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

Research Motivation

The Model

Calculated Results

Conclusion & Prospect

Outline

I. Motivation

I. Motivation

HIRFLCSR

CIAE

Japan RIBF 2007

CSR 2008

Germany FAIR2012

France SPIRAL-II 2007

USA FRIB 2016 BRIF 2012

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).

Shell Model calculations

i : single particle energy

<j1, j2, J, T | V | j3, j4, J, T > : two-body interaction matrix element

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 codeOXBASH 、 ANTOINE 、 Mshell 、 NushellX ……

m scheme J scheme

II. The Model

II. The Model

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 shellH. Jin , M. Hasegawa ,S. Tazaki ,K.Kaneko and Y. Sun, Phys. Rev. C 78, 044324 (2011) Sn132 mass region

T. Otsuka et al . Phys. Rev. Lett. 95, 232502 (2005).

134Te

PRC,56(1):R16(1997)PRL,77(18):3743(1996)empirical nucleon-nucleon interactions CD-Bonn potential

II. The Model

Model space

N=82

0g7/2+

1d5/2+

2s1/2+

1d3/2+

1h11/2-

1f7/2-

2p3/2-

0h9/2-2p1/2-

1f5/2-

1d3/2+

1h11/2-

Z=50

N=66

NushellX

II. The Model

Single-particle energy correction for the model space

( ; : )aa m a b c d J

H C C G ab cd Ja

a ae

a b c dm m m m

j m j m JM j m j m JMa b g d

a b g d 1 1

1 1C C C C

ab cd a b d gd d

( ; : )G ab cd J :two-body interaction matrix elements

'ae :single particle energy or hole energy if Sn132 is the core.

' 1(2 1) ( ; : )

2 1a aJ b holea

J G ba ba Jj

e e

Ca

( ) aj m

a

baa

a

for particles

for holes

( , )aj maa

( , )aj maa

ae :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

ParametersThe monopole correction term

Single particle energies for the model

' 1(2 1) ( ; : )

2 1a aJ b holea

J G ba ba Jj

e e

II. The Model

Truncation

proton

neutron

Truncation for the model space

II. The Model

A=133 nuclei

III. Calculated Results

17T s isomer

17 2 7 2 11 2g f h

17 2 7 2 3 2g f d

2 17 2 11 2f h

A=134 nuclei

III. Calculated Results

2 17 2 7 2 11 2g f h

2 17 2 7 2 3 2g f d

17 2 5 2 7 2 3 2g d f d

III. Calculated Results

2 17 2 7 2 11 2g f h

7 2 7 2g f

A=134 nuclei

A=135 nuclei

III. Calculated Results

2 2 17 2 7 2 11 2g f h

dipole band

Possible magnetic rotation

A=135 nuclei

III. Calculated Results

2 17 2 7 2 11 2g f h 3 1

7 2 7 2 3 2g f d

Electromagnetic Transition

III. Calculated Results

IV. Conclusion & Prospect

Research for the next step:

other neutron-rich nuclei (N=83, 84…… isotones)

shell evolution

decayb

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.

electromagnetic transition

core excitation states

octupole and hexadecupole correlation

possible magnetic rotation band of 135Te

Thanks for your attention!!