blue straggler stars in order of their distance from Earth. [1] [2] [3]
| | This article needs additional citations for verification .(September 2024) |
This is a list of blue straggler stars in order of their distance from Earth. [1] [2] [3]
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| Cluster and other | Stars | Star system | Median distance (ly) | Stars in system | Spectral type | Apparent magnitude (V) | Comments and references |
|---|---|---|---|---|---|---|---|
| Hyades | 5 | HD 27482 | 151 | 1 | B8V | The Closest Blue Straggler star to Earth. | |
| HD 27130 | 153 | 1 | B8V | ||||
| HD 27638 | 153 | 1 | B9.5V | ||||
| HD 28052 | 153 | 1 | B8V | ||||
| HD 283579 | 153 | 1 | B9.5V | ||||
| Coma Star Cluster | 3 | 13 Comae Berenices | 260 ± 20 | 1 | A3 V | 5.17 | |
| 14 Comae Berenices | 266 ± 5 | 1 | F0p | 4.95 | |||
| 12 Comae Berenices | 276 ± 5 | 2 | F6 III + A3 V | 4.80 | |||
| Pleiades Cluster (M45) | 3 | Maia (20 Tauri) | 380 ± 10 | 1 | B8III | 3.87 | |
| Atlas (27 Tauri) | 431 ± 13 | 1 | B8III | 3.63 | |||
| Taygeta | 440 | 2 | B6IV | 4.30 | [4] | ||
| Messier 67 (King Cobra or Golden Eye Cluster) | 3 | HD 73727 | 2,800 | 1 | B | ||
| BD+11°2661 | 2,800 | 1 | B | ||||
| HD 73684 | 2,800 | 1 | B | ||||
| NGC 6347 | 1 | HD 164278 | 4,000 | 1 | B2V | ||
| NGC 1907 | 1 | HIP 20867 | 4,400 | 1 | B9IV-V | ||
| NGC 188 (Caldwell 1, Polarissima Cluster) | 3 | 2MASS J00433286+8511080 | 5,000 | 1 | B | ||
| 2MASS J00444204+8510387 | 5,000 | 1 | B | ||||
| 2MASS J00443207+8510066 | 5,000 | 1 | B | ||||
| NGC 3201 | 2 | TYC 4299-1082-1 | 5,400 | 1 | B1V | ||
| TYC 4299-1237-1 | 5,400 | 1 | A1V | ||||
| NGC 2420 | 1 | HD 101205 | 10,000 | 1 | B | ||
| NGC 6752 | 1 | 13,000 | 1 | B | |||
| NGC 6791 | 1 | HD 187573 | 13,300 | 1 | B | ||
| 47 Tucanae | 21 | 15,000 ± 33 | 1 | B | |||
| Omega Centauri | 1 | 15,800 | 1 | B | |||
| Messier 13 (Hercules Cluster) | 1 | 22,200 | 1 | B | |||
| Messier 3 (NGC 5272) | 1 | 33,900 | 1 | B | |||
Lacaille 8760 is a red dwarf star in the constellation Microscopium. It is one of the nearest stars to the Sun at about 12.9 light-years' distance, and the brightest M-class main-sequence star in Earth's night sky, although it is generally too faint to be seen without a telescope. At an apparent magnitude of +6.7, it may only be visible to the unaided eye under exceptionally good viewing conditions, under dark skies.
60 Sagittarii is a suspected binary star system in the southern constellation of Sagittarius. It has the Bayer designation A Sagittarii, while 60 Sagittarii is the Flamsteed designation. This naked-eye object forms the northwest corner of the asterism called the Terebellum and, with an apparent magnitude of approximately 4.84, it is the dimmest of the four stars in the Terebellum. It is located 379 light-years from the Sun, based on parallax, but is moving closer with a radial velocity of −51 km/s.
47 Andromedae is a binary star system in the northern constellation of Andromeda. The designation is from the star catalogue of John Flamsteed, first published in 1712. The system has a combined apparent visual magnitude of 5.60, which is just bright enough to be faintly visible to the naked eye under good seeing conditions. The distance to this system, as determined from an annual parallax shift of 15.9805 mas, is about 204 light years. It is moving away from the Sun with a heliocentric radial velocity of +13.3 km/s.
Gliese 687, or GJ 687 (Gliese–Jahreiß 687) is a red dwarf in the constellation Draco. This is one of the closest stars to the Sun and lies at a distance of 14.84 light-years. Even though it is close by, it has an apparent magnitude of about 9, so it can only be seen through a moderately sized telescope. Gliese 687 has a high proper motion, advancing 1.304 arcseconds per year across the sky. It has a net relative velocity of about 39 km/s. It is known to have a Neptune-mass planet. Old books and articles refer to it as Argelander Oeltzen 17415.
HL Tau 76 is a variable white dwarf star of the DAV type. It was observed by G. Haro and W. J. Luyten in 1961, and was the first variable white dwarf discovered when, in 1968, Arlo U. Landolt found that it varied in brightness with a period of approximately 749.5 seconds, or 12.5 minutes. Like other DAV white dwarfs, its variability arises from non-radial gravity wave pulsations within itself., § 7. Later observation and analysis has found HL Tau 76 to pulsate in over 40 independent vibrational modes, with periods between 380 seconds and 1390 seconds.
HD 70573 is a variable star in the equatorial constellation of Hydra. At a mean apparent visual magnitude of +8.7, this yellow-hued star is too dim to be visible to the naked eye. Based upon parallax measurements, it is located at a distance of 193 light years from the Sun, and is drifting further away with a radial velocity of 20.5 km/s. It is a candidate member of the proposed Hercules-Lyra Association of co-moving stars, although this membership is disputed.
HD 220105 is a star in the northern constellation of Andromeda, and a member of the Sirius supercluster. It lies near the lower limit of visibility to the naked eye at an apparent visual magnitude of 6.24, and can be a challenge to spot under normal viewing conditions. The star is located 238 light years away, based upon an annual parallax shift of 13.78 mas. It is moving closer to the Earth with a heliocentric radial velocity of −2 km/s.
HD 16004 is blue-white hued star in the northern constellation of Andromeda. It is a challenge to see with the naked eye even under good viewing conditions, having an apparent visual magnitude of 6.26. Located approximately 660 light-years away from the Sun based on parallax, it is drifting closer with a heliocentric radial velocity of −7 km/s.
HR Carinae is a luminous blue variable star located in the constellation Carina. It is surrounded by a vast nebula of ejected nuclear-processed material because this star has a multiple shell expanding atmosphere. This star is among the most luminous stars in the Milky Way. It has very broad emission wings on the Balmer lines, reminiscent from the broad lines observed in the spectra of O and Wolf–Rayet stars. A distance of 5 kpc and a bolometric magnitude of −9.4 put HR Car among the most luminous stars of the galaxy.
2 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located around 1,800 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.43.
SU Andromedae is a carbon star in the constellation of Andromeda. It is a variable star classified as a slow irregular pulsating supergiant, and varies from an apparent visual magnitude of 8.5 at minimum brightness to a magnitude of 8.0 at maximum brightness with no clear period.
Theta2 Orionis is a multiple star system in the constellation Orion. It is a few arc minutes from its more famous neighbour the Trapezium Cluster, also known as θ1 Orionis.
23 Orionis is a double star located around 1,200 light-years away from the Sun in the equatorial constellation of Orion. It is visible to the naked eye as a dim, blue-white-hued point of light with a combined apparent visual magnitude of 4.99. The pair are moving away from the Earth with a heliocentric radial velocity of +18 km/s, and they are members of the Orion OB1 association, subgroup 1a.
HD 21278 is a binary star system in the constellation Perseus, located within the 60±7 million year old Alpha Persei Cluster. It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99. The system is located at a distance of approximately 580 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +1.20 km/s.
14 Persei is a single star in the northern constellation Perseus, located roughly 1,900 light years away from the Sun. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude is 5.43. The object is slowly moving closer to the Earth with a heliocentric radial velocity of −1.2 km/s.
HDE 316285 is a blue supergiant star in the constellation Sagittarius. It is a candidate luminous blue variable and lies about 6,000 light years away in the direction of the Galactic Center.
17 Comae Berenices is a multiple star system in the northern constellation of Coma Berenices. The brighter component, 17 Com A, is a naked eye star with an apparent visual magnitude of 5.2. It has a faint companion of magnitude 6.6, 17 Com B, positioned at an angular separation of 146.4″ along a position angle of 251°, as of 2018. They are located at a distance of approximately 240 light years from the Sun based on parallax measurements.
AF Andromedae is a luminous blue variable (LBV), a type of variable star. The star is one of the most luminous variables in M31, the Andromeda Galaxy.