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Neutrino process in massive stars
https://repo.qst.go.jp/records/2003084
https://repo.qst.go.jp/records/2003084c05bc353-4c83-4115-b110-2c760566f78f
| アイテムタイプ | 会議発表用資料 / Presentation(1) | |||||||
|---|---|---|---|---|---|---|---|---|
| 公開日 | 2026-03-27 | |||||||
| タイトル | ||||||||
| タイトル | Neutrino process in massive stars | |||||||
| 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_c94f | |||||||
| 資源タイプ | conference presentation | |||||||
| 著者 |
Hayakawa Takehito
× Hayakawa Takehito
|
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| 抄録 | ||||||||
| 内容記述 | A huge number of neutrinos are radiated from proto-neutronstars in the final phase of massive stars.These neutrinos generate rare isotopes in outer layers.The production rates of the neutrino-isotopes dependon the neutrino energy spectra of 3 group neutrinos.Thus, the distribution to the 3 groupsand their energy spectra are key parameters forthe final abundances.Some long-lived radioisotopes such as 10Be and 92Nbare important for understanding the origin ofradioisotopes being at the solar system formationand interstellar media.We discuss the perspective these phenomena. | |||||||
| 会議概要（会議名, 開催地, 会期, 主催者等） | ||||||||
| 内容記述 | OMEG Institute seminar | |||||||
| 発表年月日 | ||||||||
| 日付 | 2026-03-26 | |||||||
