Transport of Energy by Radiation and Conduction

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


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.


Free Path Hydrostatic Equilibrium Radiative Transport Stellar Interior Collisional Cross Section 
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  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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