Neutrino Nucleosynthesis in Supernovae

被引：0

作者：

Yoshida, Takashi ^{[1
]}

Suzuki, Toshio ^{[2
]}

Chiba, Satoshi ^{[3
]}

Kajino, Toshitaka ^{[1
,4
]}

Yokomakura, Hidekazu ^{[5
]}

Kimura, Keiichi ^{[5
]}

Takamura, Akira ^{[6
]}

Hartmann, Dieter H. ^{[7
]}

机构：

[1] Natl Astron Observ Japan, Div Theoret Astron, 2-21-1 Osawa, Tokyo 1818588, Japan

[2] Nihon Univ, Coll Human & Sci, Dept Phys, Tokyo 102, Japan

[3] Japan Atom Energy Agcy, Adv Sci Res Ctr, Tokyo, Japan

[4] Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1138654, Japan

[5] Nagoya Univ, Grad Sch Sci, Dept Phys, Nagoya, Aichi, Japan

[6] Toyota Natl Coll Technol, Dept Math, Toyota, Japan

[7] Clemson Univ, Dept Phys & Astron, Clemson, SC 29631 USA

来源：

PERSPECTIVES IN NUCLEAR PHYSICS | 2009年 / 1120卷

关键词：

supernovae; nucleosynthesis; neutrino induced processes; LIGHT-ELEMENT SYNTHESIS; NU-PROCESS; EXPLOSIONS;

D O I：

暂无

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

Neutrino nucleosynthesis is an important synthesis process for light elements in supernovae. One important physics input of neutrino nucleosynthesis is cross sections of neutrino-nucleus reactions. The cross sections of neutrino-C-12 and He-4 reactions are derived using new shell model Hamiltonians. With the new cross sections, light element synthesis of a supernova is investigated. The appropriate range of the neutrino temperature for supernovae is constrained to be between 4.3 MeV and 6.5 MeV from the B-11 abundance in Galactic chemical evolution. Effects by neutrino oscillations are also discussed.

引用

页码：165 / +

页数：2

共 20 条

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