Astronomy:Lambda Scorpii

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Short description: Triple star system in the constellation Scorpius
λ Scorpii
Scorpius constellation map.svg
Red circle.svg
Location of λ Scorpii (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Scorpius
Pronunciation /ˈʃɔːlə/[1][2]
Right ascension  17h 33m 36.520s[3]
Declination −37° 06′ 13.76″[3]
Apparent magnitude (V) 1.62 + 14.9 + 12.0[3][4]
Characteristics
Spectral type B1.5IV + B2IV[5][6]
U−B color index −0.880[7]
B−V color index −0.240[7]
Variable type Beta Cephei (A)[8]
Astrometry
Radial velocity (Rv)−3.00[9] km/s
Proper motion (μ) RA: −8.90[3][3] mas/yr
Dec.: −29.95[3] mas/yr
Parallax (π)5.71 ± 0.90[3] mas
Distanceapprox. 570 ly
(approx. 180 pc)
Absolute magnitude (MV)−3.70[10]
Orbit[11]
PrimaryA
CompanionB
Period (P)2.8825 yr
Semi-major axis (a)49.3 mas
Eccentricity (e)0.121
Inclination (i)77.2°
Orbit[11]
PrimaryAa
CompanionAb
Period (P)5.9520 d
Eccentricity (e)0.26
Semi-amplitude (K1)
(primary)		39.3 km/s
Details
λ Sco Aa
Mass10.4[5] M☉
Radius8.8±1.2[8] R☉
Luminosity36,300[8] L☉
Surface gravity (log g)3.8[6] cgs
Temperature25,000±1,000[8] K
Rotation3.4±0.5 d[8]
Rotational velocity (v sin i)150[8] km/s
λ Sco B
Mass8.1[5] M☉
Radius4.7±1.0[8] R☉
Surface gravity (log g)4.0[6] cgs
Temperature25,000±1,000[8] K
λ Sco Ab
Mass1.8[5] M☉
Other designations
Database references
SIMBADdata

Lambda Scorpii is a triple star system and the second-brightest object in the constellation of Scorpius. It is formally named Shaula; Lambda Scorpii is its Bayer designation, which is Latinised from λ Scorpii and abbreviated Lambda Sco or λ Sco. With an apparent visual magnitude of 1.62, it is one of the brightest stars in the night sky.

Nomenclature

λ Scorpii (Latinised to Lambda Scorpii) is the star system's Bayer designation.

It bore the traditional name Shaula, which comes from the Arabic الشولاء al-šawlā´ meaning 'the raised [tail]', as it is found in the tail of Scorpius, the scorpion. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[12] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[13] included a table of the first two batches of names approved by the WGSN, which included Shaula for the star λ Scorpii Aa.

In Indian Astronomy it is called MulA Nakshathram. Mūla ("root") (Devanagari मूल/मूळ) (Tamil: மூலம்) is the 19th nakshatra or "lunar mansion" in Vedic astrology. The symbol of Mula is a bunch of roots tied together (reticulated roots) or an 'elephant goad' (ankusha).[citation needed]

In Chinese, 尾宿 (Wěi Xiù), meaning Tail, refers to an asterism consisting of λ Scorpii, ε Scorpii, ζ1 Scorpii, ζ2 Scorpii, η Scorpii, θ Scorpii, ι1 Scorpii, ι2 Scorpii, κ Scorpii, μ1 Scorpii, and υ Scorpii.[14] Consequently, the Chinese name for λ Scorpii itself is 尾宿八 (Wěi Xiù bā), "the Eighth Star of Tail".[15]

Together with υ Scorpii (Lesath), Shaula is listed in the Babylonian compendium MUL.APIN as dSharur4 u dShargaz, meaning "Sharur and Shargaz".[16]

In Coptic, they were called Minamref.[17]

The indigenous Boorong people of northwestern Victoria (Australia) named it (together with Upsilon Scorpii) Karik Karik,[18] "the Falcons".[19]

Properties

A light curve for Lambda Scorpii, plotted from TESS data.[20] The large dips in brightness are eclipses, and the rapid oscillations show the Beta Cephei variability.

Lambda Scorpii is located some 570 light-years away from the Sun.

Spectroscopic and interferometric observations have shown that it is actually a triple star system consisting of two B-type stars and a pre-main-sequence star.[8] The primary star is a Beta Cephei variable star with rapid brightness changes of about a hundredth of a magnitude.[6][5] The pre-main-sequence star has an orbital period of 6 days and the B companion has a period of 1053 days. The three stars lie in the same orbital plane, strongly suggesting that they were formed at the same time. The masses of the primary, pre-main-sequence star and the B companion are 14.5, 2.0 and 10.6 solar masses, respectively. The age of the system is estimated to be in the range 10–13 million years.

A 15th-magnitude star has a separation of 42 arcseconds, whereas a 12th-magnitude star is 95 arcseconds away. It is not known whether or not these components are physically associated with Lambda Scorpii. If they both were, the first would have a projected linear separation of approximately 7,500 astronomical units (AU) and the second approximately 17,000 AU (0.27 light-years) away. Gaia Data Release 3 reports that the fainter of these two stars is a little larger and brighter than the sun and about 420 light years away,[21] while the brighter star is a luminous background object.[22]

In culture

Shaula appears on the flag of Brazil, symbolizing the state of Rio Grande do Norte.

USS Shaula (AK-118) was a U.S. Navy Crater-class cargo ship named after the star.

References

  1. ↑ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7. 
  2. ↑ "IAU Catalog of Star Names". http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt. Retrieved 28 July 2016. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Van Leeuwen, F. (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. 
  4. ↑ Reed, B. Cameron (2003), "Catalog of Galactic OB Stars", The Astronomical Journal 125 (5): 2531–2533, doi:10.1086/374771, Bibcode: 2003AJ....125.2531R. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 Tango, W. J.; Davis, J.; Ireland, M. J.; Aerts, C.; Uytterhoeven, K.; Jacob, A. P.; Mendez, A.; North, J. R. et al. (2006). "Orbital elements, masses and distance of λ Scorpii a and B determined with the Sydney University Stellar Interferometer and high-resolution spectroscopy". Monthly Notices of the Royal Astronomical Society 370 (2): 884–890. doi:10.1111/j.1365-2966.2006.10526.x. Bibcode: 2006MNRAS.370..884T. 
  6. ↑ 6.0 6.1 6.2 6.3 Uytterhoeven, K.; Willems, B.; Lefever, K.; Aerts, C.; Telting, J. H.; Kolb, U. (2004). "Interpretation of the variability of the β Cephei star λ Scorpii". Astronomy and Astrophysics 427 (2): 581–592. doi:10.1051/0004-6361:20041223. Bibcode: 2004A&A...427..581U. 
  7. ↑ 7.0 7.1 Hamdy, M. A.; Abo Elazm, M. S.; Saad, S. M. (1993). "A catalogue of spectral classification and photometric data of B-type stars". Astrophysics and Space Science 203 (1): 53–107. doi:10.1007/BF00659414. Bibcode: 1993Ap&SS.203...53H. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.7 8.8 Handler, G.; Schwarzenberg-Czerny, A. (2013). "Time-resolved multicolour photometry of bright B-type variable stars in Scorpius". Astronomy & Astrophysics 557: A1. doi:10.1051/0004-6361/201321886. Bibcode: 2013A&A...557A...1H. 
  9. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G. 
  10. ↑ Balona, L. A.; Feast, M. W. (1975). "The luminosities of the beta Canis Majoris variables, the zero age main sequence and the distance of the Sco-Cen association". Monthly Notices of the Royal Astronomical Society 172: 191–203. doi:10.1093/mnras/172.1.191. Bibcode: 1975MNRAS.172..191B. 
  11. ↑ 11.0 11.1 Tokovinin, Andrei (2018-03-01). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series 235 (1): 6. doi:10.3847/1538-4365/aaa1a5. ISSN 0067-0049. Bibcode: 2018ApJS..235....6T. 
  12. ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. Retrieved 22 May 2016. 
  13. ↑ "Bulletin of the IAU Working Group on Star Names, No. 1". http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf. Retrieved 28 July 2016. 
  14. ↑ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN:978-986-7332-25-7.
  15. ↑ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 , Hong Kong Space Museum. Accessed on line November 23, 2010.
  16. ↑ Rogers, J. H. (February 1998). "Origins of the ancient constellations: I. The Mesopotamian traditions". Journal of the British Astronomical Association 108 (1): 9–28. Bibcode: 1998JBAA..108....9R. 
  17. ↑ Robert Burnham (1978). Burnham's Celestial Handbook: An Observer's Guide to the Universe Beyond the Solar System. New York: Courier Corporation. p. 1678. ISBN 978-0-486-23673-5. https://books.google.com/books?id=PJzIt3SIlkUC. 
  18. ↑ Hamacher, Duane W.; Frew, David J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae". Journal of Astronomical History and Heritage 13 (3): 220–34. doi:10.3724/SP.J.1440-2807.2010.03.06. Bibcode: 2010JAHH...13..220H. 
  19. ↑ Stanbridge, William Edward (1857). "On the astronomy and mythology of the Aborigines of Victoria". Proceedings of the Philosophical Institute of Victoria 2: 137. Bibcode: 1857PPIVT...2..137S. 
  20. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  21. ↑ Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  22. ↑ Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.

Coordinates: Sky map 17h 33m 36.520s, −37° 06′ 13.76″



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