Astrophysical S-factor of 14N(p, γ)15O

被引：308

作者：

Formicola, A ^{[1
]}

Imbriani, G

Costantini, H

Angulo, C

Bemmerer, D

Bonetti, R

Broggini, C

Corvisiero, P

Cruz, J

Descouvemont, P

Fülöp, Z

Gervino, G

Guglielmetti, A

Gustavino, C

Gyürky, G

Jesus, AP

Junker, M

Lemut, A

Menegazzo, R

Prati, P

Roca, V

Rolfs, C

Romano, M

Alvarez, CR

Schümann, F

Somorjai, E

Straniero, O

Strieder, F

Terrasi, F

Trautvetter, HP

Vomiero, A

Zavatarelli, S

机构：

[1] Ruhr Univ Bochum, Inst Expt Phys 3, D-4630 Bochum, Germany

[2] Ist Nazl Fis Nucl, Legnaro, Italy

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

[4] Ist Nazl Fis Nucl, I-80125 Naples, Italy

[5] Univ Naples 2, Caserta, Dipartimento Sci Ambientali, Caserta, Italy

[6] Univ Naples, Dipartimento Fis, Naples, Italy

[7] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, Assergi, Italy

[8] Ist Nazl Fis Nucl, I-10125 Turin, Italy

[9] Univ Turin, Dipartimento Fis Sperimentale, Turin, Italy

[10] ATOMKI, Debrecen, Hungary

[11] Free Univ Brussels, Brussels, Belgium

[12] Univ Lisbon, Ctr Fis Nucl, P-1699 Lisbon, Portugal

[13] Ist Nazl Fis Nucl, Padua, Italy

[14] Ist Nazl Fis Nucl, I-20133 Milan, Italy

[15] Univ Milan, Ist Fis, Milan, Italy

[16] Tech Univ Berlin, Ist Atomare Phys & Fachdidaktik, Berlin, Germany

[17] Univ Catholique Louvain, Ctr Rech Cyclotron, B-1348 Louvain, Belgium

[18] Ist Nazl Fis Nucl, I-16146 Genoa, Italy

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

[20] Osservatorio Astron Collurania, Teramo, Italy

来源：

PHYSICS LETTERS B | 2004年 / 591卷 / 1-2期

基金：

匈牙利科学研究基金会;

关键词：

D O I：

10.1016/j.physletb.2004.03.092

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on a new measurement of the N-14(p, gamma) O-15 capture cross section at E-p = 140 to 400 keV using the 400 kV LUNA accelerator facility at the Laboratori Nazionali del Gran Sasso (LNGS). The uncertainties have been reduced with respect to previous measurements and their analysis. We have analyzed the data using the R-matrix method and we find that the ground state transition accounts for about 15% of the total S-factor. The main contribution to the S-factor is given by the transition to the 6.79 MeV state. We find a total S(0) = 1.7 +/- 0.2 keV b, in agreement with recent extrapolations. The result has important consequences for the solar neutrino spectrum as well as for the age of globular clusters. (C) 2004 Elsevier B.V. All rights reserved.

引用

页码：61 / 68

页数：8

共 22 条

[1] ENERGY-LEVELS OF LIGHT-NUCLEI A=13-15 [J].

AJZENBERGSELOVE, F .

NUCLEAR PHYSICS A, 1991, 523 (01) :1-196

[2] The 14N(p,γ)15O low-energy S-factor [J].

Angulo, C ;

Descouvemont, P .

NUCLEAR PHYSICS A, 2001, 690 (04) :755-768

[3] The AME2003 atomic mass evaluation (II). Tables, graphs and references [J].

Audi, G ;

Wapstra, AH ;

Thibault, C .

NUCLEAR PHYSICS A, 2003, 729 (01) :337-676

[4] STANDARD SOLAR MODELS, WITH AND WITHOUT HELIUM DIFFUSION, AND THE SOLAR NEUTRINO PROBLEM [J].

BAHCALL, JN ;

PINSONNEAULT, MH .

REVIEWS OF MODERN PHYSICS, 1992, 64 (04) :885-926

[5]

BAHCALL JN, IN PRESS PHYS REV LE

[6] OXYGEN-ENHANCED MODELS FOR GLOBULAR-CLUSTER STARS .2. ISOCHRONES AND LUMINOSITY FUNCTIONS [J].

BERGBUSCH, PA ;

VANDENBERG, DA .

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 1992, 81 (01) :163-220

[7] 14N(3He,d)15O as a probe of direct capture in the 14N(p,γ)15O reaction -: art. no. 055804 [J].

Bertone, PF ;

Champagne, AE ;

Boswell, M ;

Iliadis, C ;

Hale, SE ;

Hansper, VY ;

Powell, DC .

PHYSICAL REVIEW C, 2002, 66 (05)

[8]

BERTONE PF, 2001, PHYS REV LETT, V87

[9]

COSTANTINI H, 2003, THESIS U GENOVA

[10]

DEGINNOCENTI S, ASTROPH0312559

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