H. Sakurai

RIKEN Nishina Center

Before summarizing this workshop….

Nuclear reaction activities in Japan at RIKEN

Experimentalists (Heavy Ion Reactions)

High Energy “QGP” Physics at RHIC-Phenix, LHC Tsukuba U., Hiroshima U., CNS U. Tokyo, Kyoto U., RIKENIntermediate Energy TITech, Tsukuba U., Rikkyo U., RIKEN (1990) -> 0 (2000) ->Kyoto U.(T.Murakami) , RIKEN(Y.Nakai, H.S.)Low Energy: Fusion/Fission, DIS RIKEN, JAEA, KEK

TheoristsQCD-based Kyoto U., Osaka U.AMD, (R)QMD Tohoku U.(A.Ono), JAEA, Nihon-U.Fusion/Fission Tohoku U., Kansei U., Kyoto U., JAEA

Projectile Fragmentation at RIPS

Pi-production measurement at HIMAC

Range counters for pi-detection

Response of the spectators to the participant blast1A GeV U @GSI, PRL90, 212302(03)

Pb

Ti

40A MeV Ar @RIKEN, Notani et al 　 PRC.

Be

Ta

Hardness of equation-of-stateMomentum dependence of mean field

Shi et al., PRC64, 034061(01)

RIPS GARIS

60~100 MeV/nucleon

CRIB (CNS)

~5 MeV/nucleon

350-400 MeV/nucleon

Old facility

New facility

RIKEN RI Beam Factory (RIBF)

BigRIPS

SRC

RILAC

AVF

RRCfRC

IRC

Experiment facility

Accelerator

SHARAQ (CNS)

SAMURAI

ZeroDegree

SLOWRI

SCRIT

RI-ring

SHE (eg. Z=113)

Intense (80 kW max.) H.I. beams (up to U) of 345AMeV at SRCFast RI beams by projectile fragmentation and U-fission at BigRIPSOperation since 2007

To be fundedIn phase II

SAMURAI Spectrometer Kobayashi et al 2011-

versatile spectrometer with a large superconducting magnet

80cm gap, BL~ 7Tm, Bmax=3T PID limited to A~100

Invariant/missing mass spectroscopy giant resonances single particle states via (p,2p) etc EOS in asymmetric nuclear matter : SAMURAI-TPC Particle correlations in a few-body system 3NF Coulomb breakup for radiative capture c.s. (p,), (n,)Fission study

15M$ covers SC-Magnet 9M$ Detectors neutron counter electronics, software STQ for BT

Heavy ion collisions and dynamics of nuclear matter (experiment)

Cluster formation in dilute matter J.B.NatowitzBimodality of the heaviest fragment distribution B.BorderieIsospin Effects in 40,48Ca+40,48Ca W.G.LynchIsospin Diffusion in 58Ni induced HIC M.F.RivetDynamical emission of neutrons M.VeselskyConstrains on Symmetry Energy from Sn+Sn M.B.TsangCollective flow in 400A MeV Au+Au W.Trautman

Cross section and isospin effect in PF Wen-Dong Tianp-p correlation from breakup of 22Mg, 20Ne Xiao-Yan Sun/Jin-Gen Chen

Relativistic …

Correlations – Cluster Formation Bose Condensates Efimov States Superfluidity

PerfectLiquid?

PerfectGas ?

Few Body Syst.Suppl. 14 (2003) 361-366 Eur.Phys.J. A22 (2004) 261-269

J.B.Natowitz

GAS

LIQUID

L.Qin et al. In Preparation

J.B.Natowitz

IWND09 Bernard Borderie

INDRA@GANIL and INDRA-ALADIN@GSI

IWND09 Bernard Borderie

Bimodal behavior of the heaviest fragment distribution as signature of a

first order phase transition in finite systems

latent heat of the phase transition(EG-EL) for heavy nuclei Z~ 70

8.1 (±0.4)stat (+1.2 -0.9)syst AMeV

syst. error: different QP selectionsE.Bonnet, D. Mercier et al, PRL August

2009

Z1 versus E* using the deduced parameter values

Strategies used to study the symmetry energy with Heavy Ion collisions

• Vary the N/Z compositions of projectile and targets

124Sn+124Sn, 124Sn+112Sn, 112Sn+124Sn, 112Sn+112Sn

• Measure N/Z compositions of emitted particles

n & p yields & flow, N/Z of fragments

isotopes yields – isospin diffusion

+ & - at high incident energyNeutron Number N

Pro

ton

Nu

mb

er Z

3/2AaAaB SV 3/1

)1(

A

ZZaC

A

ZAasym

2)2(

Isospin degree of freedom

Hub

ble

S

TCrab Pulsar

B.Tsang

i

i

i

ImQMD model describes np ratios and two isospin diffusion measurements:

S()=12.5(/o)2/3 +17.6 (/o)i

Consistent constraints from the 2 analysis of three observables i

B.Tsang

Isospin diffusion data at E/A=35 MeV

Data are in good agreement with i~0.5, consistent with E/A=50 MeV data.

No complete stopping & no isospin equilibrations in central collisions

B.Tsang

Constraints from HIC at sub-saturation density:Sn+Sn collisions at E/A=35 and 50 MeV

Consistent withIAS, PDR & GDR

Summary

B.Tsang

III. First results from FOPI/LAND experimentAu+Au 400 A MeV

SB: shadow bar for background measurement

PLAWA

LAND 2LAND 1

SB

neutron squeeze-out: Y. Leifels et al., PRL 71, 963 (1993)

W. Trautmann

pt dependence of v2

Data: (PM3-PM5, 0.25<y/yp<0.75)- |v2| increases as expected- well reproduced by UrQMD- but: 15% correction missing

let's look at ratios only:- large errors at large pt

-UrQMD: decreasing sensitivity at pt>0.8

result from neut/hydro ratios:- <> = 0.94 ± 0.21- potential part just below linear

W. Trautmann

Introduction to HIRFL: Beam facilities

N

CSRm

CSRe

SFC

SSC

SFC: 10 AMeV (H.I.), 17~35 MeV (p)

SSC: 100 AMeV (H.I.), 110 MeV (p)

CSRm: 1000 AMeV (H.I.), 2.8 GeV (p)

RIBLL1: RIBs at tens of AMeV

RIBLL2: RIBs at hundreds of A MeV

CSRe: storage ring with deceleration

RIB

LL

2

RIB

LL

1

H.S.Xu

ETF I: ETF I: External Target Facility, Phase IExternal Target Facility, Phase I

Hard-photon emission Y.G. Ma

H.S.Xu

ETF II:ETF II: External Target Facility, Phase IIExternal Target Facility, Phase II

CsI+Clover 探测器

TPC

硅条探测器阵列CsI+Clover 探测器

TPC

硅条探测器阵列

New DetectorsNew Detectors

• -ball (CsI(Tl) array + Clover)• TPC (at target region)• Si-strip array (behind TPC)• MWPC (inside dipole)Possible PhysicsPossible Physics

• For RIB Physics• For EoS of asymmetry nuclear matter• For high baryon density matter

To be constructed within 3 years

H.S.Xu

CSRCollective motion effect of 129Xe+129Xe Fei XieSpecial orientation in deformed U+U Ke-Jun WuPion emission Z.G. Xiao

Hard-photon emission Y.G. Ma

Future programs

Total Interaction Cross Sections for the Ne isotopesM. Takechi, et al. NN2009

Cross section enhancement at28-32Ne has been observed. deformation effects? dynamical effects?

Cross section jump at 31Ne p-wave halo ?

240AMeV Ne+C at BigRIPS

Heavy Ion Collision Dynamics, Symmetry Energy (theory)

Transport modelsIBUU04 IQMD Xi-Guang CaoImIQMD Feng-Shou Zhang fusion-application, shell effects etc.ImQMD Ying-Xun ZhangUrQMD Qing-Feng Li HBT

Langevin Fusion/Fission coupled with particle emission Wei YeSAA Chu-Wang Ma skin effects in fragmentation??

Relativistic …

Higher order effects of SE LW.CHen

QHD Greco Relativistic-framework E>400A MeV

The Ksat,2 of asymmetric nuclear matter

then we have:

If we use the parabolic approximation to the EOS of symmetric nuclear matter, i.e.,

2 3 0000

00( ) ( ) ( ),

2! 3E E O

K

sat,2 0

sat,2

0 0 sym

0sym

0

, , and :, i.e.,

are determined by characteristic parameter

s defin t 4

6

ed a K J L K

JK LK L

K

K

symsat,2 asy6K K L K

which has been used extensively in the iterature to characterize the isospin dependence of

the incompressibility of asymmetric nuclear matter.

II. Formulism L.W.Chen

Constraining Ksat,2

V. Constraining the Ksat,2 parameter

0

sym 0

*s,0

240 20 MeV

( ) 30 5 MeV

0.8 1

: 46 111 MeV

K

E

m m

L

K0 J0/K0

L Ksym

sat,2 370 120 MeVK

Only 5 Skyrme forces in the 63 Skyrme forces used are consistent with all empirical constraint:SKM, Gs,Rs,SKO,SKO*

L.W.Chen

Kaons:- direct early production: high density phase- isovector channel effects

Au+Au@1AGeV

/K production in “open” system: Au+Au 1AGeV, central

Production stopped at the maximum of the ’s production ~15 fm/c,K’s purely coming from maximum densityNot affected by rescatterng absorption

Greco

In-In-ConclusionConclusionWhile the EOS of symmetric NM is fairly well determined, the

density (and momentum) dependence of the Esym is still rather uncertain.

Can it be done like for the symmetric part? Particle production

• Ratios and + are sensitive probe to high density Esym

- kaon signal is a sharp signal from high density

• Competing effect in isospin particle ratio production: - self-energies revert the dependence respect to the n/p

emission

- a more careful treatment of the collision integral respect to - a more careful treatment of the collision integral respect to the elastic one is essential !the elastic one is essential !

• EE≥ 1.5 A GeV can have a transient quark phase highly ≥ 1.5 A GeV can have a transient quark phase highly

asymmetricasymmetric

- signatures and effective field theories to be developed- signatures and effective field theories to be developed

Greco

Nuclear forces, 3NF, medium effects

Microscopic approach based on DBHF, ChPT R. MachleidtThe ab-initio approach to nuclear matter and its extreme states F. SammarrucaConsistent three-body force with Bonn B potential and Zeng-Hun Lineutron star structure

Isovector and spin-isospin responses F. Braghin

Isospin-dependent pion in-medium effects on charged pion ratio in HIC C.M.KoN-N cross-sections in symmetric and asymmetric matter Hong-Fei Zhang

deuteron-proton elastic scattering at 250A MeV- complete data set of deuteron analyzing powers -

online analysis (very preliminary)with 3NF

w/o 3NF

Sekiguchi et al.

2009 April

Neutron Stars

Symmetry energy on gravitational waves B.A.LiNuclear constraints on properties of neutron star crusts Jun XuEffect of the symmetry energy on gravitational waves De-Hua Wenfrom axial perturbation of neutrons starConstraining the density dependence of the symmetry Wei-Zhou JiangEnergy in finite nuclei and nuclear matter

Nuclear StructureSuper heavy Nuclei (RMF) Z.Z.RenShape coexistence in 75Kr Ying-Chu Yang

Gravitational waves from elliptically deformed pulsars

xx yy

zz

I I

I

Equatorial Ellipticity of pulsars

Mass quadrupole moment

Breaking stain: fractional deformation when the crust fails

EOS

B. Abbott et al., PRL 94, 181103 (05)B.J. Own, PRL 95, 211101 (05)

Solving linearized Einstein’s field equation of General Relativity, the leading contribution to the GW is the mass quadrupole moment

Frequency of the pulsar

Distance to the observer

Moment of inertia B.A.Li

Constraining the strength of gravitational wavesPlamen Krastev, Bao-An Li and Aaron Worley, Phys. Lett. B668, 1 (2008).

Compare with the latest upper limits from LIGO+GEO observations

Depends on the symmetry energy and structure of NS

or 0.1

ӿ

B.A.Li

Challenge to investigate EOS of neutron matter

(fm-3)

Normal density

E/A

[MeV

]

3NF　 T=3/2 channels?　 density dependence?

1S correlation BCS-BEC crossover in dilute system ( ~ 0.10) ?

3P2 correlation　　 pairing gap? Density depencence?

from nuclei to neutron starsB. A. Brown, PRL85 (2000) 5296

Role of di-neutron in skin? : collectivity, transfer reactions

Elastic d+p for T=1/2 Nuclear structure in very neutron-rich nuclei for T=3/2?Heavy-ion Collisions to achieve ~2-30 ?

????

pure neutron matter

Research Activities of Nuclear Physics in SINAPResearch Activities of Nuclear Physics in SINAP Radioactive beam physics and HIC (around ~MeV/u;

HIRF-CSR, RIKEN, TAMU etc)

total cross section & momentum distribution

nucleon-nucleon momentum correlation

isospin physics: fragment isoscaling & symmetric energy

multifrgamentation and liquid gas phase transition

anisotropic flow scaling of light particles

RHIC Physics @ STAR, BNL (~200GeV/c Au+Au)

STAR barrel Time-of-Flight Project

nuclear modification, ellitptic flow, spin ploarization

Mach-like cone and partonic cascade

relativistic hydrodynamics model

Shanghai Laser Electron Gamma Source (with <20MeV Photons) based on SSRF

future physics: nuclear astrophysics with photons

CUORE Collaboration (Gran Sasso Nat Lab, Italy)

Nuclear Energy Program

Y.G.Ma

I. Motivations

Density Dependence of the Nuclear Symmetry Energy

HIC’s induced by

neutron-rich nuclei

(CSR/Lanzhou,FRIB,GSI,RIKEN……)

Most uncertain property of an asymmetric

nuclear matter

What is the isospin dependence of the in-medium nuclear effective interactions???

Isospin Physics in medium energy nuclear physics

Neutron Stars …

Structures of Radioactive Nuclei, SHE …

Isospin Effects in HIC’s …

Many-Body Theory

Many-Body Theory

Transport Theory General Relativity

Nuclear Force

EOS for Asymmetric

Nuclear Matter

On Earth!!! In Heaven!!!

L.W.Chen

International Symposium on EOS and its associated topics

RIKENEnd of July 2010

A.Ono, B.Tsang, T.Murakami, H.S. + ?

Thank you Shanghai!!

Prof. Y.G.Ma, L.W.Chen