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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