Lambda Scorpii

Lambda Scorpii


Location of λ Scorpii (circled)

Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 17h 33m 36.520s[1]
Declination −37° 06′ 13.76″[1]
Apparent magnitude (V) 1.62 / 14.9 / 12.0[1][2]
Characteristics
Spectral type B2IV+DA7.9[3]
U−B color index −0.880[4]
B−V color index −0.240[4]
Variable type Beta Cephei (A)[5]
Astrometry
Radial velocity (Rv)−3.00[6] km/s
Proper motion (μ) RA: −8.90[1] mas/yr
Dec.: −29.95[1] mas/yr
Parallax (π)5.71 ± 0.90[1] mas
Distanceapprox. 570 ly
(approx. 180 pc)
Absolute magnitude (MV)−3.70[7]
Details
λ Sco A
Mass14.5±1.1[5] M☉
Radius8.8±1.2[5] R☉
Luminosity36,300[5] L☉
Surface gravity (log g)3.8[8] cgs
Temperature25,000±1,000[5] K
Rotational velocity (v sin i)150[5] km/s
λ Sco B
Mass9.6-11.6[5] M☉
Radius4.7±1.0[5] R☉
Surface gravity (log g)4.0[8] cgs
Temperature25,000±1,000[5] K
Other designations
Shaula, 35 Scorpii, 35 Sco, HR 6527, CD -37 11673, HD 158926, SAO 208954, FK5 652, HIP 85927, CCDM J17336-3706A/B/C.
Database references
SIMBADdata
Data sources:
CCDM (2002),
Simbad

Lambda Scorpii (λ Sco, λ Scorpii) is a blue star and the second brightest star system in the constellation Scorpius, and one of the brightest stars in the nighttime sky. It has the Bayer designation λ despite being the second brightest in its constellation. It has the traditional name Shaula, which comes from the Arabic الشولاء al-šawlā´ meaning the raised [tail], as it is found in the tail of the scorpion (Scorpius). It is known as Wei Xiu Ba 尾宿八 (the Eighth Star of the Tail) in Chinese.

Properties

Lambda Scorpii is located some 570 light years away from Earth. Spectroscopic and interferometric observations have shown that A is actually a triple system consisting of two B-type stars and a pre–main sequence star.[5] The primary star is a beta Cephei variable star with rapid brightness changes of about a hundredth of a magnitude.[8][9] 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 7500 Astronomical units (AU) and the second approximately 17,000 AU (0.27 light years) away.

In culture

See also

References

  1. 1 2 3 4 5 6 Van Leeuwen, F. (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. ↑ Reed, B. Cameron (2003), "Catalog of Galactic OB Stars", The Astronomical Journal 125 (5): 2531–2533, Bibcode:2003AJ....125.2531R, doi:10.1086/374771.
  3. ↑ Holberg, J. B.; Oswalt, T. D.; Sion, E. M.; Barstow, M. A.; Burleigh, M. R. (2013). "Where are all the Sirius-like binary systems?". Monthly Notices of the Royal Astronomical Society 435 (3): 2077. arXiv:1307.8047. Bibcode:2013MNRAS.435.2077H. doi:10.1093/mnras/stt1433.
  4. 1 2 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: 53. Bibcode:1993Ap&SS.203...53H. doi:10.1007/BF00659414.
  5. 1 2 3 4 5 6 7 8 9 10 Handler, G.; Schwarzenberg-Czerny, A. (2013). "Time-resolved multicolour photometry of bright B-type variable stars in Scorpius". Astronomy & Astrophysics 557: A1. arXiv:1307.2733. Bibcode:2013A&A...557A...1H. doi:10.1051/0004-6361/201321886.
  6. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
  7. ↑ 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. Bibcode:1975MNRAS.172..191B. doi:10.1093/mnras/172.1.191.
  8. 1 2 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. Bibcode:2004A&A...427..581U. doi:10.1051/0004-6361:20041223.
  9. ↑ Tango, W. J.; Davis, J.; Ireland, M. J.; Aerts, C.; Uytterhoeven, K.; Jacob, A. P.; Mendez, A.; North, J. R.; Seneta, E. B.; Tuthill, P. G. (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. arXiv:astro-ph/0605311. Bibcode:2006MNRAS.370..884T. doi:10.1111/j.1365-2966.2006.10526.x.
  10. ↑ Rogers, J. H. (February 1998). "Origins of the ancient constellations: I. The Mesopotamian traditions". Journal of the British Astronomical Association, no.1 108: 9–28. Bibcode:1998JBAA..108....9R.
  11. ↑ p. 1678, Burnham's Celestial Handbook: An Observer's Guide to the Universe Beyond the Solar System, Volume 3, Robert Burnham, New York, Dover Publication, Inc, 1978.
  12. ↑ 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. arXiv:1010.4610. Bibcode:2010JAHH...13..220H.
  13. ↑ 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.

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

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