Tutor: Prof. Yang Sun (孙扬 教授) Large-scale shell model calculation with core excitations for neutron-rich nuclei beyond 132Sn Hua Jin (金华) Tutor: Prof. Yang Sun (孙扬 教授) 2012.4 湖州

Outline Research Motivation The Model Calculated Results Conclusion & Prospect

I. Motivation

I. Motivation USA FRIB 2016 BRIF 2012 CSR 2008 Japan RIBF 2007 HIRFL CSR CIAE USA FRIB 2016 BRIF 2012 CSR 2008 Japan RIBF 2007 France SPIRAL-II 2007 Germany FAIR 2012 4

I. Motivation 132Sn Magic nature: Nature 465, 454(2010). Core excitation: Phys. Rev.C 65, 017302 (2001);Phys. Rev. C 63, 024322 (2001); Phys.Rev. C 79, 037304 (2009). Nucleo-synthesis(r-p): Rep. Prog. Phys. 70, 1525 (2007). Isomer state: Phys.Rev. C 79, 037304 (2009); Phys. Lett. B 688, 294 (2010). Shell evolution: Phys. Rev. C 81, 064328 (2010). Magnetic rotation: Phys. Rev. C 64, 054306 (2001).

II. The Model Shell Model calculations ei : single particle energy : two-body interaction matrix element <j1, j2, J, T | V | j3, j4, J, T > GXPF1 interaction for pf shell Based on realistic nucleon-nucleon interactions: CD-Bonn Fit to experimental energy data of many nuclei USD interaction for sd shell PQQM …… Shell Model code OXBASH、 ANTOINE、 Mshell、 NushellX …… m scheme J scheme

II. The Model The Extend PQQM Model T. Otsuka et al . Phys. Rev. Lett. 95, 232502 (2005). The Extend PQQM Model M.Hasegawa, Kaneko, S.Tazaki, Nucl. Phys. A 674, 411 (2000) pf shell K.Kaneko, Y.Sun et. al., Phys. Rev. C 78, 064312 (2008) pf-g shell M. Hasegawa, Y. Sun et. al., Phys. Lett. B 696, 197 (2011) 93,94Mo K.Kaneko, Y.Sun et. al. , Phys. Rev. C 83, 014320 (2011) neutron-rich sd shell H. Jin , M. Hasegawa ,S. Tazaki ,K.Kaneko and Y. Sun, Phys. Rev. C 78, 044324 (2011) Sn132 mass region

II. The Model 134Te PRL,77(18):3743(1996) PRC,56(1):R16(1997) empirical nucleon-nucleon interactions CD-Bonn potential

II. The Model Model space NushellX 1f5/2- 2p1/2- 0h9/2- 2p3/2- 1f7/2- 0g7/2+ 1d5/2+ 2s1/2+ 1d3/2+ 1h11/2- 1d3/2+ 1h11/2- N=66 NushellX Z=50

II. The Model Single-particle energy correction for the model space :two-body interaction matrix elements for particles for holes :single particle energy or hole energy if Sn132 is the core. :single particle energy for the present model space

II. The Model Parameters The energies of single particle or hole if Sn132 as the core Interaction strengths

II. The Model Parameters The monopole correction term Single particle energies for the model

II. The Model Truncation proton neutron Truncation for the model space

III. Calculated Results A=133 nuclei isomer

III. Calculated Results A=134 nuclei

III. Calculated Results A=134 nuclei

III. Calculated Results A=135 nuclei dipole band Possible magnetic rotation

III. Calculated Results A=135 nuclei

III. Calculated Results Electromagnetic Transition

IV. Conclusion & Prospect We use the EPPQM to find a good interaction and reproduce the experiments of the exotic nuclei beyond 132Sn near the neutron drip line well by large scale shell model calculation. electromagnetic transition core excitation states octupole and hexadecupole correlation possible magnetic rotation band of 135Te Research for the next step: other neutron-rich nuclei (N=83, 84…… isotones) shell evolution decay

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