Colliding-wind binary

A colliding-wind binary is a binary star system in which the two members are massive stars that emit powerful, radiatively-driven stellar winds. The location where these two winds collide produces a strong shock front that can cause radio, X-ray and possibly synchrotron radiation emission.[1] Wind compression in the bow shock region between the two stellar winds allows dust formation. When this dust streams away from the orbiting pair, it can form a pinwheel nebula of spiraling dust. Such pinwheels have been observed in the Quintuplet Cluster[2]

An composite optical/x-ray image of Eta Carinae and its surrounding nebula taken by the Chandra Space Telescope and the Hubble Space Telescope. The blue inner part of the nebula is optical emission, powered by the collision of winds from Eta Carinae and its unseen companion.[3] Credit: Chandra Science Center and NASA.

The archetype of such a colliding-wind binary system is WR140 (HD 193793), which consists of a 20 solar mass (M☉) Wolf-Rayet star orbiting about a 50 M☉, spectral class O4-5 main sequence star every 7.9 years. The high orbital eccentricity of the pair allows astronomers to observe changes the colliding winds as their separation varies.[4][5] Another prominent example of a colliding-wind binary is thought to be Eta Carinae, one of the most luminous objects in the Milky Way galaxy.[6] The first colliding-wind binary to be detected in the X-ray band outside the Milky Way galaxy was HD 5980, located in the Small Magellanic Cloud.[7]

See also

References

  1. ↑ Volpi, Delia; Blomme, Ronny; De Becker, Michael; Rauw, Gregor (December 2010). "Non-thermal radio emission from colliding-wind binaries: modelling Cyg OB2 No. 8A and No. 9". Proceedings of the International Astronomical Union. 6: 638–639. arXiv:1012.3403Freely accessible. Bibcode:2011IAUS..272..638V. doi:10.1017/S1743921311011689.
  2. ↑ Tuthill, Peter; et al. (August 18, 2006). "Pinwheels in the Quintuplet Cluster". Science. 313 (5789): 935. arXiv:astro-ph/0608427Freely accessible. Bibcode:2006Sci...313..935T. doi:10.1126/science.1128731. PMID 16917053. Retrieved 2011-01-14.
  3. ↑ "Eta Carinae: New View of a Doomed Star". Chandra. June 20, 2007. Retrieved 2011-01-18.
  4. ↑ Dougherty, S. M.; Trenton, V.; Beasley, A. J. (November 2010). "The orbit and distance of WR140". arXiv:1011.0779Freely accessible. Bibcode:2011BSRSL..80..658D.
  5. ↑ Finley, Dave (April 11, 2005). "Scientists Track Collision of Powerful Stellar Winds". National Radio Astronomy Observatory. Retrieved 2011-01-14.
  6. ↑ Groh, J. H.; Madura, T. I.; Owocki, S. P.; Hillier, D. J.; Weigelt, G. (June 2010). "Is Eta Carinae a Fast Rotator, and How Much Does the Companion Influence the Inner Wind Structure?". The Astrophysical Journal Letters. 716 (2): L223–L228. arXiv:1006.4816Freely accessible. Bibcode:2010ApJ...716L.223G. doi:10.1088/2041-8205/716/2/L223.
  7. ↑ Naeye, Bob (February 16, 2007). "First X-Ray Detection of a Colliding-Wind Binary Beyond Milky Way". NASA, Goddard Space Flight Center.


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