Post on 15-Jan-2016
Heavy-Ion Meeting 1
Plan for Korea Rare Iso-tope Accelerator (Ko-
RIA*)
Byungsik Hong (Korea University)
October 31, 2009
Outline- Introduction - Physics topics - Experimental observables- Summary
* Tentative
Heavy-Ion Meeting 2
2
20
126
28
20
28
82
Super Heavy Element
r process
How gold is produced?
Nuclear Structure of Double Magic Nuclei
Nuclear Synthesis in Red GiantNuclear radius of Halo nu-clei
Nuclear mass of heavy nu-clei
Fundamental Symmetry in Universe
82
Next generation Gamma CameraIR Camera
Spintronics
Mystery of High Tc Superconductor
Gateway to rp process
Lithium Film Battery
rp process
8
Gen-IV nuclear reactor
28
Cancer Therapy50
DNA research
50
October 31, 2009
Research Topics with RIB
Heavy-Ion Meeting 3
Nuclear Chart for Nuclear Physics
October 31, 2009
N
Z
Terra incógnita
Neutron halo and skin Reorganization of the nuclear shell structureDeformation at drip lines
Superheavy nuclei
r-process (Novae & Supernovae)
Drip lines are determined by interplay among
- n-p symmetry- Coulomb force- Shell structure- NN correlation
Stable Nuclei ≈ 300Unstable nuclei observed so far ≈
2700Drip-lines (limit of existence)
by theoretical predictions ≈ 6000
rp-process
s-process(Red giants)
28
28
82
20
82
50
20
50
82
Landscape of Neutron Drip Line? Where is the neutron drip line?
Shell property at drip line?
Collectivity, deformation at drip line?
Halo nuclei– abundant? universal?How halo is formed towards heavier region?
2n-halo(3body):6He,11Li,14Be,17,19B1n-halo(2body):11Be,19C
Halo found in p-shell, sd-shell
?
Giant Halo?128Zr: 6n halo?J. Meng and P. Ring, PRL80, 460 (1998)9Li
11Li
nn
122Zr
128Zr
From T. Nakamura
HHe
LiBeBC
NO
FNe
NaMgAlSi
PS
ClAr
K
N=8
N=16
N=20
N=28
N=2
32Mg
More neutron halo’s along the drip line?
* Estimated value by Audi & Wapstra
2n halo known4n halo (skin)
1n-halo known
22C [S2n*=0.42(94) MeV]
31Ne [Sn=0.29(1.64) MeV]Jurado et al. PLB649,43(2007)
Island of inversion
19C
Halo?
From T. Nakamura
Heavy-Ion Meeting 6
RIPS @ RIKEN
October 31, 2009
RIB
9Li
nn
Target
NEUT
HOD
BOMAG
DC
DALI56 NaI(Tl)
11LiFrom T. Nakamura
2n breakup of halo nuclei, e.g. 11Li
Heavy-Ion Meeting 7
Nuclear Astrophysics
October 31, 2009
7Be(p,g)8BFrom T. Moto-bayashi
We can measure 8B Coulomb dissocia-tion with RIB
8B
7Be
p
208Pb
Virtual photons
Heavy-Ion Meeting 8October 31, 2009
25Al
24Mg
23Na
22Ne21Ne20Ne
22Na
23Mg
24Al
21Na
22Mg
19F
18O
21Mg
20Na
19Ne
18F
17O
18Ne
17F
16O
15N
15O14O
13N
12C 13C
14N
(, )
ag
( , a p)
HCNO cycle
CNO cycle
(, )
ag
rp process
Stable
Unstable
CNO cycle : T9 < 0.2 HCNO cycle: 0.2 < T9 < 0.5rp process : T9 > 0.5
Nova Models
Nova Cygni
Nova Persei
O,),N( Si),Al(
F),O( Ne),O(
Ne),F( He) ,(
14142726
17141814
18173
npp
p
ppd
Heavy-Ion Meeting 9October 31, 2009
Heavy-Ion Meeting 10
Superheavy Nuclei: Current Status
October 31, 2009
116
115
114
113
112
Rg
Ds
Mt
Hs
Bh
Sg
Db
Rf
Lr
No
162
152
a
SFb+ or EC
170
176
118 294
293292291290
288287
286287288289
284283278
285284283282
277
277
280279272
281279273271270269
276275268266
264265266267 269
172
117
Heavy-Ion Meeting 11
Reactions Tried at GSI in 2007-2008
October 31, 2009
112
116
115
114
113
176
118 294
293292291290
288287
286287288289
284283278
285284283282
277
277
119
120
121
122
238U(64Ni,2-4n)300-298120
64Ni+238U 302120*
302120*
Heavy-Ion Meeting 12
Reactions Could be Stud-ied
October 31, 2009
112
116
115
114
113
176
118 294
293292291290
288287
286287288289
284283278
285284283282
277
277
119
120
121
122
238U(64Ni,4n)298120
182
238U(67Zn,3n)302122238U(68Zn,3n)303122238U(70Zn,3n)305122
From Y.H. Chung, Hallym Univ.
Heavy-Ion Meeting 13
Required Detector Sys-tem
October 31, 2009
1. Gas-filled recoil separator2. Focal plane detectors3. Rotating wheel system 4. Automated rapid chemistry apparatus –
MG wheel5. On-line gas chromatographic apparatus 6. Something like SISAK in Oslo
Heavy-Ion Meeting 14
Spin Structure of Unstable Nuclei
1. Spin-dependent interactions Origin of fundamental properties of nuclei Modification in neutron rich nuclei
2. Spin-orbit couplings and potentials Localized at the nuclear surface
Will be modified in neutron rich nuclei Should be composed of two parts localized at different posi-
tions if p and n have different r (r) Would have extended shape if n has an extended distribu-
tion in skin or halo nuclei
3. Need polarized p, d, and 3He targetsOctober 31, 2009
dr
rd
rVLS
)(1~
From W.Y. Kim, Kyungbook Nat. Univ.
Heavy-Ion Meeting 15
Present Status at RIKEN
October 31, 2009
S.Sakaguchi Ph.D. Thesis, University of Tokyo (2008)
4He
6He
valence n
4He
8He
1. Di-neutron structure→ Large recoil motion of a-core→ Large charge radius (2.068 fm)
2. Two valence neutrons→ Small matter radius (2.45 fm)
1. Isotropically distributed neutrons→ Small recoil motion of a-core→ Small charge radius (1.929 fm)
2. Four valence neutrons→ Large matter radius (2.53 fm)
Heavy-Ion Meeting 16
Present Status at RIKEN
October 31, 2009
He6p
He8p
t-matrix folding calculation
Non-local g-matrix folding calculation
S.Sakaguchi (2008)
Heavy-Ion Meeting 17October 31, 2009
18
B.-A. Li, L.-W. Chen & C.M. Ko Physics Report, 464, 113 (2008)
Nuclear Equation of State
AZNρρρδρρρ
ρEρEδ
EρE
δOδρEρρEρρE
pnpn
sym
sympnpn
/)(/)( ,with
)()(2
1)(
)()()(),(
matternuclear symmetric
matterneutron pure2
2
42
ρ0Nucleondensity
Isospin
asymmetry
Symmetricnuclear matter
(ρn=ρp)
δ
)(/ pn ρρAE
2)( δρEsym
E/A
(M
eV)
r (fm-3)
CD
R, FA
IR (2
001)
F. de Jong & H. Lenske, RPC 57, 3099 (1998)F. Hofman, C.M. Keil & H. Lenske, PRC 64, 034314 (2001)
Heavy-Ion Meeting 18
Nuclear Equation of State
October 31, 2009
Bao-An Li, PRL 88, 192701 (2002)
High (Low) density mat-ter is more neutron rich with soft (stiff) symmetry energy
Heavy-Ion Meeting 19
Importance of Symmetry Energy
October 31, 2009A.W. Steiner, M. Prakash, J.M. Lattimer and P.J. Ellis, Physics Report 411, 325 (2005)
RIB can provide crucial input. Effective field theory, QCD
isodiffusion isotransport+ isocorrelation isofractionation isoscaling
p-/p+ K+/K0
n/p +3H/3He g
Red boxes: added by B.-A. Li
Heavy-Ion Meeting 20
Uncertainty in Esym at high r
October 31, 2009
F
F
k
symF
Fk
Fpotsym
potsym
kinsymsym dkkkU
kk
k
kUktEEEE
3/12
0
23
021 )(2
3)(
6
1)(
3
1
Kinetic Isoscalar Isovector potential particleIsoscalar :3
4
1
2
1010 TTpn uuUUU
!high at termabout this little very know We
mediumin SI dep.Isospin :potentialIsovector
4
1
2
101 ρ
uuUUδ
U TTpnsym
Heavy-Ion Meeting 21
Possible Effects on Esym
October 31, 2009
G.E. Brown and M. Rho, PRL 66, 2720 (1991); Phys. Rep. 396, 1 (2004)
0
1ρ
ρα
m
mBR
ρ
ρ
Brown-Rho Scaling
3-Body Force
100
2
8)21(
)(
α
potsym
ρt
x
ρFE
Heavy-Ion Meeting 22
Is NS Stable with a Super Soft Esym?
October 31, 2009
If the symmetry energy is too soft, then a mechanical instability will occur when dP/dρ<0, neutron stars will, then, collapse while they exist in nature.
oncondensatikaon
for critical is )(ρμe
G.Q. Li, C.-H. Lee & G.E. BrownNucl. Phys. A 625, 372 (1997)
eμ
Kμ
?TOV equation: a condition at hydrodynamical equilibrium
Gravity
Nuclear pressureFor npe matter,
dP/dρ<0, if E’sym is big and negative (super-soft)
)()1(2
1)()0,(
4
1)()()(
22
20
ρρEδδδρEδρEρ
μρρ
Eρρ,δPρPρ,δP
symsym
ee
δ
asy
)2(
4 3
g
g
mrr
PπrmPε
dr
dP
Heavy-Ion Meeting 23
Astrophysical Implication
October 31, 2009
K0=211 MeV is used for this calculation; higher incompress-
ibility for symmetric matter will lead to higher masses, systemat-ically.The softest symmetry energy that the TOV is still stable is x = 0.93, giving Mmax = 0.11 M⊙ and R ≥ 28 km.
Heavy-Ion Meeting 24October 31, 2009
Range of density in HIC by
-incident energy -impact parameter
Types of particles formed
- emission time & den-sity
- n & p are emitted throughout
- Fragments (Z=3-20) at sub-saturation densi-ties
Change N/Z of nuclei
- larger N/Z ratio is preferable
π, n, p fragments
Experimental Principles
Heavy-Ion Meeting 25
Experimental Observ-ables
October 31, 2009
Signals at sub-saturation densities1)Sizes of n-skins for unstable nuclei2)n/p ratio of fast, pre-equilibrium nucleons3)3H/3He ratio4)Isospin fractionation and isoscaling in nuclear multufragmentation5)Isospin diffusion (transport)6)Differential collective flows (v1 & v2) of n and p
7)Correlation function of n and pSignals at supra-saturation densities
1)p-/p+ ratio2)K+/K0 ratio3)Differential collective flows (v1 & v2) of n and p
4)Azimuthal angle dependence of n/p ratio with respect to the R.P.Correlation of various observablesSimultaneous measurement of neutrons and charged particles
Heavy-Ion Meeting 26October 31, 2009
Soft
E sym
Stiff Esym
Central den-sity
More neutrons are emit-ted from the n-rich sys-tem and softer symme-try energies.
Yield Ratio
■n/p□3H/3He
610
500
)/(
)/(.
sym
.sym
ρρE
ρρE
M. A. Famiano et al. RPL 97, 052701 (2006)
Double ratio: min. systematic error
ImQMD
Y(n
)/Y(p
)
Esym(r)=12.7(r/r0)2/3+17.6(r/r0)gi
Heavy-Ion Meeting 27
Yield Ratio (π-/π+)
October 31, 2009
Data: FOPI Collaboration, Nucl. Phys. A 781, 459 (2007)IQMD: Eur. Phys. J. A 1, 151 (1998)
Need a symmetry energy softer than the above to make the pion produc-tionregion more neutron-rich!
2/3 0
00
2/3100 3(2corresponding t 1) ( )
5o ( )
8 FsymE E
Heavy-Ion Meeting 28
π-/π+ Ratio
October 31, 2009
Stiff Esym
Soft Esym
p- /p
+
(N/Z) reaction system
KoRIA
Heavy-Ion Meeting 29
Isospin Diffusion Param-eter
October 31, 2009
No isospin diffusion between symmetric systems
Isospin diffusion occurs only in asymmetric systems A+B
Non-isospin diffusion effects are the same for A in A+B & A+Aand also for B in B+A & B+B
BBAA
BBAAABi xx
xxxR
2/)(
2
F. Rami et al., FOPI, PRL 84, 1120 (2000)B. Hong et al., FOPI, PRC 66, 034901 (2002)Y.-J. Kim & B. Hong, in preparation
124124
112112
124112
Ri = +1
Ri = -1
Ri = 0 for
complete mixing
Heavy-Ion Meeting 30
Isospin Diffusion Param-eter
October 31, 2009
Projectile
Target
124Sn
112Sn
soft
stiff
Symmetry energy drives system towards equilibrium
stiff EOS : small diffusion (|Ri| ≫ 0)
soft EOS : large diffusion & fast equilibrium (Ri 0)
M.B. Tsang et al., PRL 92, 062701 (2004)
Heavy-Ion Meeting 31
Isospin Diffusion Param-eter
October 31, 2009
L.W. Chen et al., PRL 94, 032701 (2005)
Observable in HIC is sensitive to the r dependence of Esym and should provide constraints to the symmetry en-ergy.
0.69 1.05
stiff
IBUU04: Esym(r)~31.6(r/ro)g
soft
Esym(r)=12.7(r/ro)2/3+12.5(r/ro)gi
stiff soft
M.B. Tsang et al., PRL 92, 062701 (2004)
pBUU i~2 0.69 1.05
Korean Physical Society 32
Isospin Diffusion Param-eter
October 21-23, 2009
Esym(r)=12.5(r/r0)2/3+17.6 (r/r0)gi
)exp()8~3(
)8~3(
112112
124124 αNZY
ZYf
0.4gi 1
Ri(α
)
)Be(/)Li(
)Be(/)Li(7
1127
112
7124
7124
YY
YYf
Ri(f
)
0.4gi 1
NSCL/MSU Data at Low Energy
Heavy-Ion Meeting 33
Collective Flow
October 31, 2009
Stiff
SuperSoft
0
2
220
)(9
ρρ
symsym ρ
ρEρK
LargeN/Z
SmallN/Z
B.-A. Li, PRL 85, 4221 (2000)
Als
o k
now
n a
s v
1
Heavy-Ion Meeting 34
Multi-Purpose Detector
October 31, 2009
Heavy-Ion Meeting 35October 31, 2009
Tentative designunder discussion
Heavy-Ion Meeting 36
Summary1. Rich physics with RI beams
Neutron & proton drip lines Neutron halo & skin structures Nuclear Astrophysics Super-heavy elements Fundamental symmetries Nuclear symmetry energy
- Long-standing problem in nuclear physics- Crucial to understand the neutron matter- Crucial to understand the astrophysical objects
October 31, 2009
2. KoRIA First large scale accelerator for basic science in Korea We need your help & participation!