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Stellar Evolution toward Pre-Supernova Stage. I
https://ir.soken.ac.jp/records/4259
https://ir.soken.ac.jp/records/4259f93a89f9-6f06-4b29-be4a-9a572620a853
| Item type | 学術雑誌論文 / Journal Article(1) | |||||||||||||||
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| 公開日 | 2014-02-19 | |||||||||||||||
| タイトル | ||||||||||||||||
| タイトル | Stellar Evolution toward Pre-Supernova Stage. I | |||||||||||||||
| タイトル | ||||||||||||||||
| タイトル | Stellar Evolution toward Pre-Supernova Stage. I | |||||||||||||||
| 言語 | en | |||||||||||||||
| 言語 | ||||||||||||||||
| 言語 | eng | |||||||||||||||
| 資源タイプ | ||||||||||||||||
| 資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||||||||||||
| 資源タイプ | journal article | |||||||||||||||
| アクセス権 | ||||||||||||||||
| アクセス権 | metadata only access | |||||||||||||||
| アクセス権URI | http://purl.org/coar/access_right/c_14cb | |||||||||||||||
| 著者 |
IKEUCHI, Satoru
× IKEUCHI, Satoru
× NAKAZAWA, Kiyoshi
× MURAI, Tadayuki
× HOSHI, Reiun
× HAYASHI, Chushiro
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| 著者別名 |
池内, 了
× 池内, 了
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| 抄録 | ||||||||||||||||
| 内容記述タイプ | Abstract | |||||||||||||||
| 内容記述 | 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. |
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| 書誌情報 |
Progress of Theoretical Physics en : Progress of Theoretical Physics 巻 46, 号 6, p. 1713-1737, 発行日 1971 |
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| 出版者 | ||||||||||||||||
| 出版者 | Oxford University Press | |||||||||||||||
| ISSN | ||||||||||||||||
| 収録物識別子タイプ | ISSN | |||||||||||||||
| 収録物識別子 | 0033-068X | |||||||||||||||
| DOI | ||||||||||||||||
| 識別子タイプ | DOI | |||||||||||||||
| 関連識別子 | https://doi.org/10.1143/PTP.46.1713 | |||||||||||||||
| 関連名称 | 10.1143/PTP.46.1713 | |||||||||||||||
| 権利 | ||||||||||||||||
| 権利情報 | © 2014 The Physical Society of Japan | |||||||||||||||
