Final Explosions and Collapse

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

Abstract

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. Other stars certainly undergo explosions, ejecting a large part of their mass, if not disrupting completely. In the case where a neutron star is left as a remnant the core must have undergone a collapse, since it cannot reach the neutron-star stage by a hydrostatic sequence. Collapse and explosions are connected with supernova events, and although the theory and the numerical models are well developed and far advanced, not all questions concerning the different mechanisms have been answered, and not all different observed phenomena can be explained so far. In this section we discuss some basic effects which certainly play an important role in late phases of more massive stars, and that will probably remain to be an important part of full theories of supernovae.

Keywords

Black Hole Neutron Star Massive Star White Dwarf Core Mass 
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 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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