Revision of the 15N(p, γ)16O reaction rate and oxygen abundance in H-burning zones

被引：40

作者：

Caciolli, A. ^{[1
,2
,3
]}

Mazzocchi, C. ^{[4
,5
]}

Capogrosso, V. ^{[4
,5
]}

Bemmerer, D. ^{[6
]}

Broggini, C. ^{[1
]}

Corvisiero, P. ^{[7
,8
]}

Costantini, H. ^{[7
,8
]}

Elekes, Z. ^{[9
]}

Formicola, A. ^{[10
]}

Fueloep, Zs. ^{[9
]}

Gervino, G. ^{[11
,12
]}

Guglielmetti, A. ^{[4
,5
]}

Gustavino, C. ^{[10
]}

Gyuerky, Gy. ^{[9
]}

Imbriani, G. ^{[13
,14
]}

Junker, M. ^{[10
]}

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

Marta, M. ^{[6
]}

Menegazzo, R. ^{[1
]}

Palmerini, S. ^{[15
,16
]}

Prati, P. ^{[7
,8
]}

Roca, V. ^{[13
,14
]}

Rolfs, C. ^{[17
]}

Alvarez, C. Rossi ^{[1
]}

Somorjai, E. ^{[9
]}

Straniero, O. ^{[18
]}

Strieder, F. ^{[17
]}

Terrasi, F. ^{[14
,19
]}

Trautvetter, H. P. ^{[17
]}

Vomiero, A. ^{[20
,21
]}

机构：

[1] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[2] Univ Siena, Dipartimento Sci Terra, I-53100 Siena, Italy

[3] CGT, I-52027 San Giovanni Valdarno, Italy

[4] Univ Milan, I-20133 Milan, Italy

[5] Ist Nazl Fis Nucl, Sez Milano, I-20133 Milan, Italy

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

[7] Univ Genoa, I-16146 Genoa, Italy

[8] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy

[9] Inst Nucl Res ATOMKI, H-4026 Debrecen, Hungary

[10] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67010 Assergi, AQ, Italy

[11] Univ Turin, Dipartimento Fis Sperimentale, I-10125 Turin, Italy

[12] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[13] Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy

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

[15] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[16] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[17] Ruhr Univ Bochum, Inst Expt Phys, D-44780 Bochum, Germany

[18] INAF Osservatorio Astron Collurania, I-64100 Teramo, Italy

[19] Univ Naples 2, I-81100 Caserta, Italy

[20] Univ Brescia, CNR IDASC SENSOR Lab, Brescia, Italy

[21] Univ Brescia, Dipartimento Chim & Fis Ingn & Mat, Brescia, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 533卷

基金：

匈牙利科学研究基金会;

关键词：

stars: AGB and post-AGB; nuclear reactions; nucleosynthesis; abundances; novae; cataclysmic variables; THERMONUCLEAR REACTION-RATES; INTERMEDIATE-MASS STARS; GLOBULAR-CLUSTER STARS; RED GIANT STARS; NUCLEAR ASTROPHYSICS; PROTON CAPTURE; NUCLEOSYNTHESIS; BRANCH; ENERGY; LUNA;

D O I：

10.1051/0004-6361/201117475

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The NO cycle takes place in the deepest layer of a H-burning core or shell, when the temperature exceeds T similar or equal to 30 x 10(6) K. The O depletion observed in some globular cluster giant stars, always associated with a Na enhancement, may be due to either a deep mixing during the red giant branch (RGB) phase of the star or to the pollution of the primordial gas by an early population of massive asymptotic giant branch (AGB) stars, whose chemical composition was modified by the hot bottom burning. In both cases, the NO cycle is responsible for the O depletion. Aims. The activation of this cycle depends on the rate of the N-15(p, gamma)O-16 reaction. A precise evaluation of this reaction rate at temperatures as low as experienced in H-burning zones in stellar interiors is mandatory to understand the observed O abundances. Methods. We present a new measurement of the N-15(p, gamma)O-16 reaction performed at LUNA covering for the first time the center of mass energy range 70-370 keV, which corresponds to stellar temperatures between 65 x 10(6) K and 780 x 10(6) K. This range includes the N-15(p, gamma)O-16 Gamow-peak energy of explosive H-burning taking place in the external layer of a nova and the one of the hot bottom burning (HBB) nucleosynthesis occurring in massive AGB stars. Results. With the present data, we are also able to confirm the result of the previous R-matrix extrapolation. In particular, in the temperature range of astrophysical interest, the new rate is about a factor of 2 smaller than reported in the widely adopted compilation of reaction rates (NACRE or CF88) and the uncertainty is now reduced down to the 10% level.

引用

页数：6

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