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Early-type Emission-line Stars

  • Tomokazu Kogure
  • Kam-Ching Leung
Part of the Astrophysics and Space Science Library book series (ASSL, volume 342)

Abstract

Wolf-Rayet (WR) stars owe its name to the discoverers, C. Wolf and G. Rayet. They are one of the most conspicuous stellar objects in spectral features, activities, and in the processes of stellar evolution. They are spectroscopically characterized by the following features.

Keywords

Emission Line Spectral Type Stellar Wind Planetary Nebula Luminous Blue Variable 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Further reading

  1. Balona, L. A., Henrichs, H. F., and Le Contel, J. M. (eds.) (1994). IAU Symp. No. 162, Pulsation, Rotation and Mass Loss in Early-Type Stars. Kluwer, Dordrecht.Google Scholar
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  3. de Groot, M. and Sterken, C. (eds.) (2001). ASP Conf. Vol. 233. P Cygni 2000: 400 Years of Progress. San Francisco, CA.Google Scholar
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  5. Smith, M. and Henrichs, H. F. (eds.) (2000). IAU Coll. 175, ASP Conf. Ser. Vol. 214. The Be Phenomenon in Early-Type Stars. San Francisco, CA.Google Scholar
  6. van der Hucht, K. A. and Williams, P. M. (eds.) (1995). IAU Symp. 163, Wolf-Rayet Stars, Binaries, Colliding Winds, Pulsation. Kluwer, Dordrecht.Google Scholar
  7. van der Hucht, K. A., Herrero, A., and Cesar, E. (eds) (2003). IAU Symp. 212, A Massive Star Odyssey: From Main Sequence to Supernova. Ast. Soc. Pacific. San Francisco, CA.Google Scholar

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Copyright information

© Springer Science+Business Media, LLC 2007

Authors and Affiliations

  • Tomokazu Kogure
    • 1
  • Kam-Ching Leung
    • 2
    • 3
    • 4
  1. 1.Kyoto UniversityYawata, KyotoJapan
  2. 2.Institute of Astronomy and AstrophysicsAcademia SinicaTaiwan, China
  3. 3.Department of Physics & AstronomyUniversity of Nebraska-LincolnLincolnUSA
  4. 4.Brace LaboratoryUSA

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