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Coordinates: Sky map 17h 33m 36.520s, −37° 06′ 13.76″
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}}
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{{Starbox character
{{Starbox character
| class=B2IV+DA7.9<ref>{{cite journal|bibcode=2013MNRAS.435.2077H|title=Where are all the Sirius-like binary systems?|journal=Monthly Notices of the Royal Astronomical Society|volume=435|issue=3|pages=2077|author1=Holberg|first1=J. B.|last2=Oswalt|first2=T. D.|last3=Sion|first3=E. M.|last4=Barstow|first4=M. A.|last5=Burleigh|first5=M. R.|year=2013|doi=10.1093/mnras/stt1433}}</ref>
| class=B2IV+DA7.9<ref>{{cite journal|bibcode=2013MNRAS.435.2077H}}</ref>
| b-v=&minus;0.240<ref name=hamdy>{{cite journal|bibcode= 1993Ap&SS.203...53H}}</ref>
| b-v=&minus;0.240<ref name=hamdy>{{cite journal|bibcode= 1993Ap&SS.203...53H|title= A catalogue of spectral classification and photometric data of B-type stars|journal= Astrophysics and Space Science (ISSN 0004-640X)|volume= 203|pages= 53|author1= Hamdy|first1= M. A.|last2= Abo Elazm|first2= M. S.|last3= Saad|first3= S. M.|year= 1993|doi= 10.1007/BF00659414}}</ref>
| u-b=&minus;0.880<ref name=hamdy/>
| u-b=&minus;0.880<ref name=hamdy/>
| variable=[[Beta Cephei variable|Beta Cephei]] (A)<ref name=handler/>
| variable=[[Beta Cephei variable|Beta Cephei]] (A)<ref name=handler/>
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{{Starbox astrometry
{{Starbox astrometry
| component_name=(component A)
| component_name=(component A)
| radial_v=&minus;3.00<ref>{{cite journal|bibcode=2006AstL...32..759G}}</ref>
| radial_v=&minus;3.00<ref>{{cite journal|bibcode=2006AstL...32..759G|title=Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system|journal=Astronomy Letters|volume=32|issue=11|pages=759|author1=Gontcharov|first1=G. A.|year=2006|doi=10.1134/S1063773706110065}}</ref>
| prop_mo_ra=&minus;8.90<ref name=hipparcos/>
| prop_mo_ra=&minus;8.90<ref name=hipparcos/>
| prop_mo_dec=&minus;29.95<ref name=hipparcos/>
| prop_mo_dec=&minus;29.95<ref name=hipparcos/>
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| component1 = λ Sco A
| component1 = λ Sco A
| mass = 14.5±1.1<ref name=handler/>
| mass = 14.5±1.1<ref name=handler/>
| radius = 8.8±1.2<ref name=handler>{{cite doi|10.1051/0004-6361/201321886}}</ref>
| radius = 8.8±1.2<ref name=handler>{{cite journal|bibcode=2013A&A...557A...1H|title=Time-resolved multicolour photometry of bright B-type variable stars in Scorpius|journal=Astronomy & Astrophysics|volume=557|pages=A1|author1=Handler|first1=G.|last2=Schwarzenberg-Czerny|first2=A.|year=2013|doi=10.1051/0004-6361/201321886}}</ref>
| luminosity = 36,300<ref name=handler/>
| luminosity = 36,300<ref name=handler/>
| temperature = 25,000±1,000<ref name=handler/>
| temperature = 25,000±1,000<ref name=handler/>
| metal_fe =
| metal_fe =
| gravity = 3.8<ref name=variability>{{cite journal|doi=10.1051/0004-6361:20041223 | bibcode=2004A&A...427..581U | volume=427 | title=Interpretation of the variability of the ? Cephei star ? Scorpii | journal=Astronomy and Astrophysics | pages=581–592}}</ref>
| gravity = 3.8<ref name=variability>{{cite journal|doi=10.1051/0004-6361:20041223 | bibcode=2004A&A...427..581U | volume=427 | title=Interpretation of the variability of the β Cephei star λ Scorpii | journal=Astronomy and Astrophysics | pages=581–592}}</ref>
| rotational_velocity = 150<ref name=handler/>
| rotational_velocity = 150<ref name=handler/>
| age_myr =
| age_myr =
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==Properties==
==Properties==
Lambda Scorpii is located some 570 light years away from Earth. Spectroscopic and [[astronomical interferometer|interferometric]] observations have shown that A is actually a [[star system|triple system]] consisting of two [[stellar classification|B-type]] stars and a [[pre–main sequence star]].<ref name=handler/> The primary star is also a [[beta Cephei variable]] star.<ref>{{cite journal|bibcode=2004A&A...427...581}}</ref><ref>{{cite journal|bibcode=2006MNRAS.370..884T}}</ref> 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 (geometry)|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 mass]]es, respectively. The age of the system is estimated to be in the range 10&ndash;13 million years.
Lambda Scorpii is located some 570 light years away from Earth. Spectroscopic and [[astronomical interferometer|interferometric]] observations have shown that A is actually a [[star system|triple system]] consisting of two [[stellar classification|B-type]] stars and a [[pre–main sequence star]].<ref name=handler/> The primary star is also a [[beta Cephei variable]] star.<ref name=variability/><ref>{{cite journal|bibcode=2006MNRAS.370..884T|title=Orbital elements, masses and distance of λ Scorpii a and B determined with the Sydney University Stellar Interferometer and high-resolution spectroscopy|journal=Monthly Notices of the Royal Astronomical Society|volume=370|issue=2|pages=884|author1=Tango|first1=W. J.|last2=Davis|first2=J.|last3=Ireland|first3=M. J.|last4=Aerts|first4=C.|last5=Uytterhoeven|first5=K.|last6=Jacob|first6=A. P.|last7=Mendez|first7=A.|last8=North|first8=J. R.|last9=Seneta|first9=E. B.|last10=Tuthill|first10=P. G.|year=2006|doi=10.1111/j.1365-2966.2006.10526.x}}</ref> 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 (geometry)|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 mass]]es, respectively. The age of the system is estimated to be in the range 10&ndash;13 million years.


A 15th [[apparent magnitude|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 unit]]s (AU) and the second approximately 17,000 AU (0.27 [[light years]]) away.
A 15th [[apparent magnitude|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 unit]]s (AU) and the second approximately 17,000 AU (0.27 [[light years]]) away.
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|publisher=FOTW Flags Of The World website
|publisher=FOTW Flags Of The World website
}}</ref>
}}</ref>
*The indigenous [[Wergaia|Boorong]] people of northwestern Victoria named it as ''Karik Karik'' (together with Upsilon Scorpii).,<ref name=hamacher>{{cite journal|author=Hamacher, Duane W.; Frew, David J. |date=2010|title= An Aboriginal Australian Record of the Great Eruption of Eta Carinae|journal=Journal of Astronomical History & Heritage |volume=13|issue=3|pages= 220–34|url=http://arxiv.org/ftp/arxiv/papers/1010/1010.4610.pdf}}</ref> "the Falcons"<ref name=stanbridge>{{cite journal|author=Stanbridge, WM|date=1857|title= On the Astronomy and Mythology of the Aboriginies of Victoria|journal=Transactions Philosophical Institute Victoria |volume=2|issue=|pages= 137–140|url=http://www.atnf.csiro.au/research/AboriginalAstronomy/literature/Stanbridge1857.pdf}}</ref>
*The indigenous [[Wergaia|Boorong]] people of northwestern Victoria named it as ''Karik Karik'' (together with Upsilon Scorpii).,<ref name=hamacher>{{cite journal | last1 = Hamacher | first1 = Duane W. | last2 = Frew | first2 = David J. | date = 2010 | title = An Aboriginal Australian Record of the Great Eruption of Eta Carinae | journal = Journal of Astronomical History and Heritage | volume = 13 | issue = 3 | pages = 220–34 | arxiv = 1010.4610 | bibcode = 2010JAHH...13..220H}}</ref> "the Falcons"<ref name=stanbridge>{{cite journal|bibcode=1857PPIVT...2..137S|title=On the astronomy and mythology of the Aborigines of Victoria|journal=Proceedings of the Philosophical Institute of Victoria|volume=2|pages=137|author1=Stanbridge|first1=William Edward|year=1857}}</ref>
*The fictional [[planet]] of [[Cybertron]] (in ''[[The Transformers (IDW Publishing)|The Transformers]]'' comics continuity by [[IDW Publishing]]) orbits Lambda Scorpii (or "Shaula"), according to longtime franchise writer Simon Furman in an interview. This fact has yet to make it into an in-continuity source.
*The fictional [[planet]] of [[Cybertron]] (in ''[[The Transformers (IDW Publishing)|The Transformers]]'' comics continuity by [[IDW Publishing]]) orbits Lambda Scorpii (or "Shaula"), according to longtime franchise writer Simon Furman in an interview. This fact has yet to make it into an in-continuity source.
*[[USS Shaula (AK-118)]] was a [[United States Navy]] [[Crater class cargo ship]] named after the star.
*[[USS Shaula (AK-118)]] was a [[United States Navy]] [[Crater class cargo ship]] named after the star.

Revision as of 23:09, 17 September 2015

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 mas[1]
Distanceapprox. 570 ly
(approx. 180 pc)
Absolute magnitude (MV)−5[citation needed]
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[7] 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[7] 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 also a beta Cephei variable star.[7][8] 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

References

  1. ^ a b c d e f 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. Bibcode:2013MNRAS.435.2077H. doi:10.1093/mnras/stt1433.
  4. ^ a b 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 (ISSN 0004-640X). 203: 53. Bibcode:1993Ap&SS.203...53H. doi:10.1007/BF00659414.
  5. ^ a b c d e f g h i j Handler, G.; Schwarzenberg-Czerny, A. (2013). "Time-resolved multicolour photometry of bright B-type variable stars in Scorpius". Astronomy & Astrophysics. 557: A1. 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. ^ a b c "Interpretation of the variability of the β Cephei star λ Scorpii". Astronomy and Astrophysics. 427: 581–592. Bibcode:2004A&A...427..581U. doi:10.1051/0004-6361:20041223.
  8. ^ 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. Bibcode:2006MNRAS.370..884T. doi:10.1111/j.1365-2966.2006.10526.x.
  9. ^ 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.
  10. ^ 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.
  11. ^ "Astronomy of the Brazilian Flag". FOTW Flags Of The World website.
  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.

External links


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