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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]

β Arae
Location of β Arae (circled)
Observation data
Epoch J2000      Equinox J2000
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 mas[5]
Distance720 ± 30 ly
(219 ± 10 pc)
Absolute magnitude (MV)−3.494[6]
Details
Mass8.21[7] 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

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, thus:
              10[Fe/H] = 10+0.5 = 3.1

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. 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. 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. arXiv:1312.3474. Bibcode:2002A&A...395...97D. doi:10.1051/0004-6361:20021214.
  4. 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.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. 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. arXiv:astro-ph/0106070. Bibcode:2001A&A...374.1085C. doi:10.1051/0004-6361:20010816. S2CID 16286422.
  7. 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. arXiv:1506.06095. Bibcode:2015A&A...582A..49H. doi:10.1051/0004-6361/201526319. S2CID 53391939.
  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. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID 118629873.
  9. "bet Ara -- Star". SIMBAD. Centre de Données astronomiques de Strasbourg. 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. Retrieved 2012-01-16.
  11. "YILDIZ ADLARI SÖZLÜĞÜ" [Glossary of Star Names - V]. Mustafa Pultar (in Turkish). Retrieved 2020-03-04.
  12. "Ara". Google. Retrieved 2020-03-04.
  13. 陳久金 (2005). 中國星座神話 [Chinese horoscope myth] (in Chinese). Wunan Book Publishing Co. ISBN 978-986-7332-25-7.
  14. "天文教育資訊網". AEEA (Activities of Exhibition and Education in Astronomy) (in Chinese). 2006-07-01. Retrieved 2020-03-04.



На других языках

[de] Beta Arae

β Arae ist mit einer scheinbaren Helligkeit von +2,85 mag der hellste Stern im Sternbild Altar. Er befindet sich in einer Entfernung von etwa 650 Lichtjahren und ist ein Roter Überriese der Spektralklasse K. Der Stern hat mit etwa 90 Sonnenradien eine sehr große Ausdehnung. Wäre er in unserem Sonnensystem, so würde er beinahe die halbe Distanz zwischen Erde und Sonne ausfüllen. Der Stern rotiert vergleichsweise sehr langsam und braucht wohl mehr als 2 Jahre für eine Umdrehung.[2]
- [en] Beta Arae

[es] Beta Arae

Beta Arae (β Ara / HD 157244 / HR 6461) es la estrella más brillante en la constelación de Ara, con magnitud aparente +2,85. Comparte movimiento propio y velocidad radial con γ Arae,[1] por lo que se pensó que ambas estrellas podían formar un sistema binario amplio; sin embargo, medidas precisas de distancia realizadas por el satélite Hipparcos demostraron que Gamma Arae está casi al doble de distancia que Beta Arae. Esta última se encuentra a 603 años luz de distancia del Sistema Solar.

[ru] Бета Жертвенника

Бета Жертвенника (лат. β Arae) — одна из ярчайших звёзд в созвездии Жертвенника, относительно молодая звезда-гигант с видимой звёздной величиной 2,8 (округлённое значение)[2]. Измерения параллакса соответствуют расстоянию 650 световых лет от Солнца[1].


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