Evolution Through Helium Burning — Low-Mass Stars

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


Compared to massive stars, those of lower masses (typically M < 2.3M) evolve in a qualitatively different way after the exhaustion of hydrogen in their central regions. There are several reasons for this difference. Low-mass main-sequence stars have small, or no, convective cores and degeneracy is important, if not on the main sequence, then shortly afterwards. In addition they start at a point on the main sequence much closer to the Hayashi line than the starting points of massive stars.


Massive Star Main Sequence Asymptotic Giant Branch Evolutionary Track Convective Core 
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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Copyright information

© Springer-Verlag Berlin Heidelberg 1990

Authors and Affiliations

  • Rudolf Kippenhahn
    • 1
  • Alfred Weigert
  1. 1.GöttingenGermany

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