Beta Trianguli

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Not to be confused with Beta Trianguli Australis.
Beta Trianguli
Diagram showing star positions and boundaries of the Triangulum constellation and its surroundings
Cercle rouge 100%.svg

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]
Spectral type A5IV[3]
U−B color index +0.11[2]
B−V color index +0.14[2]
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[1] mas
Distance 127 ± 2 ly
(38.9 ± 0.5 pc)
Mass 3.5[5] M
Radius ~4 R
Luminosity 74 (combined)[5] L
Surface gravity (log g) 3.70[3] cgs
Temperature 8186[3] K
Rotational velocity (v sin i) 70[6] km/s
Age 0.73[7] Gyr
Other designations
β Trianguli, β Tri, Beta Tri, 4 Trianguli, HR 622, HD 13161, BD+34°381, FK5 75, HIP 10064, SAO 55306.[8]

Beta Trianguli (Beta Tri, β Trianguli, β Tri) is the Bayer designation for a binary star 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.[9]

The star Beta Trianguli has a stellar classification of A5IV, indicating that it has evolved away from the main sequence and is now a giant star, but the classification is uncertain and not consistent with the mass derived from the orbit.[5] It is among the least variable of the stars that were observed by the Hipparcos spacecraft, with a magnitude varying by only 0.0005.[10] This is a probable spectroscopic binary star system with an orbital period of 31.39 days and an eccentricity of 0.43.[11] They are separated by a distance of less than 5 AU.[12]

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.[12] It is thought to extend from 50 to 400 AU away from the stars.[5]



  1. ^ a b c d e f van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752free to read. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d 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. ^ a b c 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/0308182free to read. Bibcode:2003AJ....126.2048G. doi:10.1086/378365. 
  4. ^ Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Washington, Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W 
  5. ^ a b c d 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:1208.1759free to read. Bibcode:2012MNRAS.426.2115K. doi:10.1111/j.1365-2966.2012.21865.x. 
  6. ^ 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/0205255free to read, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943 
  7. ^ 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. (2012). "Resolved debris discs around a stars in the Herschel DEBRIS survey". Monthly Notices of the Royal Astronomical Society. 428 (2): 1263. arXiv:1210.0547free to read. Bibcode:2013MNRAS.428.1263B. doi:10.1093/mnras/sts117. 
  8. ^ "bet Tri -- Spectroscopic binary", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2011-12-12 
  9. ^ a b Garfinkle, Robert A. (1997), Star-Hopping: Your Visa to Viewing the Universe, Cambridge University Press, p. 238, ISBN 0-521-59889-3 
  10. ^ 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 
  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:0806.2878free to read, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x 
  12. ^ a b 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. 
  13. ^ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 10 日