@article{oai:ir.soken.ac.jp:00004259,
 author = {池内, 了 and IKEUCHI, Satoru and NAKAZAWA, Kiyoshi and MURAI, Tadayuki and HOSHI, Reiun and HAYASHI, Chushiro},
 issue = {6},
 journal = {Progress of Theoretical Physics, Progress of Theoretical Physics},
 month = {},
 note = {The evolution of carbon-oxygen stars of 5M⊙, 10M⊙ and 30M⊙ 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 cross 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⊙ and 10M⊙ become unstable on account of the photo-disintegration of iron, while the star of 30M⊙ 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.},
 pages = {1713--1737},
 title = {Stellar Evolution toward Pre-Supernova Stage. I},
 volume = {46},
 year = {1971}
}