Improved Direct Measurement of the 64.5 keV Resonance Strength in the 17O(p,α)14N Reaction at LUNA

被引：58

作者：

Bruno, C. G. ^{[1
]}

Scott, D. A. ^{[1
]}

Aliotta, M. ^{[1
]}

Formicola, A. ^{[2
]}

Best, A. ^{[3
,4
]}

Boeltzig, A. ^{[5
]}

Bemmerer, D. ^{[6
]}

Broggini, C. ^{[7
]}

Caciolli, A. ^{[7
,8
]}

Cavanna, F. ^{[9
,10
]}

Ciani, G. F. ^{[5
]}

Corvisiero, P. ^{[9
,10
]}

Davinson, T. ^{[1
]}

Depalo, R. ^{[7
,8
]}

Di Leva, A. ^{[3
,4
]}

Elekes, Z. ^{[11
]}

Ferraro, F. ^{[9
,10
]}

Fulop, Zs. ^{[11
]}

Gervino, G. ^{[12
,13
]}

Guglielmetti, A. ^{[14
,15
]}

Gustavino, C. ^{[16
]}

Gyurky, Gy. ^{[11
]}

Imbriani, G. ^{[3
,4
]}

Junker, M. ^{[2
]}

Menegazzo, R. ^{[7
]}

Mossa, V. ^{[17
,18
]}

Pantaleo, F. R. ^{[17
,18
]}

Piatti, D. ^{[7
,8
]}

Prati, P. ^{[9
,10
]}

Somorjai, E. ^{[11
]}

Straniero, O. ^{[19
]}

Strieder, F. ^{[20
]}

Szuecs, T. ^{[6
]}

Takacs, M. P. ^{[6
,20
]}

Trezzi, D. ^{[14
,15
]}

机构：

[1] Univ Edinburgh, Sch Phys & Astron, SUPA, Edinburgh EH9 3FD, Midlothian, Scotland

[2] Ist Nazl Fis Nucl, LNGS, I-67100 Assergi, Italy

[3] Univ Napoli Federico II, I-80126 Naples, Italy

[4] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy

[5] Gran Sasso Sci Inst, Ist Nazl Fis Nucl, Viale F Crispi 7, I-67100 Laquila, Italy

[6] Helmholtz Zentrum Dresden Rossendorf, Bautzner Landstr 400, D-01328 Dresden, Germany

[7] Ist Nazl Fis Nucl, Sez Padova, Via F Marzolo 8, I-35131 Padua, Italy

[8] Univ Padua, Via F Marzolo 8, I-35131 Padua, Italy

[9] Univ Genoa, Via Dodecaneso 33, I-16146 Genoa, Italy

[10] Ist Nazl Fis Nucl, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy

[11] Inst Nucl Res MTA ATOMKI, POB 51, HU-4001 Debrecen, Hungary

[12] Univ Turin, Via P Giuria 1, I-10125 Turin, Italy

[13] Ist Nazl Fis Nucl, Sez Torino, Via P Giuria 1, I-10125 Turin, Italy

[14] Univ Milan, Via G Celoria 16, I-20133 Milan, Italy

[15] Ist Nazl Fis Nucl, Sez Milano, Via G Celoria 16, I-20133 Milan, Italy

[16] Ist Nazl Fis Nucl, Sez Roma La Sapienza, Piazzale A Moro 2, I-00185 Rome, Italy

[17] Univ Bari, I-70125 Bari, Italy

[18] Ist Nazl Fis Nucl, Sez Bari, I-70125 Bari, Italy

[19] Osservatorio Astron Collurania, Teramo, Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy

[20] South Dakota Sch Mines, 501 E St Joseph St, Rapid City, SD 57701 USA

来源：

PHYSICAL REVIEW LETTERS | 2016年 / 117卷 / 14期

基金：

英国科学技术设施理事会;

关键词：

REACTION-RATES; CNO ISOTOPES; RED GIANTS; GRAPHS; TABLES;

D O I：

10.1103/PhysRevLett.117.142502

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

The O-17(p,alpha)N-14 reaction plays a key role in various astrophysical scenarios, from asymptotic giant branch stars to classical novae. It affects the synthesis of rare isotopes such as O-17 and F-18, which can provide constraints on astrophysical models. A new direct determination of the E-R = 64.5 keV resonance strength performed at the Laboratory for Underground Nuclear Astrophysics (LUNA) accelerator has led to the most accurate value to date omega gamma = 10.0 +/- 1.4(stat) +/- 0.7(syst) neV, thanks to a significant background reduction underground and generally improved experimental conditions. The (bare) proton partial width of the corresponding state at E-x = 5672 keV in F-18 is Gamma(p) = 35 +/- 5(stat) +/- 3(syst) neV. This width is about a factor of 2 higher than previously estimated, thus leading to a factor of 2 increase in the O-17(p,alpha)N-14 reaction rate at astrophysical temperatures relevant to shell hydrogen burning in red giant and asymptotic giant branch stars. The new rate implies lower O-17/O-16 ratios, with important implications on the interpretation of astrophysical observables from these stars.

引用

页数：6

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