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Superbubble

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For other uses, see Super bubble (disambiguation).
"supershell" redirects here. For other uses, see Super shell (disambiguation).
The superbubble Henize 70, also known as N70 or DEM301, in the Large Magellanic Cloud[1]

A superbubble or supershell is a cavity which is hundreds of light years across and is populated with hot (106 K) gas atoms, less dense than the surrounding interstellar medium, blown against that medium and carved out by multiple supernovae and stellar winds. The winds, passage and gravity of newly born stars strip superbubbles of any other dust or gas.[2] The Solar System lies near the center of an old superbubble, known as the Local Bubble, whose boundaries can be traced by a sudden rise in dust extinction of exterior stars at distances greater than a few hundred light years.

Formation

The most massive stars, with masses ranging from eight to roughly one hundred solar masses and spectral types of O and early B, are usually found in groups called OB associations. Massive O stars have strong stellar winds, and most of these stars explode as supernovae at the end of their lives.

The strongest stellar winds release kinetic energy of 1051 ergs (1044 J) over the lifetime of a star, which is equivalent to a supernova explosion. These winds can form stellar wind bubbles dozens of light years across.[3] Inside OB associations, the stars are close enough that their wind bubbles merge, forming a giant bubble called a superbubble. When stars die, supernova explosions, similarly, drive blast waves that can reach even larger sizes, with expansion velocities up to several hundred km s−1. Stars in OB associations are not gravitationally bound, but they drift apart at small speeds (of around 20 km s−1), and they exhaust their fuel rapidly (after a few millions of years). As a result, most of their supernova explosions occur within the cavity formed by the stellar wind bubbles.[4][5] These explosions never form a visible supernova remnant, but instead expend their energy in the hot interior as sound waves. Both stellar winds and stellar explosions thus power the expansion of the superbubble in the interstellar medium.

The interstellar gas swept up by superbubbles generally cools, forming a dense shell around the cavity. These shells were first observed in line emission at twenty-one centimeters from hydrogen,[6] leading to the formulation of the theory of superbubble formation. They are also observed in X-ray emission from their hot interiors, in optical line emission from their ionized shells, and in infrared continuum emission from dust swept up in their shells. X-ray and visible emission are typically observed from younger superbubbles, while older, larger objects seen in twenty-one centimeters may even result from multiple superbubbles combining, and so are sometimes distinguished by calling them supershells.

Large enough superbubbles can blow through the entire galactic disk, releasing their energy into the surrounding galactic halo or even into the intergalactic medium.[7][8]

Examples

Very Large Telescope image of superbubble LHA 120-N 44 in the Large Magellanic Cloud. Credit: ESO/Manu Mejias.

References

  1. ^ a b Henize 70: A SuperBubble In The LMC, Astronomy Picture of the Day, 1999-11-30
  2. ^ Thomson, Jason (2016-05-18). "Sublime image reveals superbubbles, star formation, and satellite galaxies". ProQuest 1789525419.
  3. ^ Castor, J.; McCray, R.; Weaver, R. (1975). "Interstellar Bubbles". Astrophysical Journal Letters. 200: L107–L110. Bibcode:1975ApJ...200L.107C. doi:10.1086/181908.
  4. ^ Tomisaka, K.; Habe, A.; Ikeuchi, S. (1981). "Sequential explosions of supernovae in an OB association and formation of a superbubble". Astrophys. Space Sci. 78 (2): 273–285. Bibcode:1981Ap&SS..78..273T. doi:10.1007/BF00648941. S2CID 119740951.
  5. ^ McCray, R.; Kafatos, M. (1987). "Supershells and Propagating Star Formation". Astrophys. J. 317: 190–196. Bibcode:1987ApJ...317..190M. doi:10.1086/165267. hdl:2060/19870005634.
  6. ^ Heiles, C. (1979). "H I shells and supershells". Astrophys. J. 229: 533–544. Bibcode:1979ApJ...229..533H. doi:10.1086/156986.
  7. ^ Tomisaka, K.; Ikeuchi, S. (1986). "Evolution of superbubble driven by sequential supernova explosions in a plane-stratified gas distribution". Publ. Astron. Soc. Jpn. 38 (5): 697–715. Bibcode:1986PASJ...38..697T.
  8. ^ Mac Low, M.-M.; McCray, R. (1988). "Superbubbles in Disk Galaxies". Astrophys. J. 324: 776–785. Bibcode:1988ApJ...324..776M. doi:10.1086/165936.
  9. ^ "A Cosmic Superbubble". ESO Photo Release. Retrieved 20 July 2011.
  10. ^ Nemiroff, R.; Bonnell, J., eds. (6 February 2006). "N44 Superbubble". Astronomy Picture of the Day. NASA.
  11. ^ Monogem Ring, The Internet Encyclopedia of Science
  12. ^ Yurii Pidopryhora, Felix J. Lockman, and Joseph C. Shields. The Ophiuchus Superbubble: A Gigantic Eruption from the Inner Disk of the Milky Way, The Astrophysical Journal 656:2, 928-942 (2007)
  13. ^ "Huge 'Superbubble' of Gas Blowing Out of Milky Way". PhysOrg.com. 2006-01-13. Retrieved 2008-07-04.
  14. ^ STIS and GHRS Observations of Warm and Hot Gas Overlying the Scutum Supershell (GS 018−04+44), The Astrophysical Journal
  15. ^ Observational Evidence of Supershell Blowout in GS 018-04+44: The Scutum Supershell, The Astrophysical Journal, Volume 532, Issue 2, pp. 943–969.
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