The impact of the revised 17O(p, α)14N reaction rate on 17O stellar abundances and yields

被引：29

作者：

Straniero, O. ^{[1
,2
]}

Bruno, C. G. ^{[5
]}

Aliotta, M. ^{[5
]}

Best, A. ^{[6
,7
]}

Boeltzig, A. ^{[3
]}

Bemmerer, D. ^{[4
]}

Broggini, C. ^{[8
]}

Caciolli, A. ^{[8
,9
]}

Cavanna, F. ^{[10
,11
]}

Ciani, G. F. ^{[3
]}

Corvisiero, P. ^{[10
,11
]}

Cristallo, S. ^{[1
,21
]}

Davinson, T. ^{[5
]}

Depalo, R. ^{[8
,9
]}

Di Leva, A. ^{[6
,7
]}

Elekes, Z. ^{[12
]}

Ferraro, F. ^{[10
,11
]}

Formicola, A. ^{[2
]}

Fulop, Zs. ^{[12
]}

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

Guglielmetti, A. ^{[15
,16
]}

Gustavino, C. ^{[17
]}

Gyurky, G. ^{[12
]}

Imbriani, G. ^{[6
,7
]}

Junker, M. ^{[2
]}

Menegazzo, R. ^{[8
]}

Mossa, V. ^{[18
,19
]}

Pantaleo, F. R. ^{[18
,19
]}

Piatti, D. ^{[8
,9
]}

Piersanti, L. ^{[1
,21
]}

Prati, P. ^{[10
,11
]}

Samorjai, E. ^{[12
]}

Strieder, F. ^{[20
]}

Szucs, T. ^{[4
]}

Takacs, M. P. ^{[4
]}

Trezzi, D. ^{[13
,14
]}

机构：

[1] Osservatorio Astron Teramo, INAF, I-64100 Teramo, Italy

[2] INFN, LNGS, I-67100 Assergi, Italy

[3] INFN, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy

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

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

[6] Univ Naples Federico II, I-80126 Naples, Italy

[7] INFN, Sez Napoli, I-80126 Naples, Italy

[8] INFN, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy

[9] Univ Padua, Dept Phys & Astron, Via Marzolo 8, I-35131 Padua, Italy

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

[11] INFN, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy

[12] Inst Nucl Res MTA ATOMKI, POB 51, H-4001 Debrecen, Hungary

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

[14] INFN, Sez Torino, Via P Giuria 1, I-10125 Turin, Italy

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

[16] INFN, Sez Milano, Via G Celoria 16, I-20133 Milan, Italy

[17] INFN, Sez Roma La Sapienza, Piazzale A Moro 2, I-00185 Rome, Italy

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

[19] INFN, Sez Bari, I-70125 Bari, Italy

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

[21] INFN, Sez Perugia, I-06123 Perugia, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 598卷

关键词：

nuclear reactions; nucleosynthesis; abundances; stars: abundances; stars: evolution; ASYMPTOTIC GIANT BRANCH; OXYGEN ISOTOPIC-RATIOS; THERMONUCLEAR REACTION-RATES; SOLAR METALLICITY STARS; MASSIVE AGB STARS; RED GIANTS; S-PROCESS; EVOLVED STARS; CNO ISOTOPES; EVOLUTION;

D O I：

10.1051/0004-6361/201629624

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Material processed by the CNO cycle in stellar interiors is enriched in O-17. When mixing processes from the stellar surface reach these layers, as occurs when stars become red giants and undergo the first dredge up, the abundance of O-17 increases. Such an occurrence explains the drop of the O-16/O-17 observed in RGB stars with mass larger than similar to 1.5 M-circle dot. As a consequence, the interstellar medium is continuously polluted by the wind of evolved stars enriched in O-17. Aims. Recently, the Laboratory for Underground Nuclear Astrophysics (LUNA) collaboration released an improved rate of the O-17(p, alpha)N-14 reaction. In this paper we discuss the impact that the revised rate has on the O-16/O-17 ratio at the stellar surface and on O-17 stellar yields. Methods. We computed stellar models of initial mass between 1 and 20 M-circle dot and compared the results obtained by adopting the revised rate of the O-17(p, alpha)N-14 to those obtained using previous rates. Results. The post- first dredge up O-16/O-17 ratios are about 20% larger than previously obtained. Negligible variations are found in the case of the second and the third dredge up. In spite of the larger O-17(p, alpha)N-14 rate, we confirm previous claims that an extra-mixing process on the red giant branch, commonly invoked to explain the low carbon isotopic ratio observed in bright low-mass giant stars, marginally affects the O-16/O-17 ratio. Possible effects on AGB extra-mixing episodes are also discussed. As a whole, a substantial reduction of O-17 stellar yields is found. In particular, the net yield of stars with mass ranging between 2 and 20 M-circle dot is 15 to 40% smaller than previously estimated. Conclusions. The revision of the O-17(p, alpha)N-14 rate has a major impact on the interpretation of the O-16/O-17 observed in evolved giants, in stardust grains and on the O-17 stellar yields.

引用

页数：8

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