Astronomy:Beta Arae

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Short description: Star in the constellation Ara
β Arae
Ara constellation map.svg
Red circle.svg
Location of β Arae (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Ara
Right ascension  17h 25m 17.98835s[1]
Declination −55° 31′ 47.5868″[1]
Apparent magnitude (V) 2.84[2]
Characteristics
Spectral type K3 Ib-II[3]
U−B color index +1.56[4]
B−V color index +1.46[4]
Astrometry
Radial velocity (Rv)−0.30±0.20[3] km/s
Proper motion (μ) RA: −8.51[1] mas/yr
Dec.: −25.24[1] mas/yr
Parallax (π)4.5601 ± 0.2077[5] mas
Distance720 ± 30 ly
(219 ± 10 pc)
Absolute magnitude (MV)−3.494[6]
Details
Mass8.21[7] ,6.2~7.3 M☉
Luminosity5,636[7] L☉
Surface gravity (log g)1.20[7] cgs
Temperature4,197[7] K
Metallicity [Fe/H]−0.05[7] dex
Rotational velocity (v sin i)5.4±1.0[3] km/s
Age50.1±4.4[8] Myr
Other designations
CPD−55°8100, FK5 645, HD 157244, HIP 85258, HR 6461, SAO 244725[9]
Database references
SIMBADdata

Beta Arae (β Ara, β Arae), the brightest star in the constellation of Ara, is a very luminous, relatively young, giant star with an apparent visual magnitude of 2.8 (rounded).[2] Parallax measurements place it at roughly 650 light-years (200 parsecs) from Earth.[1]

The spectrum of this star matches a stellar classification of K3 Ib-IIa,[3] with the luminosity class notation 'Ib-IIa' indicating that the star lies part way between a higher luminosity bright giant (IIa) and a lower luminosity supergiant (Ib). This represents two of the evolutionary stages that a massive star passes through after it has exhausted the hydrogen at its core. Beta Arae is radiating energy from its outer envelope at an effective temperature of 4,200 K, which causes it to take on the orange hue of a K-type star.[10] This enlarged star appears to be rotating slowly with a projected rotational velocity of about 5 km/s.[3] The abundance of elements other than hydrogen and helium, its metallicity, is more than three times that of the Sun.[3][lower-alpha 1]

Rarely, this star is called Vasat-ül-cemre a Turkisation of Arabic وسط الجمر (wasaṭ al-jamar), meaning "middle of the embers."[11] The constellation is named in Arabic المجمرة (al-mijmarah), meaning brazier/incense-burner.[12] In Chinese, 杵 (Chǔ), meaning Pestle, refers to an asterism of β, σ and α Arae.[13] The Chinese name for β Arae is 杵三 (Chǔ sān, English: the Third Star of Pestle.)[14]

Notes

  1. ↑ The abundance is estimated by taking [Fe/H] to the power of ten:
              10[Fe/H] = 10+0.5 = 3.1

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 Wielen, R. et al. (1999). "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions". Veröff. Astron. Rechen-Inst. Heidelb (Astronomisches Rechen-Institut Heidelberg) 35 (35): 1. Bibcode: 1999VeARI..35....1W. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 De Medeiros, J. R. et al. (November 2002). "A catalog of rotational and radial velocities for evolved stars. II. Ib supergiant stars". Astronomy and Astrophysics 395: 97–98. doi:10.1051/0004-6361:20021214. Bibcode: 2002A&A...395...97D. 
  4. ↑ 4.0 4.1 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. 
  5. ↑ Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  6. ↑ Cassatella, A.; Altamore, A.; Badiali, M.; Cardini, D. (2001). "On the Wilson-Bappu relationship in the Mg II k line". Astronomy and Astrophysics 374 (3): 1085–1091. doi:10.1051/0004-6361:20010816. Bibcode: 2001A&A...374.1085C. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Heiter, U.; Jofré, P.; Gustafsson, B.; Korn, A. J.; Soubiran, C.; Thévenin, F. (2015). "Gaia FGK benchmark stars: Effective temperatures and surface gravities". Astronomy & Astrophysics 582: A49. doi:10.1051/0004-6361/201526319. Bibcode: 2015A&A...582A..49H. 
  8. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society 410 (1): 190–200. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T. 
  9. ↑ "bet Ara -- Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Beta+Arae. Retrieved 2012-01-15. 
  10. ↑ "The Colour of Stars". Australia Telescope, Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. December 21, 2004. Archived from the original on 2012-03-18. https://web.archive.org/web/20120318151427/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html. Retrieved 2012-01-16. 
  11. ↑ "YILDIZ ADLARI SÖZLÜĞÜ". http://www.pultar.org/~mustafa/YAS/V.html#VasatUlCemre. Retrieved 2020-03-04. 
  12. ↑ "Ara". https://sites.google.com/site/urjuzatalkawakib/ara. Retrieved 2020-03-04. 
  13. ↑ 陳久金 (2005). 中國星座神話. Wunan Book Publishing Co.. ISBN 978-986-7332-25-7. https://books.google.com/books?id=0Vex0rYzdu8C. 
  14. ↑ "天文教育資訊網". 2006-07-01. http://aeea.nmns.edu.tw/2006/0607/ap060701.html. Retrieved 2020-03-04. 

External links



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