Neutron physics of the Re/Os clock. III. Resonance analyses and stellar (n, γ) cross sections of 186,187,188Os

被引：29

作者：

Fujii, K. ^{[1
]}

Mosconi, M. ^{[2
]}

Mengoni, A. ^{[3
,18
]}

Domingo-Pardo, C. ^{[4
]}

Kaeppeler, F. ^{[2
]}

Abbondanno, U. ^{[1
]}

Aerts, G. ^{[5
]}

Alvarez-Pol, H. ^{[6
]}

Alvarez-Velarde, F. ^{[7
]}

Andriamonje, S. ^{[5
]}

Andrzejewski, J. ^{[8
]}

Assimakopoulos, P. ^{[9
]}

Audouin, L. ^{[2
]}

Badurek, G. ^{[10
]}

Baumann, P. ^{[11
]}

Becvar, F. ^{[12
]}

Belloni, F. ^{[1
]}

Berthoumieux, E. ^{[5
]}

Bisterzo, S. ^{[2
,13
]}

Calviani, M. ^{[14
]}

Calvino, F. ^{[15
]}

Cano-Ott, D.

Capote, R. ^{[3
]}

de Albornoz, A. Carrillo ^{[17
]}

Cennini, P. ^{[18
]}

Chepel, V. ^{[19
,20
]}

Chiaveri, E. ^{[18
]}

Colonna, N. ^{[21
]}

Cortes, G. ^{[15
]}

Couture, A. ^{[22
]}

Cox, J. ^{[22
]}

Dahlfors, M. ^{[18
]}

David, S. ^{[23
]}

Dillmann, I.

Dolfini, R. ^{[24
]}

Dridi, W. ^{[5
]}

Duran, I. ^{[6
]}

Eleftheriadis, C. ^{[25
]}

Embid-Segura, M. ^{[7
]}

Ferrant, L. ^{[23
]}

Ferrari, A. ^{[18
]}

Ferreira-Marques, R. ^{[19
,20
]}

Fitzpatrick, L. ^{[18
]}

Frais-Koelbl, H. ^{[3
]}

Furman, W. ^{[26
]}

Gallino, R. ^{[13
]}

Goncalves, I. ^{[19
,20
]}

Gonzalez-Romero, E. ^{[7
]}

Goverdovski, A. ^{[27
]}

Gramegna, F. ^{[14
]}

机构：

[1] Ist Nazl Fis Nucl, I-34149 Trieste, Italy

[2] KIT, Inst Kernphys, D-76021 Karlsruhe, Germany

[3] IAEA, NAPC Nucl Data Sect, A-1400 Vienna, Austria

[4] Univ Valencia, CSIC, Inst Fis Corpuscular, E-46980 Paterna, Spain

[5] CEA Saclay, DSM, F-91191 Gif Sur Yvette, France

[6] Univ Santiago de Compostela, Santiago De Compostela 15782, Spain

[7] Ctr Invest Energet Medioambient & Technol, E-28040 Madrid, Spain

[8] Univ Lodz, PL-90142 Lodz, Poland

[9] Univ Ioannina, GR-45110 Ioannina, Greece

[10] Vienna Univ Technol, Atominst Osterreich Univ, A-1020 Vienna, Austria

[11] CNRS IN2P3, IReS, F-67037 Strasbourg, France

[12] Charles Univ Prague, CZ-25241 Prague, Czech Republic

[13] Univ Turin, Dipartimento Fis Gen, I-10149 Turin, Italy

[14] Ist Nazl Fis Nucl, Lab Nazl Legnaro, I-35020 Padua, Italy

[15] Univ Politecn Cataluna, E-08034 Barcelona, Spain

[16] Univ Seville, E-41004 Seville, Spain

[17] ITN, P-2686953 Lisbon, Portugal

[18] CERN, CH-1211 Geneva, Switzerland

[19] Univ Coimbra, LIP, P-3004531 Coimbra, Portugal

[20] Univ Coimbra, Dept Fis, P-3004531 Coimbra, Portugal

[21] Ist Nazl Fis Nucl, I-70126 Bari, Italy

[22] Univ Notre Dame, Notre Dame, IN 46556 USA

[23] CNRS IN2P3, IPN, F-91406 Orsay, France

[24] Univ Pavia, I-27100 Pavia, Italy

[25] Aristotle Univ Thessaloniki, GR-54124 Thessaloniki, Greece

[26] Joint Inst Nucl Res, Frank Lab Neutron Phys, RUS-141980 Dubna, Russia

[27] Inst Phys & Power Engn, RUS-249020 Obninsk, Russia

[28] CENBG, CNRS IN2P3, F-33175 Gradignan, France

[29] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[30] Tokyo Inst Technol, Tokyo 1528550, Japan

[31] Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA

[32] NCSR Demokritos, GR-15310 Athens, Greece

[33] Univ Bologna, Dipartmento Fis, I-40126 Bologna, Italy

[34] Sez INFN Bologna, I-40126 Bologna, Italy

[35] Japan Atom Energy Res Inst, Tokai, Ibaraki 3191184, Japan

[36] Natl Tech Univ Athens, GR-10682 Athens, Greece

[37] Univ Vienna, Fac Phys, A-1010 Vienna, Austria

[38] CEC JRC IRMM, B-2440 Geel, Belgium

[39] Univ Basel, Dept Phys & Astron, CH-4003 Basel, Switzerland

[40] ENEA, I-40129 Bologna, Italy

来源：

PHYSICAL REVIEW C | 2010年 / 82卷 / 01期

关键词：

GIANT BRANCH STARS; METAL-POOR; RE-187-OS-187; SYSTEMATICS; CHEMICAL EVOLUTION; CAPTURE; AGE; METEORITES; CHRONOLOGY; FORMULA;

D O I：

10.1103/PhysRevC.82.015804

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：

Neutron resonance analyses have been performed for the capture cross sections of Os-186, Os-187, and Os-188 measured at the n_TOF facility at CERN. Resonance parameters have been extracted up to 5, 3, and 8 keV, respectively, using the SAMMY code for a full R-matrix fit of the capture yields. From these results average resonance parameters were derived by a statistical analysis to provide a comprehensive experimental basis for modeling of the stellar neutron capture rates of these isotopes in terms of the Hauser-Feshbach statistical model. Consistent calculations for the capture and inelastic reaction channels are crucial for the evaluation of stellar enhancement factors to correct the Maxwellian averaged cross sections obtained from experimental data for the effect of thermally populated excited states. These factors have been calculated for the full temperature range of current scenarios of s-process nucleosynthesis using the combined information of the experimental data in the region of resolved resonances and in the continuum. The consequences of this analysis for the s-process component of the Os-187 abundance and the related impact on the evaluation of the time duration of galactic nucleosynthesis via the Re/Os cosmochronometer are discussed.

引用

页数：18

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