Astronomy:Beta Trianguli

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Short description: Binary star in the constellation Triangulum
β Trianguli
Triangulum constellation map.svg
Red circle.svg
Location of β Trianguli (circled)
Observation data
Equinox J2000.0]] (ICRS)
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[1] mas
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

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 it is only a third-magnitude star,[2] it is the brightest star in the constellation Triangulum.[12]

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. 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode2007A&A...474..653V. 
  2. 2.0 2.1 2.2 2.3 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99): 99, Bibcode1966CoLPL...4...99J 
  3. 3.0 3.1 3.2 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. doi:10.1086/378365. Bibcode2003AJ....126.2048G. 
  4. Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Washington (Carnegie Institution of Washington), Bibcode1953GCRV..C......0W 
  5. Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode2012AstL...38..331A. 
  6. 6.0 6.1 Pourbaix, D. et al. (2004), "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits", Astronomy & Astrophysics 424: 727–732, doi:10.1051/0004-6361:20041213, Bibcode2004A&A...424..727P. 
  7. 7.0 7.1 7.2 7.3 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. doi:10.1111/j.1365-2966.2012.21865.x. Bibcode2012MNRAS.426.2115K. 
  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, doi:10.1051/0004-6361:20020943, Bibcode2002A&A...393..897R 
  9. Booth, M.; Kennedy, G.; Sibthorpe, B.; Matthews, B. C.; Wyatt, M. C.; Duchene, G.; Kavelaars, J. J.; Rodriguez, D. et al. (2013). "Resolved debris discs around a stars in the Herschel DEBRIS survey". Monthly Notices of the Royal Astronomical Society 428 (2): 1263. doi:10.1093/mnras/sts117. Bibcode2013MNRAS.428.1263B. 
  10. "bet Tri -- Spectroscopic binary", SIMBAD (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Beta+Trianguli, 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode2008MNRAS.389..869E 
  12. 12.0 12.1 Garfinkle, Robert A. (1997), Star-Hopping: Your Visa to Viewing the Universe, Cambridge University Press, p. 238, ISBN 0-521-59889-3, https://books.google.com/books?id=40JzBYGREL0C&pg=PA238 
  13. 13.0 13.1 Stansberry, J. A.; Stapelfeldt, K. R.; Trilling, D. T.; Su, K. Y.; Rieke, G. H.; Chen, C. (2005). "Protostars and Planets V, Proceedings of the Conference held October 24-28, 2005, in Hilton Waikoloa Village, Hawai'i". 8613. Bibcode2005prpl.conf.8613S. 
  14. Adelman, S. J. (February 2001), "Research Note Hipparcos photometry: The least variable stars", Astronomy and Astrophysics 367: 297–298, doi:10.1051/0004-6361:20000567, Bibcode2001A&A...367..297A 
  15. (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 10 日