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Wolf-Rayet star

Wolf-Rayet stars (often referred to as WR stars) are evolved, massive stars (over 20 solar masses), and are losing their mass rapidly by means of a very strong stellar wind, with speeds up to 2000 km/s. While our own sun loses 10−16 of its own mass every year, a Wolf-Rayet star loses 10−5 solar masses a year. These stars are also very hot: their surface temperatures are in the range of 25,000 K to 50,000 K..

Hubble Space Telescope image of nebula M1-67 around Wolf Rayet star WR 124

Observation history

In 1867, astronomers using the 40 cm Foucault telescope at the Paris Observatory, discovered three stars in the constellation Cygnus that displayed broad emission bands on an otherwise continuous spectrum.[1] The astronomer's names were Charles Wolf and Georges Rayet, and thus this category of stars became named Wolf-Rayet (WR) stars.[2] Most stars display absorption bands in the spectrum, as a result of overlaying elements absorbing light energy at specific frequencies. The number of stars with emission lines is quite low, so these were clearly unusual objects.

The nature of the emission bands in the spectra of a Wolf-Rayet star remained a mystery for several decades. Edward C. Pickering theorized that the lines were caused by an unusual state of hydrogen, and it was found that this "Pickering series" of lines followed a pattern similar to the Balmer series, when half-integral quantum numbers were substituted. It was later shown that the lines resulted from the presence of helium; a gas that was discovered in 1868.[3]

By 1929, the width of the emission bands was being attributed to the Doppler effect, and hence that the gas surrounding these stars must be moving with velocities of 300–2400 km/s along the line of sight. The conclusion was that a Wolf-Rayet star is continually ejecting gas into space, producing an expanding envelope of nebulous gas. The force ejecting the gas at the high velocities observed is radiation pressure.[4]

In addition to helium, emission lines of carbon, oxygen and nitrogen were identified in the spectra of Wolf-Rayet stars.[5] In 1938, the International Astronomical Union classified the spectra of Wolf-Rayet stars into types WN and WC, depending on whether the spectrum was dominated by lines of nitrogen or carbon-oxygen respectively.[6]


Wolf-Rayet stars are a normal stage in the evolution of very massive stars, in which strong, broad emission lines of helium and nitrogen ("WN" sequence) or helium, carbon, and oxygen ("WC" sequence) are visible. Due to their strong emission lines they can be identified in nearby galaxies. About 230 Wolf-Rayets are known in our own Milky Way Galaxy[7], about 100 are known in the Large Magellanic Cloud, while only 12 have been identified in the Small Magellanic Cloud.

Conti (1976)[8] originally proposed that the WR stars as a class are descended from massive O-stars in which the strong stellar winds characteristic of extremely luminous stars have ejected the unprocessed outer H-rich layers. The characteristic emission lines are formed in the extended and dense high-velocity wind region enveloping the very hot stellar photosphere, which produces a flood of UV radiation that causes florescence in the line-forming wind region. This ejection process uncovers in succession, first the nitrogen-rich products of CNO cycle burning of hydrogen (WN stars), and later the carbon-rich layer due to He burning (WC & WO stars). Most of these stars are believed finally to progress to become supernovae of Type Ib or Type Ic. A few (roughly 10%) of the central stars of planetary nebulae are, despite their much lower (typically ~0.6 solar) masses, also observationally of the WR-type; i.e., they show emission line spectra with broad lines from helium, carbon and oxygen. Denoted [WR], they are much older objects descended from evolved low-mass stars and are closely related to white dwarfs, rather than to the very young, very massive stars that comprise the bulk of the WR class.[9]

It is possible for a Wolf-Rayet star to progress to a "collapsar" stage in its death throes: This is when the core of the star collapses to form a black hole, pulling in the surrounding material. This is thought to be the precursor of a long gamma-ray burst.

The best known (and most visible) example of a Wolf-Rayet star is Gamma 2 Velorum (γ² Vel), which is a bright star visible to those located south of 40 degrees northern latitude. One of the members of the star system (Gamma Velorum is actually at least six stars) is a Wolf-Rayet star. Due to the exotic nature of its spectrum (bright emission lines in lieu of dark absorption lines) it is dubbed the "Spectral Gem of Southern Skies".[10]

See also

* Gamma-ray burst
* Hypernova
* Starburst galaxy
* Wolf-Rayet nebula
* WR 104


  • ^ Huggins, William (1890-1). "On Wolf and Rayet's Bright-Line Stars in Cygnus". Proceedings of the Royal Society of London 49: 33-46. Retrieved on 2007-09-06.
  • ^ Murdin, P. (2001). Wolf, Charles J E (1827-1918). Bristol: Institute of Physics Publishing. DOI:10.1888/0333750888/4101. 
  • ^ Fowler, A. (1912). "Hydrogen, Spectrum of, Observations of the principal and other series of lines in the". Monthly Notices of the Royal Astronomical Society 73: 62-105. Retrieved on 2007-02-04.
  • ^ Beals, C. S. (1929). "On the nature of Wolf-Rayet emission". Monthly Notices of the Royal Astronomical Society 90: 202-212. Retrieved on 2007-09-10.
  • ^ Beals, C. S. (1933). "Classification and temperatures of Wolf-Rayet stars". The Observatory 56: 196-197. Retrieved on 2007-09-10.
  • ^ Swings, P. (1942). "The Spectra of Wolf-Rayet Stars and Related Objects". Astrophysical Journal 95: 112-133. Retrieved on 2007-09-10.
  • ^ van der Hucht, K.A. 2001, New Astron. Rev., 45:135
  • ^ Conti, P.S. 1976, in Proc. 20th Colloq Int. Astrophys. Liege
  • ^ Crowther, P.A., 2007, Physical Properties of Wolf-Rayet Stars, Ann. Rev. A&A, 45:177-219.
  • ^ Hoffleit. The Bright Star Catalogue, 5th Revised Ed.. Retrieved on August 08, 2007.

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