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Beta Trianguli (Beta Tri, β Trianguli, β Tri) is the Bayer designation for a binary star[11] system in the constellation Triangulum, located about 127 light years from Earth.[1] Although the apparent magnitude is only 3.0,[2] it is the brightest star in the constellation Triangulum.[12]

Not to be confused with Beta Trianguli Australis.
β Trianguli
Location of β Trianguli (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Triangulum
Right ascension 02h 09m 32.62712s[1]
Declination +34° 59′ 14.2694″[1]
Apparent magnitude (V) +3.00[2]
Characteristics
Spectral type A5IV[3]
U−B color index +0.11[2]
B−V color index +0.14[2]
Astrometry
Radial velocity (Rv)+9.9[4] km/s
Proper motion (μ) RA: 149.16[1] mas/yr
Dec.: –39.10[1] mas/yr
Parallax (π)25.71 ± 0.34 mas[1]
Distance127 ± 2 ly
(38.9 ± 0.5 pc)
Absolute magnitude (MV)+0.05[5]
Orbit[6]
Period (P)31.3884 d
Eccentricity (e)0.53
Periastron epoch (T)2432004.255 JD
Argument of periastron (ω)
(secondary)		318.4°
Semi-amplitude (K1)
(primary)		33.3 km/s
Semi-amplitude (K2)
(secondary)		69.2 km/s
Details
Mass3.5[7] M☉
Luminosity74 (combined)[7] L☉
Surface gravity (log g)3.70[3] cgs
Temperature8,186[3] K
Rotational velocity (v sin i)70[8] km/s
Age0.73[9] Gyr
Other designations
β Trianguli, β Tri, Beta Tri, 4 Trianguli, HR 622, HD 13161, BD+34°381, FK5 75, HIP 10064, SAO 55306.[10]
Database references
SIMBADdata

This is a double-lined spectroscopic binary star system with an orbital period of 31.39 days and an eccentricity of 0.53.[6] The members are separated by a distance of less than 5 AU.[13] The primary component has a stellar classification of A5IV, indicating that it has evolved away from the main sequence and is now a subgiant star. However, the classification is uncertain and not consistent with the mass derived from the orbit.[7] It is among the least variable of the stars that were observed by the Hipparcos spacecraft, with a magnitude varying by only 0.0005.[14]

Based on observations using the Spitzer Space Telescope, as reported in 2005, this system is emitting an excess of infrared radiation. This emission can be explained by a circumbinary ring of dust. The dust is emitting infrared radiation at a blackbody temperature of 100 K.[13] It is thought to extend from 50 to 400 AU away from the stars.[7]


Naming



References


  1. van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J
  3. Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Robinson, P. E. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I". The Astronomical Journal. 126 (4): 2048. arXiv:astro-ph/0308182. Bibcode:2003AJ....126.2048G. doi:10.1086/378365. S2CID 119417105.
  4. Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Washington, Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W
  5. Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  6. Pourbaix, D.; et al. (2004), "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits", Astronomy & Astrophysics, 424: 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
  7. Kennedy, G. M.; Wyatt, M. C.; Sibthorpe, B.; Phillips, N. M.; Matthews, B.; Greaves, J. S. (2012). "Coplanar Circumbinary Debris Disks". Monthly Notices of the Royal Astronomical Society. 426 (3): 2115–28. arXiv:1208.1759. Bibcode:2012MNRAS.426.2115K. doi:10.1111/j.1365-2966.2012.21865.x. S2CID 59408005.
  8. Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393 (3): 897–911, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID 14070763
  9. Booth, M.; Kennedy, G.; Sibthorpe, B.; Matthews, B. C.; Wyatt, M. C.; Duchene, G.; Kavelaars, J. J.; Rodriguez, D.; Greaves, J. S.; Koning, A.; Vican, L.; Rieke, G. H.; Su, K. Y. L.; Moro-Martin, A.; Kalas, P. (2013). "Resolved debris discs around a stars in the Herschel DEBRIS survey". Monthly Notices of the Royal Astronomical Society. 428 (2): 1263. arXiv:1210.0547. Bibcode:2013MNRAS.428.1263B. doi:10.1093/mnras/sts117.
  10. "bet Tri -- Spectroscopic binary", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2011-12-12
  11. Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976
  12. Garfinkle, Robert A. (1997), Star-Hopping: Your Visa to Viewing the Universe, Cambridge University Press, p. 238, ISBN 0-521-59889-3
  13. Stansberry, J. A.; et al. (2005). "A Spitzer Survey for Debris Disks in Binary Star Systems". Protostars and Planets V, Proceedings of the Conference held October 24-28, 2005, in Hilton Waikoloa Village, Hawai'i. Protostars and Planets V. p. 8613. Bibcode:2005prpl.conf.8613S.
  14. Adelman, S. J. (February 2001), "Research Note Hipparcos photometry: The least variable stars", Astronomy and Astrophysics, 367: 297–298, Bibcode:2001A&A...367..297A, doi:10.1051/0004-6361:20000567
  15. (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 10 日

На других языках

[de] Beta Trianguli

β Trianguli ist mit einer scheinbaren Helligkeit von +3,00 mag der hellste Stern im Sternbild Dreieck. Er befindet sich in einer Entfernung von knapp 127 Lichtjahren und ist ein Stern der Spektralklasse A. Der Stern ist des Weiteren ein spektroskopischer Doppelstern. Der Begleiter umläuft dabei den Hauptstern mit einer Umlaufzeit von 31,8 Tagen in einer Entfernung von lediglich 0,3 AE. Aufgrund der großen Nähe der beiden Sterne könnte es sein, dass sie in ferner Zukunft verschmelzen.[2]
- [en] Beta Trianguli

[es] Beta Trianguli

Beta Trianguli (β Tri / 4 Trianguli / HD 13161) es la estrella más brillante en la constelación de Triangulum con magnitud aparente +3,00, por delante de Metallah o Mothallah (α Trianguli). Ocasionalmente recibe los nombres de Deltotum —de origen latino— y Deltotron —de origen griego—. Ambos hacen alusión a la forma de la constelación, que a los antiguos griegos les recordaba la letra Delta mayúscula (Δ). Se encuentra a 124 años luz de distancia del sistema solar.


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