Transport of Energy by Radiation and Conduction

  • Rudolf Kippenhahn
  • Alfred Weigert
  • Achim Weiss
Chapter
Part of the Astronomy and Astrophysics Library book series (AAL)

Abstract

The energy the star radiates away so profusely from its surface is generally replenished from reservoirs situated in the very hot central region. This requires an effective transfer of energy through the stellar material, which is possible owing to the existence of a non-vanishing temperature gradient in the star. Depending on the local physical situation, the transfer can occur mainly via radiation, conduction, and convection.

Keywords

Free Path Hydrostatic Equilibrium Radiative Transport Stellar Interior Collisional Cross Section 
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.

References

  1. Landau, L.D., Lifshitz, E.M. (1987): Fluid Mechanics, Vol. 6 of Course of Theoretical Physics, 2nd edition reprinted 2004 (Butterworth-Heinemann, Amsterdam)Google Scholar
  2. Weiss, A., Hillebrandt, W., Thomas, H.-C., Ritter, H. (2004) Cox & Giuli’s Principles of Stellar Structure, second edition (Cambridge Scientific Publishers, Cambridge)Google Scholar

Copyright information

© Springer-Verlag Berlin Heidelberg 2012

Authors and Affiliations

  • Rudolf Kippenhahn
    • 1
  • Alfred Weigert
    • 2
  • Achim Weiss
    • 3
  1. 1.GöttingenGermany
  2. 2.Universität HamburgHamburgGermany
  3. 3.Max-Planck-Institut für AstrophysikGarchingGermany

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