= Post-asymptotic giant branch evolution
After substantial envelope loss on the <Asymptotic giant branch>, a low- or intermediate-mass star's exposed core heats while its radius shrinks, often at approximately constant <luminosity> during continued shell burning. It may ionize the expelled envelope as a <planetary nebula>. After the remaining nuclear fuel is depleted, its luminosity decreases and it joins a <white dwarf> cooling track. Evolutionary tracks on the <Hertzsprung-Russell diagram> connect the central-star temperature and luminosity with core mass and elapsed time.
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