Final Explosions and Collapse

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


We have seen that stars can evolve to the white-dwarf stage through a sequence of consecutive hydrostatic states if they develop a degenerate core and have final masses less than the Chandrasekhar limit MCh. It is not well known, however, how much mass the stars can have initially (on the main sequence) in order to end this way. Sometimes an upper limit of 4M is quoted, but it may be even up to 10M. The main uncertainty here is the total amount of mass lost by stellar winds.


Neutron Star Detonation Wave White Dwarf Core Mass Detonation Front 
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.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

Copyright information

© Springer-Verlag Berlin Heidelberg 1990

Authors and Affiliations

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

Personalised recommendations