Astronomy:Mu1 Scorpii

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Short description: Binary star system in the constellation Scorpius


For other stars with this Bayer designation, see μ Scorpii.
μ1 Scorpii
Scorpius constellation map.svg
Red circle.svg
Location of μ1 Scorpii (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Scorpius
Right ascension  16h 51m 52.23111s[1]
Declination −38° 02′ 50.5694″[1]
Apparent magnitude (V) 2.94 - 3.22[2]
Characteristics
Spectral type B1.5 V + B6.5 V[3]
U−B color index −0.859[4]
B−V color index −0.202[4]
Variable type β Lyr[2]
Astrometry
Radial velocity (Rv)−25[5] km/s
Proper motion (μ) RA: −10.58[1] mas/yr
Dec.: −22.06[1] mas/yr
Parallax (π)6.51 ± 0.91[1] mas
Distanceapprox. 500 ly
(approx. 150 pc)
Absolute magnitude (MV)−2.9±0.3[3]
Orbit[3]
Period (P)1.44627 days
Semi-major axis (a)12.90±0.04 R☉
Eccentricity (e)0.0
Inclination (i)65.4±1°
Periastron epoch (T)2412374.434 HJD
Details[6]
μ1 Sco A
Mass8.3±1.0 M☉
Radius3.9±0.2 R☉
Surface gravity (log g)4.17±0.10 cgs
Temperature24,000±1,000 K
Rotational velocity (v sin i)191.5 km/s
μ1 Sco B
Mass4.6±1.0 M☉
Radius4.6±0.3 R☉
Surface gravity (log g)3.77±0.12 cgs
Temperature17,000±700 K
Rotational velocity (v sin i)165.0 km/s
Other designations
Xamidimura, CD−37°11033, FK5 1439, HD 151890, HIP 82514, HR 6247, SAO 208102, WDS 16519-3803
Database references
SIMBADdata

Mu1 Scorpii (μ1 Scorpii, abbreviated Mu1 Sco, μ1 Sco) is a binary star system in the southern zodiac constellation of Scorpius. The combined apparent visual magnitude of the pair is about magnitude 3, making it one of the brighter members of Scorpius. Based upon parallax measurements, the distance of this system from the Sun is roughly 500 light-years (150 parsecs).[1] This system is a member of the Scorpius–Centaurus association, the nearest OB association of co-moving stars to the Sun.[3]

The primary (Mu1 Scorpii Aa) is formally named Xamidimura /ˌkæmidiˈmʊərə/, from the Khoekhoe xami di mûra IPA: [xami ti mũːɾa] 'the (two) eyes of the lion'.[7]

Properties

A light curve for Mu1 Scorpii, plotted from TESS data[8]

Mu1 Scorpii is an eclipsing binary of the Beta Lyrae type. Discovered to be a spectroscopic binary by Solon Irving Bailey in 1896, it was only the third such eclipsing pair to be discovered. This is a semidetached binary system where the secondary is close to filling its Roche lobe, or it may even be overflowing. The two stars revolve each other along a circular orbit with the components separated by 12.9 times the Sun's radius.[3] Due to occultation of each component by the other, the apparent magnitude of the system decreased by 0.3 and 0.4 magnitudes over the course of the binary's orbit, which takes 34 hours 42.6 minutes to complete.

The primary component is a B-type main sequence star with a stellar classification of B1.5 V. It has 8.3 times the mass of the Sun and 3.9 times the Sun's radius. The secondary is a smaller B-type main sequence star with a classification of about B6.5 V, having 3.6 times the Sun's mass and 4.6 times the radius of the Sun. The effective temperature of the outer atmosphere for each star is 24,000 K for the primary and 17,000 K for the secondary. At these temperatures, the two stars glow with a blue-white hue.[9]

Nomenclature

μ1 Scorpii (Latinised to Mu1 Scorpii) is the system's Bayer designation. The designations of the primary as Mu1 Scorpii Aa derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[10]

The pair of stars Mu1 and Mu2 Scorpii are known as the xami di mura 'eyes of the lion' by the Khoikhoi people of South Africa .[11]

In 2016, the IAU organized a Working Group on Star Names (WGSN)[12] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[13] It approved the name Xamidimura for the component Mu1 Scorpii Aa on 5 September 2017 (along with Pipirima for the partner of Mu1 Scorpii) and it is now so included in the List of IAU-approved Star Names.[7]

In Chinese, 尾宿 (Wěi Xiù), meaning Tail, refers to an asterism consisting of Mu1 Scorpii, Epsilon Scorpii, Zeta1 Scorpii and Zeta2 Scorpii, Eta Scorpii, Theta Scorpii, Iota1 Scorpii and Iota2 Scorpii, Kappa Scorpii, Lambda Scorpii and Upsilon Scorpii.[14] Consequently, the Chinese name for Mu1 Scorpii itself is 尾宿一 (Wěi Xiù yī), "the First Star of Tail".[15]

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. Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 Samus, N. N. et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1 61 (1): 80–88. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 van Antwerpen, C.; Moon, T. (January 2010). "New observations and analysis of the bright semidetached eclipsing binary μ1 Sco". Monthly Notices of the Royal Astronomical Society 401 (3): 2059–2066. doi:10.1111/j.1365-2966.2009.15796.x. Bibcode: 2010MNRAS.401.2059V. 
  4. ↑ 4.0 4.1 Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968). "A photometric investigation of the Scorpio-Centaurus association". Astrophysical Journal Supplement 15: 459. doi:10.1086/190168. Bibcode: 1968ApJS...15..459G. 
  5. ↑ Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication (Washington: Carnegie Institution of Washington). Bibcode: 1953GCRV..C......0W. 
  6. ↑ Budding, E.; Butland, R.; Blackford, M. (2015). "Absolute parameters of young stars: GG Lup and μ1 Sco". Monthly Notices of the Royal Astronomical Society 448 (4): 3784. doi:10.1093/mnras/stv234. Bibcode: 2015MNRAS.448.3784B. 
  7. ↑ 7.0 7.1 "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/. Retrieved 16 December 2017. 
  8. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  9. ↑ "The Colour of Stars". Australia Telescope, Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. December 21, 2004. http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html. Retrieved 2012-01-16. 
  10. ↑ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  11. ↑ Astronomical Society of Southern Africa (2013) African ethnoastronomy
  12. ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. Retrieved 22 May 2016. 
  13. ↑ "WG Triennial Report (2015-2018) - Star Names". p. 5. https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf. Retrieved 2018-07-14. 
  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.



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