= 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.
Back to article page
