Stellar Spectra

  • Hannu Karttunen
  • Pekka Kröger
  • Heikki Oja
  • Markku Poutanen
  • Karl Johan Donner


All our information about the physical properties of stars comes more or less directly from studies of their spectra. In particular, by studying the strength of various absorption lines, stellar masses, temperatures and compositions can be deduced. The line shapes contain detailed information about atmospheric processes.


Spectral Type Main Sequence Equivalent Width Main Sequence Star Bright Star 
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. Böhm-Vitense: Introduction to Stellar Astrophysics Google Scholar
  2. Cambridge University Press, Vol. 1–3, 1989–1992.Google Scholar
  3. Gray: Lectures on Spectral-line Analysis: F, G, and Kstars, Arva, Ontario, 1988.Google Scholar
  4. Gray: The Observation and Analysis of Stellar Photospheres,2nd edition, Cambridge University Press 1992.Google Scholar
  5. Mihalas: Stellar Atmospheres,Freeman 1978.Google Scholar
  6. Novotny: Introduction to Stellar Atmospheres and Interiors,Oxford University Press 1973.Google Scholar

Copyright information

© Springer-Verlag Berlin Heidelberg 2003

Authors and Affiliations

  • Hannu Karttunen
    • 1
  • Pekka Kröger
    • 2
  • Heikki Oja
    • 3
  • Markku Poutanen
    • 4
  • Karl Johan Donner
    • 5
  1. 1.Tuorla ObservatoryUniversity of TurkuPiikkiöFinland
  2. 2.HelsinkiFinland
  3. 3.Observatory and University of HelsinkiHelsinkiFinland
  4. 4.Finnish Geodetic InstituteMasalaFinland
  5. 5.Finnish Geodetic InstituteHelsinkiFinland

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