Advanced Phases of Evolution of Population II Stars ---Growth of the Carbon Core and Shell Helium Flashes---

Details Advanced Phases of Evolution of Population II Stars ---Growth of the Carbon Core and Shell Helium Flashes--- Advanced Phases of Evolution of Population II Stars ---Growth of the Carbon Core and Shell Helium Flashes---

Dec 1965

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1965pthph..34..885h&link_type=abstract

Progress of Theoretical Physics, Vol. 34, No. 6, pp. 885-911

Physics

18

Scientific paper

As the extension of our previous work, calculations have been made of the evolution of a population II star after the formation of a carbon core. We start from a stage when the star has an inactive hydrogen shell-source, a helium-burning shell-source and a partially-degenerate isothermal carbon core. The luminosity due to shell helium-burning attains a maximum value, 1.6times10^3 L_odot, when the core mass grows to 0.47 M_odot. After this stage, helium-burning decays rapidly while the hydrogen shell-source becomes active. In the next phase the mass of the helium grows through shell hydrogen-burning and the inner layers of the helium zoen begin to be degenerate. The gravitational contraction of the helium zone gives rise to the heating of the helium shell-source, until the second helium flash sets in at the degenerate shell when the mass interior to the hydrogen shell-source becomes 0.61 M_odot. The subsequent evolution is, in general, the repetition of the preceding phases. The third helium flash sets in when the mass interior to the hydrogen shell-source becomes about 0.7 M_odot and the luminosity is about 8times10^3 L_odot.

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