Large-scale shell model calculation with core excitations for neutron-rich nuclei beyond 132 Sn

1. 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

2. Outline • Research Motivation • The Model • Calculated Results • Conclusion & Prospect

3. I. Motivation

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

5. 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).

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

7. II. The 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

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

9. 1f5/2- 2p1/2- 0h9/2- II. The Model 2p3/2- 1f7/2- N=82 1h11/2- 1d3/2+ 1d3/2+ 1h11/2- 2s1/2+ 1d5/2+ 0g7/2+ Model space N=66 NushellX Z=50

10. II. The Model :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 Single-particle energy correction for the model space

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

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

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

14. III. Calculated Results isomer A=133 nuclei

15. III. Calculated Results A=134 nuclei

16. III. Calculated Results A=134 nuclei

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

18. III. Calculated Results A=135 nuclei

19. III. Calculated Results Electromagnetic Transition

20. IV. Conclusion & Prospect Conclusion: 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. • core excitation states • octupole and hexadecupole correlation • electromagnetic transition • possiblemagnetic rotation band of 135Te Research for the next step: • other neutron-rich nuclei (N=83, 84…… isotones) • decay • shell evolution

21. Thanks for your attention!!