= Evolution of a solar-mass star
Core hydrogen fusion supports the <main sequence>. Hydrogen-shell fusion around an inert helium core then produces the <subgiant> and <red giant> phases. Core helium fusion gives the <red clump>, followed by hydrogen- and helium-shell burning on the <Asymptotic giant branch>. Envelope loss can expose a hot <planetary nebula> nucleus before a carbon-oxygen <white dwarf> cools. This sequence concerns a roughly solar-mass star; initial <mass>, composition and mass loss affect detailed tracks and timescales.
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