 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.