Shell and explosive hydrogen burning

被引：30

作者：

Boeltzig, A. ^{[1
]}

Bruno, C. G. ^{[2
]}

Cavanna, F. ^{[3
]}

Cristallo, S. ^{[4
,5
]}

Davinson, T. ^{[2
]}

Depalo, R. ^{[6
,7
]}

deBoer, R. J. ^{[8
]}

Di Leva, A. ^{[5
,9
]}

Ferraro, F. ^{[3
]}

Imbriani, G. ^{[5
,9
]}

Marigo, P. ^{[6
]}

Terrasi, F. ^{[5
,10
]}

Wiescher, M. ^{[8
]}

机构：

[1] Gran Sasso Sci Inst, Laquila, Italy

[2] Univ Edinburgh, Sch Phys & Astron, SUPA, Edinburgh, Midlothian, Scotland

[3] Univ Genoa, Dipartimento Fis, Genoa, Italy

[4] Osservatorio Astron Collurania, INAF, Teramo, Italy

[5] Ist Nazl Fis Nucl, Sez Napoli, I-80125 Naples, Italy

[6] Univ Padua, Dipartimento Fis & Astron, Padua, Italy

[7] Ist Nazl Fis Nucl, Sez Padova, Padua, Italy

[8] Univ Notre Dame, Joint Inst Nucl Astrophys, Inst Struct & Nucl Astrophys, Notre Dame, IN 46556 USA

[9] Univ Naples Federico II, Dipartimento Fis, Naples, Italy

[10] Univ Naples 2, Dipartimento Matemat & Fis, Caserta, Italy

来源：

EUROPEAN PHYSICAL JOURNAL A | 2016年 / 52卷 / 04期

基金：

美国国家科学基金会;

关键词：

LOW-ENERGY RESONANCES; EVOLVED STARS. I; REACTION-RATES; PROTON CAPTURE; MG-25(P; GAMMA)AL-26; REACTION; NOVA NUCLEOSYNTHESIS; GAMMA)AL-26 REACTION; AGB STARS; S-FACTOR; MASS;

D O I：

10.1140/epja/i2016-16075-4

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：

The nucleosynthesis of light elements, from helium up to silicon, mainly occurs in Red Giant and Asymptotic Giant Branch stars and Novae. The relative abundances of the synthesized nuclides critically depend on the rates of the nuclear processes involved, often through non-trivial reaction chains, combined with complex mixing mechanisms. In this paper, we summarize the contributions made by LUNA experiments in furthering our understanding of nuclear reaction rates necessary for modeling nucleosynthesis in AGB stars and Novae explosions.

引用

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