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Stellar Structure

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

Abstract

The stars are huge gas spheres, hundred thousands or millions of times more massive than the Earth. A star such as the Sun can go on shining steadily for thousands of millions of years. This is shown by studies of the prehistory of the Earth, which indicate that the energy radiated by the Sun has not changed by much during the last four thousand million years. The equilibrium of a star must remain stable for such periods.

Keywords

Radiation Pressure Fermi Momentum Helium Nucleus Stellar Structure Mass Absorption Coefficient 
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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References

  1. Clayton, D. D. (1968/1983): Principles of Stellar Evolution and Nucleosynthesis (McGraw-Hill, New York/University of Chicago Press, Chicago)Google Scholar
  2. Novotny, E. (1973): Introduction to Stellar Atmospheres and Interiors (Oxford University Press, New York)Google Scholar
  3. Schwarzschild, M. (1958/1965): Structure and Evolution of the Stars (Princeton University Press, Princeton/Dover, New York)Google Scholar

Copyright information

© Springer-Verlag Berlin Heidelberg 1994

Authors and Affiliations

  • Hannu Karttunen
    • 1
  • Pekka Kröger
    • 2
  • Heikki Oja
    • 3
  • Markku Poutanen
    • 4
  • Karl Johan Donner
    • 3
  1. 1.Center for Scientific Computing Ltd.EspooFinland
  2. 2.HelsinkiFinland
  3. 3.ObservatoryUniversity of HelsinkiFinland
  4. 4.Finnish Geodetic InstituteHelsinkiFinland

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