Evolution Through Helium Burning — Low-Mass Stars
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Compared to massive stars, those of lower masses (typically M < 2.3M⊙) evolve in a qualitatively different way after the exhaustion of hydrogen in their central regions. There are several reasons for this difference. Low-mass main-sequence stars have small, or no, convective cores and degeneracy is important, if not on the main sequence, then shortly afterwards. In addition they start at a point on the main sequence much closer to the Hayashi line than the starting points of massive stars.
KeywordsMassive Star Main Sequence Asymptotic Giant Branch Evolutionary Track Convective Core
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