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!