Low Mass Star
Stars with an initial mass on the Zero Age Main Sequence lower than ∼1.2 M⊙ (spectral types later than G) are called low mass stars. They evolve on timescales of ∼several Gyr, fusing H through the p-p chains and going through the Asymptotic Giant Branch (AGB) phase of double shell (H- and He-) burning (fusion). After the Planetary nebula phase, they finally leave behind a white dwarf. They play a limited role in galactic chemical evolution, mainly by “astrating” (i.e., destroying) fragile nuclides like deuterium. Because of their long lifetimes, which would facilitate the development of complex life, they are major targets for extrasolar planet research.