Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Orion |
Right ascension | 05h 36m 30.991s [2] |
Declination | +11° 19′ 40.33″ [2] |
Apparent magnitude (V) | 8.80 - 9.05 [3] |
Characteristics | |
Spectral type | M0.0 Ve [4] |
Variable type | RS CVn [3] |
Astrometry | |
Radial velocity (Rv) | 21.772 [5] km/s |
Proper motion (μ) | RA: −2.811 ± 0.080 [2] mas/yr Dec.: −56.368 ± 0.060 [2] mas/yr |
Parallax (π) | 87.66 ± 0.29 mas [2] |
Distance | 37.2 ± 0.1 ly (11.41 ± 0.04 pc) |
Absolute magnitude (MV) | 8.6 |
Details | |
Mass | 0.646 [6] M☉ |
Radius | 0.601 [6] R☉ |
Luminosity | 0.08 [7] L☉ |
Temperature | 3,966 [6] K |
Metallicity [Fe/H] | +0.05 [6] dex |
Age | 2.7 [6] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
Gliese 208 (Gj 208) is a red dwarf star with an apparent magnitude of 8.9. It is 37 light years away in the constellation of Orion. It is an extremely wide binary with 2MASS J0536+1117, an M4 star 2.6 arcminutes away (at least 0.028 light years)
The spectral type of Gj 208 has variously been described between K6 and M1. [8] [9] [10] Two of the most recent observations give a statistically calculated spectral type of K7.9 [6] or a more traditional classification of M0.0 Ve. [4] It is a cool dwarf star and probably a spectroscopic binary. [3]
Calculations from 2010 suggest that this star passed as close as 1.537 parsecs (5.0 light-years) from the Sun about 500,000 years ago. [11]
GJ 208 is an RS Canum Venaticorum variable, close binary systems which show small amplitude brightness changes caused by chromospheric activity. Its visual magnitude varies by about a quarter magnitude with a period of 12.285 days. [3]
Ross 248, also called HH Andromedae or Gliese 905, is a small star approximately 10.30 light-years from Earth in the northern constellation of Andromeda. Despite its proximity it is too dim to be seen with the naked eye. It was first catalogued by Frank Elmore Ross in 1926 with his second list of proper-motion stars; on which count it ranks 261st in the SIMBAD database. It was too dim to be included in the Hipparcos survey. In about 40,000 years, Voyager 2 will pass 1.7 light-years from the star.
9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.
UW Canis Majoris is a star in the constellation Canis Major. It is classified as a Beta Lyrae eclipsing contact binary and given the variable star designation UW Canis Majoris. Its brightness varies from magnitude +4.84 to +5.33 with a period of 4.39 days. Bode had initially labelled it as Tau2 Canis Majoris, but this designation had been dropped by Gould and subsequent authors.
Gliese 105 is a triple star system in the constellation of Cetus. It is located relatively near the Sun at a distance of 23.6 light-years. Despite this, even the brightest component is barely visible with the unaided eye (see Bortle scale). No planets have yet been detected around any of the stars in this system.
HD 83944 is a star system in the constellation Carina. This has the Bayer designation m Carinae, while HD 83944 is the identifier from the Henry Draper catalogue. It is a suspected variable with an apparent visual magnitude that fluctuates around 4.51 with an amplitude of 0.5. The system is located at a distance of approximately 226 light years from the Sun based on parallax, and it has an absolute magnitude of 0.31. It is a member of the Carina association of co-moving stars.
GJ 1245 is a double star with components G 208-44 and G 208-45, 14 light-years away, relatively close to the Solar System. G 208-44 is itself a closer double star made up of two red dwarfs, while G 208-45 is also a red dwarf. GJ 1245 is the 37th closest stellar system to the Solar System, located in the constellation Cygnus. GJ 1245 A and B are active flare stars, and the pair are collectively designated V1581 Cygni.
Gliese 445 is an M-type main sequence star in the northern part of the constellation Camelopardalis.
R Arae is an Algol-type eclipsing binary in the constellation Ara. Located approximately 298 parsecs (970 ly) distant, it normally shines at magnitude 6.17, but during eclipses can fall as low as magnitude 7.32. It has been suggested by multiple studies that mass transfer is occurring between the two stars of this system, and the period of eclipses seems to be increasing over time. The primary is a blue-white main sequence star of spectral type B5V that is 5 times as massive as the Sun, while the secondary is a yellow-white star of spectral type F1IV that is 1.5 times as massive as the Sun. Stellar material is being stripped off the secondary and accreting on the primary.
V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.
QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.
42 Persei is a binary star system in the northern constellation of Perseus. It has the Bayer designation n Persei, while 42 Persei is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.11. It is located around 93 parsecs (302 ly) distant from the Sun, but is drifting closer with a radial velocity of −12.4 km/s.
21 Persei is a single, variable star in the northern constellation of Perseus, located about 331 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.10 km/s. The object is moving further from the Earth with a heliocentric radial velocity of +8.5 km/s. It has the variable star designation LT Persei; 21 Persei is the Flamsteed designation.
31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, ο2 Cygni or V695 Cygni, is a ternary star system about 750 light years away in the constellation Cygnus.
Gliese 908 is a red dwarf star, located in constellation Pisces at 19.3 light-years from Earth. It is a BY Draconis variable star with a variable star designation of BR Piscium. Its apparent magnitude varies between magnitude 8.93 and magnitude 9.03 as a result of starspots and varying chromospheric activity.
ADS 7251 is a binary star system 6.33 parsecs from the Sun. The components are near-identical red dwarfs separated by 17″ in 2019.
EQ Pegasi is a nearby binary system of two red dwarfs. Both components are flare stars, with spectral types of M4Ve and M6Ve respectively, and a current separation between the components of 5.8 arcseconds. The system is at a distance of 20.4 light-years, and is 950 million years old. The primary star is orbited by one known exoplanet.
Gliese 402 is a star located 22.7 light years from the Solar System. Located in the constellation of Leo, it is also known as Wolf 358 from its entry in Max Wolf's star catalogue. The stars nearest to Gliese 402 are Gliese 393, at 3.43 light years, Gliese 408, at 6.26 light years, and Gliese 382 at 6.66 light years.
XX Pyxidis is a star located in the constellation Pyxis. It has an apparent magnitude that varies slightly at about 11.5, and is about 2,300 light years away.
DH Tauri, also known as DH Tau, is a type M star, located 140 parsecs away. It forms a binary system with DI Tauri 15″ away, and has a substellar companion, either a brown dwarf or massive exoplanet.
Gliese 569 is a ternary star system composed of a main-sequence star orbited by a pair of brown dwarfs in the constellation of Boötes about 32 light years away.