Stellar Evolution. VII. The Evolution of a 2.25 Mₛᵤₙ Star from the Main Sequence to the Helium-Burning Phase

Prior to reaching the giant phase, the evolution of a 2.25 Mo star is qualitatively identical with the evolution of more massive stars examined in earlier papers of this series. After reaching the giant branch, 2.25 Mo evolution is quite similar to that of lighter stars examined earlier. The 2.25 Mo star is very near the limiting mass above which helium flashing will not occur. Near the top of the red-giant branch, nuclear burning via the N14 018 reactions is initiated in an electron-degenerate core. The ensuing development of the "N14-flash" phase is followed until the star begins to descend from the red-giant tip