Organization:Scorpius–Centaurus Association

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Short description: The OB association closest to the sun
Map of the Area Containing Stars of the Scorpius–Centaurus Association.
Main associations of the Solar antapex half of the galactic plane, with Sco-Cen on the left

The Scorpius–Centaurus Association (sometimes called Sco–Cen or Sco OB2) is the nearest OB association to the Sun. This stellar association is composed of three subgroups (Upper Scorpius, Upper Centaurus–Lupus, and Lower Centaurus–Crux) and its distance is about 130 parsecs or 420 light-years.[1] Using improved Hipparcos data, Rizzuto and colleagues analysed nearby stars more closely, bringing the number of known members to 436. They doubt the need to add a subclassification because they found a more continuous spread of stars.[2]

The Sco–Cen subgroups range in age from 11 million years (Upper Scorpius)[3] to roughly 15 million years (Upper Centaurus–Lupus and Lower Centaurus–Crux). Many of the bright stars in the constellations Scorpius, Lupus, Centaurus, and Crux are members of the Sco–Cen association, including Antares (the most massive member of Upper Scorpius), and most of the stars in the Southern Cross.[4] Hundreds of stars have been identified as members of Sco-Cen, with masses ranging from roughly 15 solar masses (Antares) down to below the hydrogen-burning limit (i.e. brown dwarfs),[5] and the total stellar population in each of the three subgroups is probably of the order 1000–2000.[6] The Sco–Cen OB association appears to be the most pronounced part of a large complex of recent (<20 million years) and ongoing star-formation. The complex contains several star-forming molecular clouds in Sco–Cen's immediate vicinity—the Rho Oph, Pipe Nebula, Barnard 68, Chamaeleon, Lupus, Corona Australis, and Coalsack cloud complexes (all at distances of ~120-200 parsecs), and several less populous, young stellar groups on the periphery of Sco–Cen, including the ~3–5 million-year-old epsilon Cha group, ~7 million-year-old eta Chamaeleontis cluster (also called Mamajek 1), ~8 million-year-old TW Hydrae association, ~12 million-year-old Beta Pictoris moving group, and possibly the ~30–50 million-year-old IC 2602 open cluster.[4]

The stellar members of the Sco–Cen association have convergent proper motions of approximately 0.02–0.04 arcseconds per year, indicative that the stars have nearly parallel velocity vectors, moving at about 20 km/s with respect to the Sun. The dispersion of the velocities within the subgroups are only of order 1–2 km/s,[7] and the group is most likely gravitationally unbound. Several supernovae have exploded in Sco–Cen over the past 15 million years, leaving a network of expanding gas superbubbles around the group,[8] including the Loop I Bubble. To explain the presence of radioactive 60Fe in deep ocean ferromanganese crusts and in biogenic magnetite crystals within Pacific Ocean sediments[9] it has been hypothesized that a nearby supernova, possibly a member of Sco–Cen, exploded in the Sun's vicinity roughly 3 million years ago,[10] causing the Pliocene–Pleistocene boundary marine extinction.[11] However, other findings cite the distance at which this supernova occurred at more than 100 parsec, maintaining that it is not likely not to have contributed to this extinction through the mechanism of what is known as the ultra-violet B (UV-B) catastrophe.[9][12] In 2019, researchers found interstellar iron in Antarctica which they relate to the Local Interstellar Cloud, which might have been formed near the Sco-Cen Association. [13]

Close up on the Orion Arm, with major stellar associations (yellow), nebulae (red) and dark nebulae (grey) coreward from the Local Bubble with Sco-Cen.

See also

References

  1. ↑ Melnik, A. M.; Dambis, A. K. (2020). "Distance scale for high-luminosity stars in OB associations and in field with Gaia DR2. Spurious systematic motions". Astrophysics and Space Science 365 (7): 112. doi:10.1007/s10509-020-03827-0. Bibcode: 2020Ap&SS.365..112M. 
  2. ↑ Rizzuto, Aaron; Ireland, Michael; Robertson, J. G. (October 2011), "Multidimensional Bayesian membership analysis of the Sco OB2 moving group", Monthly Notices of the Royal Astronomical Society 416 (4): 3108–17, doi:10.1111/j.1365-2966.2011.19256.x, Bibcode: 2011MNRAS.416.3108R. 
  3. ↑ Mark J. Pecaut; Eric E. Mamajek; Eric J. Bubar (February 2012). "A Revised Age for Upper Scorpius and the Star Formation History among the F-type Members of the Scorpius-Centaurus OB Association". Astrophysical Journal 746 (2): 154. doi:10.1088/0004-637X/746/2/154. Bibcode: 2012ApJ...746..154P. 
  4. ↑ 4.0 4.1 Preibisch, T.; Mamajek, E. (2009). "The Nearest OB Association: Scorpius-Centaurus (Sco OB2)". Handbook of Star-Forming Regions 2: 0. Bibcode: 2008hsf2.book..235P. 
  5. ↑ Preibisch, T. (2002). "Exploring the Full Stellar Population of the Upper Scorpius OB Association". Astronomical Journal 124 (1): 404–416. doi:10.1086/341174. Bibcode: 2002AJ....124..404P. 
  6. ↑ Mamajek, E.E.; Meyer, M.R.; Liebert, James (2002). "Post-T Tauri Stars in the Nearest OB Association". Astronomical Journal 124 (3): 1670–1694. doi:10.1086/341952. Bibcode: 2002AJ....124.1670M. 
  7. ↑ Madsen, S. (2002). "Astrometric radial velocities. III. Hipparcos measurements of nearby star clusters and associations". Astronomy & Astrophysics 381 (2): 446–463. doi:10.1051/0004-6361:20011458. Bibcode: 2002A&A...381..446M. 
  8. ↑ de Geus, E.J. (1992). "Interaction of Stars and Interstellar Matter in Scorpio Centaurus". Astronomy & Astrophysics 262: 258–270. Bibcode: 1992A&A...262..258D. 
  9. ↑ 9.0 9.1 Ludwig, Peter (2016). "Time-resolved 2-million-year-old supernova activity discovered in Earth's microfossil record". Proceedings of the National Academy of Sciences 113 (33): 9232–9237. doi:10.1073/pnas.1601040113. ISSN 0027-8424. PMID 27503888. Bibcode: 2016PNAS..113.9232L. 
  10. ↑ Fields, Brian D.; Hochmuth, Kathrin A.; Ellis, John (2005). "Deep-Ocean Crusts as Telescopes: Using Live Radioisotopes to Probe Supernova Nucleosynthesis". Astrophys. J. 621 (2): 902–07. doi:10.1086/427797. Bibcode: 2005ApJ...621..902F. 
  11. ↑ Benítez, N.; Maíz-Apellániz, J.; Canelles M. (2005). "Evidence for nearby supernova explosions". Phys. Rev. Lett. 88 (8): 081101. doi:10.1103/physrevlett.88.081101. PMID 11863949. Bibcode: 2002PhRvL..88h1101B. 
  12. ↑ Cockell, CS (1999). "Crises and extinction in the fossil record—A role for ultraviolet radiation?". Paleobiology 25 (2): 212–225. doi:10.1017/S0094837300026518. 
  13. ↑ Koll, D.; et., al. (2019). "Interstellar 60Fe in Antarctica". Physical Review Letters 123 (7): 072701. doi:10.1103/PhysRevLett.123.072701. PMID 31491090. Bibcode: 2019PhRvL.123g2701K. 




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