1. 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) 湖州

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

3. I. Motivation

4. 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

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

6. 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

7. II. The Model The Extend PQQM Model
T. Otsuka et al .
Phys. Rev. Lett. 95, (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, (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, (2011) neutron-rich sd shell
H. Jin , M. Hasegawa ,S. Tazaki ,K.Kaneko and Y. Sun, Phys. Rev. C 78, (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. 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

10. 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

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
Truncation
proton
neutron
Truncation for the model space

14. III. Calculated Results
A=133 nuclei
isomer

15. III. Calculated Results
A=134 nuclei

16. III. Calculated Results
A=134 nuclei

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

18. III. Calculated Results
A=135 nuclei

19. III. Calculated Results
Electromagnetic Transition

20. 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

21. Thanks for your attention!!