Stellar Spectra

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

Abstract

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.

Keywords

Titanium Magnesium Zirconium Mercury Chromium 

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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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