hiroshi masui kitami institute of technology collaborators:k. katohokkaido univ. k. ikedariken 22-26...
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Hiroshi MASUI
Kitami Institute of Technology
Collaborators: K. Kato Hokkaido Univ.K. Ikeda RIKEN
22-26 Aug. 2011, APFB2011, Sungkyunkwan Univ., Seoul, Korea
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Matter radius of nuclei near the drip-linesAn “abrupt” change of the radius due to the
weakly bound neutron or proton
A. Ozawa 2001
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Difference from typical halo nuclei: 6He, 11Be, 11Li
Core + XnCore+n (+2n)
Large Sn values of 23O and 24O ( 2.7MeV and 3.7MeV )
6He : 0.98MeV11Li : 0.38MeV11Be: 0.50MeV
23O : 2.7MeV24O : 3.7MeV
Weakly-bound neutrons Strongly-bound neutrons
22O
Sn Sn
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To reproduce the drip-line at 24O
ab initio calc. + Realistic force
Effect of the thee-body interactionT. Otsuka et al, Phys. Rev. Lett. 105, 032501 (2010)
G. Hagen et al., Phys. Rev. C 80, 021306(R) (2009)
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Ab initio calc. + Realistic force G. Hagen et al., Phys. Rev. C 80, 021306(R) (2009)
Coupled-cluster (2-body) + N3LO int.
-dependence: lack of many-body int.
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Effect of the three-body interactionT. Otsuka et al, Phys. Rev. Lett. 105, 032501 (2010)
3-body int.
Pauli-forbidden state
Getting weakerfor more valence particle system
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T. Otsuka et al, Phys. Rev. Lett. 105, 032501 (2010)
Getting weakeras the number of valence particles increases
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How about the radius?
h ~ 27 MeV
b ~ 1.24 (fm)
Very small radius
G. Hagen et al., Phys. Rev. C 80, 021306(R) (2009)
Coupled-cluster (2-body) + N3LO int.
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Our approaches
Role of many valence neutrons16O+Xn model m-scheme COSM + Gaussian basis
Role of last one- or two-neutrons “Core” + n or “Core”+2n modelA simplified model approach
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M-Scheme COSM + Gaussian base H. Masui, K. Kato and K. Ikeda, Euro. Phys. Jour. A42 (2009) 535
•Core (16O) +Xn model space
•Gaussian radial function
•Stochastic approach for the basis set
•M-scheme approach
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M-Scheme COSM approach
Wave function for the valence nucleons:
•Radial part
Product of Gaussian
•Spin-isospin part
Total M and MT are fixed
Coordinate system
We check the expectation value of the total J as <J2>
H. Masui, K. Kato and K. Ikeda, Euro. Phys. Jour. A42 (2009) 535
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Expectation value of J2
J=0J=1/2
J=5/2
J=3/2
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B=H=0.25
B=H=0.07
B=H=0.07
Sn for O-isotopes
NN-int.: Volkov No.2 (M=0.58)
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Change the coresize with A1/6
B=H=0.07
B=H=0.25
b: 1.723 (fm)
b~A1/6
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Comparison with other approaches
[3] G. Hagen et al., PRC 80 (2009)[2] B. Ab-Ibrahim et al., JPSJ 78 (2009)[1] H. Nakada, NPA764 (2006)
□: [2]
■: [1]
△: [3]+0.5(fm)
▲: [3]
○: fixed-b
●: m-COSM with b 〜 A1/6
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Result of M-scheme COSM (16O+Xn model space)
•From 18O to 22O
•For23O and24O
16O-core with a fixed size + valence neutrons
16O-core with A1/6 (Mean-field-like) +valence neutrons
How large?(is the amount of the change of the radius)
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Core+2n modelWe adjust the core radius and energy of the core+nsystem⇒ calculate the core+2n system
Core
Core+n
Core+2n
Fit
Rrms
E
E
(Core-n int.)
(n-n int)
Rrms
Rrms
Calc.
16O
17O (16O+n)
18O (16O+2n)
18O
19O (18O+n)
20O (18O+2n)
20O
21O (20O+n)
22O (20O+2n)
22O
23O (22O+n)
24O (22O+2n)
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Results for the core+2n model
We define the difference between the calculated and experimental radii as
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20O 21O
22O
Difference of the radius between Calc. and Exp.16O-17O-18O, 18O-19O-20O, 20O-21O-22O
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22O 23O 24O
Difference of the radius between Calc. and Exp.22O-23O-24O
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22O 23O 24O
0.238 (fm)
A schematic figure to illustrate the change of the radius of 22O
Rrms[1] 2.88±0.06 3.20±0.04 3.19±0.13
[1] A. Ozawa et al, NPA693 (2001)
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Expansion of the core
Matter radius
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SummaryWe studied the energy and radius of oxygen isotopeswith M-Scheme COSM and Core+2n model
1. Mean-field-like configuration with b~A1/6
2. Shrunk core size configuration until 22O
H.O. : 0p-0h configuration
Shrunk b⇒ High mom. ⇒ TOSM
It is suggested that a coupled-channel model is necessary to be introduced
The size of 22O is drastically changed when a neutron is added (23O)
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Inclusion of the core excitation
TOSM in 9Li T. Myo, K. Kato, H. Toki and K. Ikeda, PRC76(2007)
2. Some config. are suppressed due to the Pauli-blocking
1. Different size for each orbit