Final Explosions and Collapse
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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.
KeywordsNeutron Star Detonation Wave White Dwarf Core Mass Detonation Front
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