The Chandrasekhar limit determines whether a star ends its life as a smoldering white dwarf, or explodes in a supernova to become a neutron star or black hole.
, eventually becoming a planetary nebula that surrounds a scorching hot, albeit gradually cooling stellar core known as a white dwarf.
This isn’t the end for all stars, however. Some have enough mass to push past this white dwarf phase and initiate further nuclear fusion, a supernova, and the transformation into an exotic stellar remanent. What protects a Chandrasekhar mass star against further collapse? A white dwarf with a mass of 1.4 solar masses or less can’t initiate carbon burning but continues to contract until this is halted byThis is the principle from quantum physics that prevents two electrons from occupying the same quantum state and essentially prevents them from cramming too close together, providing the pressure to support the white dwarf against its own gravity. But even this limit can be exceeded.In stellar cores with a mass greater than 1.
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