Epsilon Scorpii

Epsilon Scorpii
Diagram showing star positions and boundaries of the Scorpius constellation and its surroundings


Location of ε Scorpii (circled)

Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 16h 50m 09.8s[1]
Declination –34° 17′ 36″[1]
Apparent magnitude (V) +2.310[2]
Characteristics
Spectral type K1 III[3]
U−B color index +1.147[2]
B−V color index +1.150[2]
Astrometry
Radial velocity (Rv)–2.5[4] km/s
Proper motion (μ) RA: –614.85[1] mas/yr
Dec.: –255.98[1] mas/yr
Parallax (π)51.19 ± 0.22[1] mas
Distance63.7 ± 0.3 ly
(19.54 ± 0.08 pc)
Absolute magnitude (MV)0.78 ± 0.04[5]
Details
Radius12.6[6] R☉
Surface gravity (log g)2.49[7] cgs
Temperature4,560[7] K
Metallicity [Fe/H]–0.17[7] dex
Rotational velocity (v sin i)2.6 ± 0.5[8] km/s
Other designations
Wei, 26 Scorpii, CD–34 11285, FK5 628, GCTP 3823.00, Gl 639.1, HD 151680, HIP 82396, HR 6241, LHS 3244, SAO 208078.[9]

Epsilon Scorpii (ε Sco, ε Scorpii) is a star in the southern zodiac constellation of Scorpius. Patrick Moore introduced the name Wei but this seems to be a misreading;[10] Wěi (尾), meaning the Tail, was originally the name of a Chinese asterism or Xiù comprising the stars ε, μ1−2, ζ1−2, η, θ, ι, κ, υ, and λ Scorpii.[11] This star has an apparent visual magnitude of +2.3,[2] making it the fifth brightest member of the constellation. Parallax measurements made during the Hipparcos mission provide an estimated distance to this star of around 63.7 light-years (19.5 parsecs).[1]

Epsilon Scorpii has a stellar classification of K1 III,[3] which indicates it has exhausted the supply of hydrogen at its core and evolved into a giant star. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is 5.99 ± 0.06 mas,[12] which, at its estimated distance, equates to a physical radius of nearly 13 times the radius of the Sun.[6] Presently it is generating energy through the nuclear fusion of helium at its core, which, considering the star's composition, places it along an evolutionary branch termed the red clump. The star's outer atmosphere has an effective temperature of 4,560 K,[7] giving it the orange hue of a cool K-type star. It is classified as a variable star, although it only varies by around 0.01–0.02 magnitudes.[13] Epsilon Scorpii is an X-ray source with a luminosity of (1.5–1.6) × 1027 erg s−1.[5][14]

Modern legacy

Wei appears on the flag of Brazil, symbolising the state of Ceará.[15]

See also

References

  1. 1 2 3 4 5 6 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
  2. 1 2 3 4 Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968), "A photometric investigation of the Scorpio-Centaurus association", Astrophysical Journal Supplement 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168
  3. 1 2 Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637
  4. ↑ Wielen, R.; et al. (1999), Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions (35), Astronomisches Rechen-Institut Heidelberg, Bibcode:1999VeARI..35....1W
  5. 1 2 Schroeder, K.-P.; Huensch, M.; Schmitt, J. H. M. M. (July 1988), "X-ray activity and evolutionary status of late-type giants", Astronomy and Astrophysics 335: 591–595, Bibcode:1998A&A...335..591S
  6. 1 2 Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
    \begin{align} 2\cdot R_* & = \frac{(10^{-3}\cdot 19.54\cdot 5.99)\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 25.2\cdot R_{\bigodot} \end{align}
  7. 1 2 3 4 McWilliam, Andrew (December 1990), "High-resolution spectroscopic survey of 671 GK giants", Astrophysical Journal Supplement Series 74: 1075–1128, Bibcode:1990ApJS...74.1075M, doi:10.1086/191527
  8. ↑ Carney, Bruce W.; et al. (March 2008), "Rotation and Macroturbulence in Metal-Poor Field Red Giant and Red Horizontal Branch Stars", The Astronomical Journal 135 (3): 892–906, arXiv:0711.4984, Bibcode:2008AJ....135..892C, doi:10.1088/0004-6256/135/3/892
  9. ↑ "eps Sco -- Variable Star", SIMBAD Astronomical Object Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-02-23
  10. ↑ Moore, P. (1983), The Guinness Book of Astronomy: Facts (2nd ed.), Middlesex, UK: Guinness Superlatives Limited, p. 242
  11. ↑ Ridpath, Ian, Star Tales.
  12. ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics 431: 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039
  13. ↑ Adelman, Saul J. (2001), "On the Photometric Variability of Red Clump Giants", Baltic Astronomy 10: 593–597, Bibcode:2001BaltA..10..593A
  14. ↑ Gondoin, P. (December 1999), "Evolution of X-ray activity and rotation on G-K giants", Astronomy and Astrophysics 352: 217–227, Bibcode:1999A&A...352..217G
  15. ↑ "Astronomy of the Brazilian Flag". FOTW Flags Of The World website.
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