Jump to content

Gliese 65

Coordinates: Sky map 01h 39m 01.54s, −17° 57′ 01.8″
From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by AstroChara (talk | contribs) at 00:10, 21 August 2023 (Stars parameter update #2). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

Luyten 726-8 A/B
Luyten 726-8 is located in the constellation Cetus.
Luyten 726-8 is located in the constellation Cetus.
     Luyten 726-8
Location of Luyten 726-8 in the constellation Cetus

Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus
Luyten 726-8 A (BL Ceti)
Right ascension 01h 39m 01.3773s[1]
Declination –17° 57′ 02.587″[1]
Apparent magnitude (V) 12.8[2]
Luyten 726-8 B (UV Ceti)
Right ascension 01h 39m 01.6377s[3]
Declination –17° 57′ 01.001″[3]
Apparent magnitude (V) 12.8[2]
Characteristics
Luyten 726-8 A (BL Ceti)
Spectral type M5.5V[4]
U−B color index 1.10
B−V color index 1.87
Variable type UV Cet[5]
Luyten 726-8 B (UV Ceti)
Spectral type M6 V[4]
Variable type UV Cet[6]
Astrometry
Luyten 726-8 A (BL Ceti)
Radial velocity (Rv)+29.0 km/s
Proper motion (μ) RA: 3385.316[1] mas/yr
Dec.: 544.386[1] mas/yr
Parallax (π)367.7119 ± 0.7418 mas[1]
Distance8.87 ± 0.02 ly
(2.720 ± 0.005 pc)
Absolute magnitude (MV)15.7[2]
Luyten 726-8 B (UV Ceti)
Proper motion (μ) RA: 3178.694[3] mas/yr
Dec.: 584.061[3] mas/yr
Parallax (π)373.8443 ± 0.5009 mas[3]
Distance8.72 ± 0.01 ly
(2.675 ± 0.004 pc)
Absolute magnitude (MV)15.7[2]
Orbit[7]
CompanionLuyten 726-8 B
Period (P)26.284±0.038 yr
Semi-major axis (a)2.0584±0.0097″
Eccentricity (e)0.6185±0.0020
Inclination (i)307.82±0.28°
Longitude of the node (Ω)145.79±0.32°
Periastron epoch (T)1972.115±0.047
Argument of periastron (ω)
(secondary)		283.27±0.21°
Details
Luyten 726-8 A
Mass0.1225±0.0043[7] M☉
Radius0.165±0.006[7] R☉
Luminosity0.00006 L☉
Surface gravity (log g)5.092±0.015[7] cgs
Temperature2,670 K
Metallicity [Fe/H]−0.03±0.20[7] dex
Rotation0.2430±0.0005 days[8]
Rotational velocity (v sin i)28.2±2[7] km/s
Luyten 726-8 B
Mass0.1195±0.0043[7] M☉
Radius0.159±0.006[7] R☉
Luminosity0.00004 L☉
Surface gravity (log g)5.113±0.015[7] cgs
Temperature2650 K
Metallicity [Fe/H]−0.12±0.20[7] dex
Rotation0.2268±0.0003 days[8]
Rotational velocity (v sin i)30.6±2[7] km/s
Other designations
GCTP 343.10, GJ 65, G 272-61
Luyten 726-8 A: BL Ceti, LHS 9
Luyten 726-8 B: UV Ceti, LHS 10
Database references
SIMBADThe system
A (BL Cet)
B (UV Cet)

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. The two component stars are both flare stars with the variable star designations BL Ceti and UV Ceti.

Star system

UV Ceti by Andrew Posa (1982)

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.[9] 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, 0.98 pc (3.20 ly) away from it. If 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.[10]

Luyten-726-8A was later found to be a variable star and given the variable star designation BL Ceti.[5] It is a red dwarf of spectral type M5.5V. 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.

An ultraviolet light curve for UV Ceti, adapted from Beskin et al. (2017).[11] The main plot shows the full flare event and the inset plot shows the time around peak brightness with an expanded time scale.

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.[6] 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 M6V.[4]

Both stars are listed as spectral standard stars for their respective classes, being considered typical examples of the classes.[4]

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.[12]

Luyten 726-8 is a possible member of the Hyades Stream.[13]

See also

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d Houdebine, Éric R.; Mullan, D. J.; Doyle, J. G.; de la Vieuville, Geoffroy; Butler, C. J.; Paletou, F. (2019). "The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs". The Astronomical Journal. 158 (2): 56. arXiv:1905.07921. Bibcode:2019AJ....158...56H. doi:10.3847/1538-3881/ab23fe. S2CID 159041104.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  3. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  4. ^ a b c d Kirkpatrick, J. Davy; Henry, Todd J.; McCarthy, Donald W. Jr. (1991). "A standard stellar spectral sequence in the red/near-infrared - Classes K5 to M9". Astrophysical Journal Supplement. 77: 417. Bibcode:1991ApJS...77..417K. doi:10.1086/191611.
  5. ^ a b "Query= BL Cet". General Catalogue of Variable Stars. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16.
  6. ^ a b "Query= UV Cet". General Catalogue of Variable Stars. Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-16.
  7. ^ a b c d e f g h i j k Kervella, Pierre; et al. (October 2016), "The red dwarf pair GJ65 AB: inflated, spinning twins of Proxima. Fundamental parameters from PIONIER, NACO, and UVES observations", Astronomy & Astrophysics, 593, arXiv:1607.04351, Bibcode:2016A&A...593A.127K
  8. ^ a b Barnes, J. R.; et al. (October 2017), "Surprisingly different star-spot distributions on the near equal-mass equal-rotation-rate stars in the M dwarf binary GJ 65 AB", Monthly Notices of the Royal Astronomical Society, 471: 811–823, arXiv:1706.03979, Bibcode:2017MNRAS.471..811B
  9. ^ 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.
  10. ^ "Annotations on V* UV Cet object". Centre de Données astronomiques de Strasbourg. Retrieved 2010-04-14.
  11. ^ Beskin, G.; Karpov, S.; Plokhotnichenko, V.; Stepanov, A.; Tsap, Yu. (January 2017). "Discovery of the subsecond linearly polarized spikes of synchrotron origin in the UV Ceti giant optical flare". Publications of the Astronomical Society of Australia. 34. arXiv:1702.06660. doi:10.1017/pasa.2017.3. S2CID 125084280.
  12. ^ Potemine, Igor Yu. (April 2010). "Transit of Luyten 726-8 within 1 ly from Epsilon Eridani". arXiv:1004.1557 [astro-ph.SR].
  13. ^ Montes, D.; et al. (2001). "Late-type members of young stellar kinematic groups - I. Single stars". MNRAS. 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode:2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x. S2CID 55727428. Archived from the original on 2012-07-09. Retrieved 2010-04-18.{{cite journal}}: CS1 maint: unflagged free DOI (link)

Notes

Further reading

Retrieved from "https://en.wikipedia.org/w/index.php?title=Gliese_65&oldid=1171414611"