Approaching the precursor nuclei of the third r-process peak with RIBs

6th Nuclear Physics in Astrophysics

物理学;天文学

Domingo-Pardo, C.^1 ; Caballero-Folch, R.^2 ; Agramunt, J.^1 ; Algora, A.^1,3 ; Arcones, A.^4 ; Ameil, F.^4 ; Ayyad, Y.^5 ; Benlliure, J.^5 ; Bowry, M.^6 ; Calviño, F.^3 ; Cano-Ott, D.^7 ; Cortés, G.^2 ; Davinson, T.^8 ; Dillmann, I.^4,9 ; Estrade, A.^4,10 ; Evdokimov, A.^4,9 ; Faestermann, T.^11 ; Farinon, F.^4 ; Galaviz, D.^12 ; García-Rios, A.^7 ; Geissel, H.^4,9 ; Gelletly, W.^6 ; Gernhäuser, R.^11 ; Gómez-Hornillos, M.B.^3 ; Guerrero, C.^13 ; Heil, M.^4 ; Hinke, C.^11 ; Knöbel, R.^4 ; Kojouharov, I.^4 ; Kurcewicz, J.^4 ; Kurz, N.^4 ; Litvinov, Y.^4 ; Maier, L.^11 ; Marganiec, J.^14 ; Marta, M.^4,9 ; Martínez, T.^7 ; Martínez-Pinedo, G.^4 ; Meyer, B.S.^21 ; Montes, F.^15,16 ; Mukha, I.^4 ; Napoli, D.R.^17 ; Nociforo, Ch.^4 ; Paradela, C.^5 ; Pietri, S.^4 ; Podolyák, Z.^6 ; Prochazka, A.^4 ; Rice, S.^6 ; Riego, A.^2 ; Rubio, B.^1 ; Schaffner, H.^4 ; Scheidenberger, Ch.^4,9 ; Smith, K.^18,19 ; Sokol, E.^20 ; Steiger, K.^11 ; Sun, B.^4 ; Taín, J.L.^1 ; Takechi, M.^4 ; Testov, D.^20,22 ; Weick, H.^4 ; Wilson, E.^6 ; Winfield, J.S.^4 ; Wood, R.^6 ; Woods, P.^8 ; Yeremin, A.^20

IFIC, CSIC, University of Valencia, Valencia, Spain^1

INTE-DFEN, UPC, Barcelona, Spain^2

Institute of Nuclear Research, Hungarian Academy of Sciences, Debrecen, Hungary^3

GSI Helmholtzzentrum für Schweionenforschung GmbH, Darmstadt, Germany^4

Universidade de Santiago de Compostela, Santiago de Compostela, Spain^5

Deptartment of Physics, University of Surrey, Guildford, United Kingdom^6

Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Madrid, Spain^7

School of Physics and Astronomy, University of Edinburgh, United Kingdom^8

Physikalisches Institut, Justus-Liebig Universität Giessen, Germany

(10) St. Mary's University, Halifax

NS, Canada

(11) Physics Department E12, Technische Universität Munchen, Garching, Germany

(12) Centro de Fisica Nuclear, Universidade de Lisboa, Lisboa, Portugal

(13) CERN, Geneva, Switzerland

(14) ExtreMe Mater Institute, Darmstadt, Germany

(15) National Superconducting Cyclotron Laboratory, Michigan State University, EastLansing, United States

(16) Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, United States

(17) Instituto Nazionale di Fisica Nucleare, Laboratori Nazionale di Legnaro, Italy

(18) Department of Physics, University of Notre Dame, South Bend, United States

(19) Joint Institute for Nuclear Astrophysics, University of Notre Dame, South Bend, United States

(20) Flerov Laboratory, Joint Institute for Nuclear Research, Dubna, Russia

(21) Clemson University, United States

(22) Institut de Physique Nucleaire d'Orsay, France^9

关键词: Abundance distribution;    Branching ratio;    Decay properties;    Delayed neutron emission;    Half lives;    Mass regions;    Neutron-rich nuclei;    Nuclear structure;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/665/1/012045/pdf
DOI  :  10.1088/1742-6596/665/1/012045

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

The rapid neutron nucleosynthesis process involves an enormous amount of very exotic neutron-rich nuclei, which represent a theoretical and experimental challenge. Two of the main decay properties that affect the final abundance distribution the most are half-lives and neutron branching ratios. Using fragmentation of a primary238U beam at GSI we were able to measure such properties for several neutron-rich nuclei from208Hg to218Pb. This contribution provides a short update on the status of the data analysis of this experiment, together with a compilation of the latest results published in this mass region, both experimental and theoretical. The impact of the uncertainties connected with the beta-decay rates and with beta-delayed neutron emission is illustrated on the basis of r-process network calculations. In order to obtain a reasonable reproduction of the third r-process peak, it is expected that both half-lives and neutron branching ratios are substantially smaller, than those based on FRDM+QRPA, commonly used in r-process model calculations. Further measurements around N ∼ 126 are required for a reliable modelling of the underlying nuclear structure, and for performing more realistic r-process abundance calculations.