Stellar Evolution toward Pre-Supernova Stage. I : Carbon and Oxygen Stars of 5M_&odoi;, 10M_&odoi; and 30M_&odoi;

概要

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The evolution of carbon-oxygen stars of 5M&odoi;, 10M&odoi; and 30M&odoi; is computed from a pre-carbon-burning contraction stage to a pre-supernova stage through the phases of central burning of C, Ne, O, Mg, Si and Ni. These stars are regarded as representing the cores inside the helium shell-source of ordinary evolved stars. The computation is made for the two alternative cases, with and without neutrino production by electron-neutrino interaction. It is found that in the case without neutrinos the stars contract nearly homologously with structure almost similar to the polytrope of index 3 and each central burning begins gently. Finally, the stars of 5M&odoi; and 10M&odoi; become unstable on account of the photo-disintegration of iron, while the star of 30M&odoi; becomes unstable in a central neon-burning phase by electron pair production. In the case with neutrinos, energy loss through neutrinos accelerates the evolution and, at the same time, gives rise to a deviation from the homologous contraction. The stars tend to be centrally condensed with evolution and both O and Si begin to burn at the center as strong flashes. Finally, all of the stars become unstable after the formation of an iron core.
理論物理学刊行会の論文
1971-12-25