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


Stars having remarkable emission lines in the optical spectra are called emission-line stars and widely distributed on the Hertzsprung-Russell (HR) diagram including various stellar types:
  1. (1)

    Early type stars—Wolf-Rayet (WR) stars, Of, Oe/Be/Ae stars, Luminous Blue Variables (LBV).

  2. (2)

    Late type stars—dMe stars, flare stars, red giants, Mira variables.

  3. (3)

    Close binaries—Algol stars, cataclysmic variables (CV), symbiotic stars.

  4. (4)

    Pre-main sequence stars—Herbig Be/Ae stars, T Tauri stars.



Emission Line Planetary Nebula Stellar Atmosphere Bright Line Tauri Star 


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Further reading

  1. Hearnshaw, J. B. (1986). The Analysis of Starlight, One Hundred and Fifty Years of Astronomical Spectroscopy. Cambridge University Press, Cambridge.Google Scholar
  2. Leverington, D. (1995). A History of Astronomy from 1890 to the Present. Springer-Verlag, Berlin.Google Scholar
  3. Tassoul, J.-L. and Tassoul, M. (2004). A Concise History of Solar and Stellar Physics. Princeton University Press, Princeton, NJ.Google Scholar


  1. Beals, C. S. (1929). On the nature of Wolf-Rayet emission. MNRAS, 90, 202–212.ADSGoogle Scholar
  2. Bowen, I. S. (1928). The origin of the nebular lines and the structure of the planetary nebulae. Ap. J. 67, 1–15.CrossRefADSGoogle Scholar
  3. Burgers, J. M. and van de Hulst, H. C. (1951). Problems of cosmical aerodynamics. Proceedings of the Symposium on the Motion of Gaseous Masses of Cosmical Dimensions, Paris, August 16–19, 1949.Google Scholar
  4. Cannon, A. J. (1916). Spectra having bright lines. Ann. Harvard Coll. Obs. 76, 19–42.ADSGoogle Scholar
  5. Deutsch, A. J. and Merrill, P. W. (1959). Gross differences between the R Cygni spectra at two successive maxima. Ap. J. 130, 570–577.CrossRefADSGoogle Scholar
  6. Henyey, L. G. (1938). The theory of cyclic transitions. Ap. J. 88, 133–163.MATHCrossRefADSGoogle Scholar
  7. Herbig, G. H. (1952). Emission-line stars in galactic nebulosities. JRAS. Canada, 46, 222–233.ADSGoogle Scholar
  8. Herbig, G. H. (1958). Stars of F, G, and K with emission lines: Introductory report. Etoiles a raies d’emission. Liège Conference, July 1957, 251–270.Google Scholar
  9. Herbig, G. H. (1960). The spectra of Be and Ae type stars associated with nebulosity. Ap. J. Suppl. 4, 337–368.CrossRefADSGoogle Scholar
  10. Hertzsprung, E. (1924). Note on a peculiar star or nova of short duration. Bull. Astr. Inst. 2, 87–88.ADSGoogle Scholar
  11. Joy, A. H. (1945). T Tauri variable stars. Ap. J. 102, 168–195.CrossRefADSGoogle Scholar
  12. Joy, A. H. (1948). Emission lines in stellar spectra. Ap. J. 53, 107.ADSGoogle Scholar
  13. Joy, A. H. and Humason, M. L. (1949). Observations of the faint dwarf star L726-8. PAS. Pacific, 61, 133–134.ADSGoogle Scholar
  14. Menzel, D. H. (ed.) (1962). Selected Papers on Physical Processes in Ionized Plasmas, Dover, New York.Google Scholar
  15. Menzel, D. H. (ed.) (1966) Selected Papers on the Transfer of Radiation. Dover, NY.Google Scholar
  16. Merrill, P. W. (1933). Four stars whose spectra have bright helium lines. Ap. J. 77, 44–50.CrossRefADSGoogle Scholar
  17. Merrill, P. W. (1958). Symbiosis in astronomy: Introductory report. Etoiles a raies d’emission. Liège Conference, July 1957, 436–448.Google Scholar
  18. Miyamoto, S. (1943). On the envelopes of peculiar stars (in Japanese). Tenmongaku Iho 2, 157–186.Google Scholar
  19. Miyamoto, S. (1953). The atmospheres of the P Cygni stars. PAS. Japan, 5, 55–73.ADSGoogle Scholar
  20. Parker, E. N. (1958). Dynamics of interplanetary gas and magnetic fields. Ap. J. 128, 664–676.CrossRefADSGoogle Scholar
  21. Pickering, E. C. (1890). The Draper Catalogue of stellar spectra photographed with the 8-inch Bache telescope as a part of Henry Draper Memorial. Harvard College Obs. Ann., 27, 1–388.ADSGoogle Scholar
  22. Pikel’ner, S. B. (1954). Spectrophotometric investigation on the mechanisms of excited filamentary nebulae. Izv. Krimk. Astrofiz. Obs. 12, 93.Google Scholar
  23. Roques, P. (1955). A search for flare stars. PASP, 67, 34–38.CrossRefADSGoogle Scholar
  24. Rosseland, S. (1926). On the Origin of bright lines in stellar spectra. Ap. J., 63, 218–235.CrossRefADSGoogle Scholar
  25. Rosseland, S. (1936). Stars with extensive envelopes. Theoretical Astrophysics. Chapter 20. Oxford University Press, Oxford.Google Scholar
  26. Schatzman, E. (1949). The heating of the solar corona and chromosphere. Ann. d’Ap., 12, 203–218.ADSGoogle Scholar
  27. Sobolev, V. V. (1847). Moving Envelopes of Stars (in Russian, English translation is published from Harvard Univ. Press in 1960).Google Scholar
  28. Struve, O. (1931). On the origin of bright lines in spectra of stars of class B. Ap. J., 73, 94–103.CrossRefADSGoogle Scholar
  29. Struve, O. (1942). Extended stellar atmospheres: A review of the problems of gaseous shells. Ap. J., 95, 134–151.MATHCrossRefADSGoogle Scholar
  30. van Maanen, A. (1940). The photographic determination of stellar parallaxes with the 60-and 100-inch telescopes Ap. J., 91, 503–506.CrossRefADSGoogle Scholar
  31. Wallerstein, G. (1959). The shock-wave model for the population II Cepheids. Ap. J., 130, 560–569.CrossRefADSGoogle Scholar
  32. Wilson, O. C. and Bappu, M. K. V. (1957). H and K emission in late type stars: Dependence of line width on luminosity and related topics. Ap. J., 125, 661–683.CrossRefADSGoogle Scholar
  33. Zanstra, H. (1927). An application of the quantum theory to the luminosity of diffuse nebulae. Ap. J., 65, 50–70.CrossRefADSGoogle Scholar

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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