The Hayashi Line

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


We have seen that convection can occur in quite different regions of a star. In this section we consider the limiting case of fully convective stars, i.e. stars which are convective in the whole interior from centre to photosphere, while only the atmosphere remains radiative. The Hayashi Line (HL) is defined as the locus in the Hertzsprung–Russell diagram of fully convective stars of given parameters (mass M and chemical composition).


Main Sequence Interior Solution Hydrostatic Equilibrium Radiative Region Ionization Zone 
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.


  1. Hayashi, C. (1961): Publ. Astron. Soc. Japan 13, 450ADSGoogle Scholar
  2. Henyey, L.G., Vardya, M.S., Bodenheimer, P.L. (1965): Astrophys. J. 142, 841ADSCrossRefGoogle 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

Personalised recommendations