Gliese 208

Last updated
Gliese 208
V2689OriLightCurve.png
A visual band light curve for V2689 Orionis, adapted from Kiraga (2012) [1]
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 [2]   mas
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
Gliese  208, Gj 208, V2689  Orionis, BD+11°878, HIP  26335, HD  245409, TYC  709-63-1, SAO  94695
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]

Related Research Articles

Struve 2398 is a binary star system in the northern constellation of Draco. Struve 2398 is star number 2398 in the Struve Double Star Catalog of Baltic-German astronomer Friedrich Georg Wilhelm von Struve. The astronomer's surname, and hence the star identifier, is sometimes indicated by a Greek sigma, Σ. Although the components are too faint to be viewed with the naked eye, this star system is among the closest to the Sun. Parallax measurements by the Hipparcos spacecraft give them an estimated distance of about 11.6 light years away.

Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge. Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years from the Sun. This positions the pair among the nearest stars to the Solar System.

Gliese 674(GJ 674) is a small red dwarf star with an exoplanetary companion in the southern constellation of Ara. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.38 and an absolute magnitude of 11.09. The system is located at a distance of 14.8 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −2.9 km/s. It is a candidate member of the 200 million year old Castor stream of co-moving stars.

6 Andromedae is an astrometric binary star system in the northern constellation of Andromeda. The designation comes from the star catalogue of John Flamsteed, first published in 1712. Its apparent visual magnitude is 5.91, which is just bright enough to be visible to the naked eye under good seeing conditions. Based upon an annual parallax shift of 34.1 mas as seen from Earth, it is around 96 light years from the Sun. It is moving closer to the Sun with a radial velocity of −32.4 km/s. The system has a relatively high proper motion, advancing across the celestial sphere at the rate of 0.272 arc seconds per annum.

Gliese 105 Triple star system in the constellation Cetus

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.

Zeta Cephei Star in the constellation Cepheus

Zeta Cephei is a star in the constellation of Cepheus. Zeta Cephei marks the left shoulder of Cepheus, the King of Joppa (Ethiopia). It is one of the fundamental stars of the MK spectral sequence, defined as type K1.5 Ib.

GJ 1245 Triple star system in the constellation Cygnus

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.

Theta Persei Star in the constellation Perseus

Theta Persei is a star system 37 light years away from Earth, in the constellation Perseus. It is one of the closest naked-eye stars.

Gliese 412 is a pair of stars that share a common proper motion through space and are thought to form a binary star system. The pair have an angular separation of 31.4″ at a position angle of 126.1°. They are located 15.8 light-years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.

Gliese 445 Star in the constellation Camelopardalis

Gliese 445 is an M-type main sequence star in the northern part of the constellation Camelopardalis.

R Arae Variable star in the constellation Ara

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.

Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of about 19 light years. This system consists of two M-type stars. The primary star is the magnitude 9 Gliese (GJ) 752 A. The secondary star is the dim magnitude 17 Gliese (GJ) 752 B, more commonly referred to as VB 10. This stellar pair form a binary star system separated by about 74 arc seconds. This system is also known for its high proper motion of about 1 arc second a year.

Sigma Coronae Borealis Star in the constellation Corona Borealis

Sigma Coronae Borealis is a star system in the constellation of Corona Borealis. It is a quintuple star system containing three sunlike main-sequence stars and two other low-mass stars. The combined visual magnitude is 5.3 and the system lies 74 light years from Earth. σ CrB A is the variable star TZ Coronae Borealis.

Gliese 205 is a nearby red dwarf star of spectral type M1.5, located in constellation Orion at 18.45 light-years from Earth.

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 Star system in the constellation Pegasus

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.

Gliese 402 Star in the constellation Leo

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.

Gliese 54 is a star near the Solar System located at 25.7 light years away. It is located in the constellation of Tucana, close to the edge, almost in the neighboring Hydrus. It is below the threshold brightness to be observable eye with an apparent magnitude of +9.80,.

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.

References

  1. ↑ Kiraga, M. (March 2012). "ASAS Photometry of ROSAT Sources. I. Periodic Variable Stars Coincident with Bright Sources from the ROSAT All Sky Survey". Acta Astronomica. 62 (1): 67–95. arXiv: 1204.3825 . Bibcode:2012AcA....62...67K . Retrieved 10 February 2022.
  2. 1 2 3 4 5 Gaia Collaboration (2016). "VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016)". VizieR On-line Data Catalog: I/337. Originally Published in: Astron. Astrophys. 1337. Bibcode:2016yCat.1337....0G.
  3. 1 2 3 4 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. 1 2 Lépine, Sébastien; Hilton, Eric J.; Mann, Andrew W.; Wilde, Matthew; Rojas-Ayala, Bárbara; Cruz, Kelle L.; Gaidos, Eric (2013). "A Spectroscopic Catalog of the Brightest (J < 9) M Dwarfs in the Northern Sky". The Astronomical Journal. 145 (4): 102. arXiv: 1206.5991 . Bibcode:2013AJ....145..102L. doi:10.1088/0004-6256/145/4/102. S2CID   117144290.
  5. ↑ Soubiran, C.; Jasniewicz, G.; Chemin, L.; Crifo, F.; Udry, S.; Hestroffer, D.; Katz, D. (2013). "The catalogue of radial velocity standard stars for Gaia. I. Pre-launch release". Astronomy & Astrophysics. 552: A64. arXiv: 1302.1905 . Bibcode:2013A&A...552A..64S. doi:10.1051/0004-6361/201220927. S2CID   56094559.
  6. 1 2 3 4 5 6 Mann, Andrew W.; Feiden, Gregory A.; Gaidos, Eric; Boyajian, Tabetha; von Braun, Kaspar (2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius". The Astrophysical Journal. 804 (1): 64. arXiv: 1501.01635 . Bibcode:2015ApJ...804...64M. doi:10.1088/0004-637X/804/1/64. S2CID   19269312.
  7. ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental parameters and infrared excesses of Hipparcos stars". Monthly Notices of the Royal Astronomical Society. 427 (1): 343–357. arXiv: 1208.2037 . Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x. S2CID   118665352.
  8. ↑ Stephenson, C. B. (1986). "Dwarf K and M stars of high proper motion found in a hemispheric survey". Astronomical Journal. 92: 139. Bibcode:1986AJ.....92..139S. doi:10.1086/114146.
  9. ↑ Stephenson, C. B.; Sanduleak, N. (1975). "Dwarf K and M stars discovered on objective-prism plates". Astronomical Journal. 80: 972. Bibcode:1975AJ.....80..972S. doi:10.1086/111829.
  10. ↑ Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)". VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014). 1. Bibcode:2014yCat....1.2023S.
  11. ↑ Bobylev, Vadim V. (March 2010). "Searching for Stars Closely Encountering with the Solar System". Astronomy Letters. 36 (3): 220–226. arXiv: 1003.2160 . Bibcode:2010AstL...36..220B. doi:10.1134/S1063773710030060. S2CID   118374161.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.