A star's fate is almost entirely determined by its mass. The main sequence is the stable hydrogen-burning phase: L ~ M³·⁵ (a star twice as massive shines 11× brighter, lives 6× less). After exhausting hydrogen the star expands onto the giant branch. Below 8 solar masses: planetary nebula + white dwarf. Above: supernova, then neutron star or black hole. Chandrasekhar limit: 1.44 M☉. Tolman-Oppenheimer-Volkoff limit: ~3 M☉.
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