Luyten 726-8

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Luyten 726-8 A/B
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus
Luyten 726-8A (BL Ceti)
Right ascension 01h 39m 01.54s[1]
Declination –17° 57′ 01.8″[1]
Apparent magnitude (V) 12.7[1]
Luyten 726-8B (UV Ceti)
Right ascension 01h 39m 01.54s[2]
Declination –17° 57′ 01.8″[2]
Apparent magnitude (V) 13.2[2]
Characteristics
Spectral type M5.5 V + M6 V
U−B color index 1.10/?
B−V color index 1.87/?
Variable type UV Cet[3]/UV Cet[4]
Astrometry
Radial velocity (Rv) +29.0 km/s
Proper motion (μ) RA: 3321 mas/yr
Dec.: 562 mas/yr
Parallax (π) 373.70 ± 2.70[5] mas
Distance 8.73 ± 0.06 ly
(2.68 ± 0.02 pc)
Orbit[6]
Companion Luyten 726-8 B
Period (P) 26.52 yr
Semi-major axis (a) 1.95"
Eccentricity (e) 0.62
Inclination (i) 127.3°
Longitude of the node (Ω) 150.5°
Periastron epoch (T) 1971.91
Argument of periastron (ω)
(secondary)
285.3°
Details
Luyten 726-8 A
Mass 0.102 ± 0.010[7] M
Radius 0.14 R
Luminosity 0.00006 L
Temperature 2,670 K
Luyten 726-8 B
Mass 0.100 ± 0.010[7] M
Radius 0.14 R
Luminosity 0.00004 L
Other designations
BL Ceti/UV Ceti, GCTP 343.10 A/B, LHS 9/10, GJ 65 A/B
Database references
SIMBAD data

Luyten 726-8 (also known as Gliese 65) is a binary star system that is one of Earth's nearest neighbors, at about 8.7 light years from Earth in the constellation Cetus. Luyten 726-8B is also known under the variable star designation UV Ceti, being the archetype for the class of flare stars.

Star system[edit]

The star system was discovered in 1948 by Willem Jacob Luyten in the course of compiling a catalog of stars of high proper motion; he noted its exceptionally high proper motion of 3.37 arc seconds annually and cataloged it as Luyten 726-8.[8] The two stars are of nearly equal brightness, with visual magnitudes of 12.7 and 13.2 as seen from Earth. They orbit one another every 26.5 years. The distance between the two stars varies from 2.1 to 8.8 astronomical units (310 to 1,320 Gm). The Luyten 726-8 system is approximately 2.63 parsecs (8.58 ly) from Earth's Solar System, in the constellation Cetus, and is thus the seventh-closest star system to Earth. Its own nearest neighbor is Tau Ceti, 0.88 pc (2.87 ly) away from it. If R_v=+29 km/s then approximately 28,700 years ago Luyten 726-8 was at its minimal distance of 2.21 pc (7.2 ly) from the Sun.[9]

Luyten 726-8 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Woolley et al. (1970) 367 ± 9 2.72 ± 0.07 8.89+0.22
−0.21
[10]
Gliese & Jahreiß (1991) 380.7 ± 4.3 2.627+0.03
−0.029
8.57 ± 0.1 [11]
van Altena et al. (1995) 373.7 ± 2.7 2.676 ± 0.019 8.73 ± 0.06 [5]
RECONS TOP100 (2012) 373.7 ± 2.7[nb 1] 2.676 ± 0.019 8.73 ± 0.06 [12]

Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.

Luyten-726-8A was found to be a variable star and given the variable star designation BL Ceti.[3] It is a red dwarf of spectral type M5.5e. It is also a flare star, and classified as a UV Ceti variable type, but it is not nearly as remarkable or extreme in its behavior as its companion star UV Ceti. BL Ceti is also known as G 272-061.[1]

UV Ceti by Andrew Posa (1982)

Soon after[when?] the discovery of Luyten 726-8A, the companion star Luyten 726-8B was discovered. Like Luyten 726-8A, this star was also found to be variable and given the variable star designation UV Ceti.[4] Although UV Ceti was not the first flare star discovered, it is the most prominent example of such a star, so similar flare stars are now classified as UV Ceti type variable stars. This star goes through fairly extreme changes of brightness: for instance, in 1952, its brightness increased by 75 times in only 20 seconds. UV Ceti is a red dwarf of spectral type M6.0e.[2]

In approximately 31,500 years, Luyten 726-8 will have a close encounter with Epsilon Eridani at the minimal distance of about 0.93 ly. Luyten 726-8 can penetrate a conjectured Oort cloud about Epsilon Eridani, which may gravitationally perturb some long-period comets. The duration of mutual transit of two star systems within 1 ly from each other is about 4,600 years.[13]

Luyten 726-8 is a possible member of the Hyades Stream.[14]

See also[edit]

References[edit]

  1. ^ a b c d "V* BL Cet -- Flare Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16. 
  2. ^ a b c d "V* UV Cet -- Flare Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16. 
  3. ^ a b "Query= BL Cet". General Catalogue of Variable Stars. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16. 
  4. ^ a b "Query= UV Cet". General Catalogue of Variable Stars. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16. 
  5. ^ a b Van Altena W. F., Lee J. T., Hoffleit E. D. (1995). "GCTP 343.1". The General Catalogue of Trigonometric Stellar Parallaxes, Fourth Edition. Retrieved 2014-06-05. 
  6. ^ Geyer, David W.; Harrington, Robert S.; Worley, Charles E. (June 1988), "Parallax, orbit, and mass of the visual binary L726-8", Astronomical Journal 95: 1841–1842, Bibcode:1988AJ.....95.1841G, doi:10.1086/114781 
  7. ^ a b Delfosse, X. et al. (December 2000), "Accurate masses of very low mass stars. IV. Improved mass-luminosity relations", Astronomy and Astrophysics 364: 217–224, arXiv:astro-ph/0010586, Bibcode:2000A&A...364..217D 
  8. ^ Luyten, W. J. (December 1949). "New stars with proper motions exceeding 0.5" annually.". The Astronomical Journal 55: 15. Bibcode:1949AJ.....55...15L. doi:10.1086/106322. 
  9. ^ "Annotations on V* UV Cet object". Centre de Données astronomiques de Strasbourg. Retrieved 2010-04-14. 
  10. ^ Woolley R.; Epps E. A.; Penston M. J.; Pocock S. B. (1970). "Woolley 65". Catalogue of stars within 25 parsecs of the Sun. Retrieved 2014-06-05. 
  11. ^ Gliese, W. and Jahreiß, H. (1991). "Gl 65". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 2014-06-05. 
  12. ^ "RECONS TOP100". THE ONE HUNDRED NEAREST STAR SYSTEMS brought to you by RECONS (Research Consortium On Nearby Stars). 2012. Retrieved 2014-06-05. 
  13. ^ Potemine, Igor Yu. (April 2010). "Transit of Luyten 726-8 within 1 ly from Epsilon Eridani". Cornell University Library. Retrieved 2010-04-12. 
  14. ^ D. Montes et al. (2001). "Late-type members of young stellar kinematic groups - I. Single stars.". MNRAS (328): 45–63. Retrieved 2010-04-18. 

Notes[edit]

  1. ^ Parallax from van Altena et al. (1995).

Further reading[edit]

External links[edit]