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Esy
m(ρ
B)
(MeV
)
ρB/ρ01 2 30
?
Esy
m(ρ
B)
(MeV
)
ρB/ρ01 2 30
?Equation of Equation of sstate of tate of
aasymmetricsymmetricicic nnuclear uclear mmatteratter aat supra-t supra-
saturation densitiessaturation densities
Equation of Equation of sstate of tate of aasymmetricsymmetricicic nnuclear uclear
mmatteratter aat supra-t supra-saturation densitiessaturation densities
CBM collaboration meetingApril 15, 2010, Darmstadt, Germany
Laboratory for nuclear physicsLaboratory for nuclear physics Division of Experimental Physics Division of Experimental Physics
R Ruđeruđer Bošković Bošković Institute, Zagreb, Institute, Zagreb,
CroatiaCroatia
Zoran Basrak
1950 – 2010
Introduction
Symmetry energy
Low densities
High density
Ongoing projrcts
Summary and outlook
Outline
*D.H. Youngblood et al., PRL 82 (1999) 691
From the nuclear monopole resonance* K∞ of symmetric nuclear matter
E (,T ) = E (T=0) + E’ (,T )
K∞ = 231 ± 5 MeV
Nuclear EOS
0 0
2 2 20( ) 9 ( / )K d E d
Side flow v1
Eliptic flow v2
P. D
an
iele
wic
z et
al., S
cien
ce 2
98
(2
00
2)
15
92
C.
Fu
chs
et
al.,
PR
L 8
6 (
20
01
) 1
97
4
Data from KAOS
N = Z
E(,) = E(,0) + 2Esym() + O(4)
= (n- p) / = (N-Z)/A
B (N,Z) = aVA - aSA2/3 – aCZ (Z - 1)/A1/3 - asym (N – Z )2 / A + Δ(A)
Bethe – Weizsäcker mass formula
Nuclear EOS – Asymmetric term
ma
ny
mo
re i
n:
B.A
. L
i et
al.,
Ph
Re
p.
46
4 (
20
08
) 1
13
Esym() ≈ E()neutr. matter - E()sym. nucl. matter
Various notations: Esym() = S(), = x = I
asym = 23.7 MeV
BHF
SkyrmeRMF
L.W
. Che
n et
al.,
PR
C80
(20
09)
0143
22
Symmetry energy• The density dependence
of symmetry energy is largely unconstrainedlargely unconstrained.
• What is “stiff” or “soft”“stiff” or “soft” (curvature) is density dependent
The asymmetry term contributes a greater uncertainty than does the symmetric matter
EOS.(Bao-An Li)
C.
Fu
chs
an
d H
.H.
Wo
lter,
Eu
Ph
J A
30
(2
00
6)
5
Z.
Xia
o e
t a
l., P
RL
10
2 (
20
09
) 0
62
50
2
Where Esym shows up Nuclear structure
Nuclear reactions
GDR & PYGNY RESONANCE
Supernova collapse
p / n ≤ 0.1 – 0.2
c ≤ (2-15)0
Neutron star
StabilityStability against gravitational collapse
Radial density profiledensity profile
Internal structurestructure, composition and evolutio
CoolingCooling mechanism
Esym dependent
ObservablesCooling rates of proto-neutron starCooling rates for X-ray bursters NS masses, radii and moments of inertia
J.M
. La
ttim
er
an
d M
. Pra
kash
, S
cien
ce 3
04
(2
00
4)
53
6
N-star observations
PULSAR
BINARY OBJECTS
Direct or modified Urca process
R & M coupled observables
“SQM” vs. “normal”
matter EOS ?
J.M. Lattimer and M. Prakash, Science 304 (2004) 536
By HIC in the Fermi energy regime
P
Nbefore after
Intermediate & relativistic energy HIC
Isospin sensitive observables
- n/p differential flow - meson production, π+/π-,K0 /K+
- etc.
Lack of data, but … - ASY-EOS experiment @ GSI - SAMURAI @ RIKEN
Constraining Esym
Finite symmetry energy at zero energy due to
clustering effects
0,K, p, n
Intermediate & relativistic energy HIC
Isospin sensitive observables
- n/p differential flow - meson production, π+/π-,K0 /K+
- etc.
Nuclear structure
data
Isospin- and momentum-dependentmomentum-dependent IBUU04 model calculation with the Gogny effective interaction
M.B. Tsang et al., PRL 92 (2004) 062701
Esym/A = 12.5 ( /0) = 2
BUU transport model calculation without momentum dependence
Esym as f(ρ) from MSU data
Added in-medium modificationsin-medium modifications of NN cross sections
L.W. Chen et al., PRL 94 (2005) 032701
B.A. Li & L.W. Chen, PRC 72 (2005) 064611
Esym/A = 31.6 ( /0) = 1.05
Esym/A = 31.6 ( /0) = 0.69
(Courtesy of W.G. Lynch)
Sub-saturation densities
Esym() = 12.5·u2/3 + C·uγ
M.B. Tsang et al., PRL 102 (2009) 122701
Expansion around ρ0
Esym(ρ) = S0 + L·ξ/3 + Ksym·ξ2/18 + …, ξ = (ρ - ρ0)/ρ0
Symmetry slope L & curvature Ksym
L = 3·[∂Esym/∂ρ]ρ=ρ0 /ρ0 = 3·Psym /ρ0
u = ρ/ρ0 P.
Danie
lew
icz
and L
ee,
NPA
81
8 (
20
09
)
A. Klimkiewicz et al., PRC 76 (2007) 051603
Two parameterizationsHIC fited by transport codes IBUU04, ImQMD
Isobaric analog states & Pygny dipole resonance
1. n-p squeeze-out data from Au+Au collisions at E = 400A MeV [Y. Leifels et al., PRL 71 (1993) 963] → the UrQMD code predicts a steady rise of Esteady rise of Esym sym
→ γ=0.60.3 [W. Trautmann et al., ProgPartNuPh (2009)].
1. n-p squeeze-out data from Au+Au collisions at E = 400A MeV [Y. Leifels et al., PRL 71 (1993) 963] → the UrQMD code predicts a steady rise of Esteady rise of Esym sym
→ γ=0.60.3 [W. Trautmann et al., ProgPartNuPh (2009)].
2. π+-/π+ yield ratio data for Au+Au collisions in a broad energy range [Reisdorf et al., NP A781 (2007) 459] → the IBUU04 code predicts a vanishing Evanishing Esymsym → γ=0.960.21, super soft asyEOSsuper soft asyEOS [Z. Xiao et al., PRL 102 (2009) 062502].
Supra-saturation densities
The only available data (FOPI and FOPI–LAND) result in a contradictory predictions for Esym:
(Courtesy of M.B. Tsang) Z.Q. Feng, G.M. Jin, PL B683 (2010) 140
Constraining Esym ( > 0)
Two experimental proposals:
- GSI: n-p differential flow - Nishina / RIKEN: pion production
SIS18 ASY-EOS experiment S394
Spoakpersons of ASY-EOS experiment R. Lemmon and P. Russotto (approved by GSI-PAC)
Zagreb, CroatiaCaen, Orsay, FranceDarmstadt, Frankfurt, GermanyIoannina, GreeceCatania, Milano, Napoli, ItalyKatowice, Krakow, Warsaw, PolandBucharest, RomaniaSantiago de Compostela, SpainLund, Malmo, SwedenDaresbury, Liverpool, United Kingdom
Kolkata, IndiaNSCL-MSU, Rochester, USA
Main observable: n/p differential flow
SIS18 ASY-EOS experiment S394
Au+Au @ 400A MeV (increased statistics)96Zr+96Zr @ 400A MeV 96Ru+96Ru @ 400A MeV
(increased isospin sensitivity)
}
Detect:Detect: n, p, t, 3He, N/Z of light IMFs
Determine:Determine: reaction plane, reaction centrality
Improve:Improve: statistics and neutron background determination + code clusterization algorithm
IPJ
ph
osw
ich
MS
U m
inib
all
.5 mLu
nd
-Sd
C C
alif
a
GS
I L
AN
D
LN
S C
him
era
Towards FAIR
132Sn, 106Sn beams
RIKEN experiment
Main partners: MSU & RIKEN
Main requirements: - pion detector with large solid angle - centrality filter
Solution: - SAMURAI superconducting dipole - TPC detector – should be operational in 2014 - and many more (neutron wall, light charged particles, IMFs, …)
B.A
. Li
, PR
C 6
7 (
20
03
) 0
17
60
1
SAMURAIA/Z = 3Ekin = 250A MeVBρ = 7.3 Tm
AT-TPC
differences in available - beams, - energies, and - intensities different observables chosen complementary parts in a global effort to constrain symmetry energy
NSF-PIRE project
NSCL-MSU (M.Y.B. Tsang) abd collaborators have started a Partnerships for International Research & Education (PIRE) project : collaborative research between US, Japan collaborative research between US, Japan and Europeand Europe [MSU, RIKEN, GSI (FAIR)]
European Science FoundationResearch Networking Programmes
Constraining the Symmetry Energy
CoSymECoSymE
European Science FoundationResearch Networking Programmes
Constraining the Symmetry Energy
CoSymECoSymE Z. Basrak, M. Colonna and W. Trautmann
Creation of discussion foradiscussion fora
ExchangeExchange of students & experts
Facilitate a global dimensionglobal dimension (complementarities to NSF-PIRE)
Timely initiativeTimely initiative
Prepare futurePrepare future
What for ?
- new intensive RIB facilities - train up a new generation of scientists to take over leadership
Open characterOpen character
CBM & Esym ( >> 0)The Science Mission of CBM (IMoU)
The primary mission of CBM is to study key questions of QCD in the region of moderate temperature and very region of moderate temperature and very high baryonic densitieshigh baryonic densities: - chiral symmetry restoration - nuclear equation of state - confinement CBM may contribute in clarifyingthe question of question of ““exoticaexotica” in ” in thetheneutronneutron-star core-star core
- deconfinement - quarkyonic matter - in-medium meson properties at high density - multi-strange hyperonic matter
Nuclear matter physics at SIS100
Nuclear equation-of-state: What are the properties and the degrees-of-freedom of nuclear matter at neutron star core densities?
Hadrons in dense matter: What are the in-medium properties of hadrons? Is chiral symmetry restored at very high baryon densities?
Strange matter: Does strange matter exist in the form of heavy multi-strange objects?
Heavy flavor physics: How ist charm produced at low beam energies, and how does it propagate in cold nuclear matter?
s
s
s
uud? Λ
Λ
Who ?European Science Foundation at present 30 member states
Who ?
1 Croatia
2 France
3 Germany
4 Italy
5 Poland
6 Romania
7 Spain
8 Sweden
9 United Kingdom
European Science Foundation at present 30 member states
Road map ?
Selection outcome – June 2010
Re-submission of Re-submission of full list of thefull list of the collaborating institutions and collaborating institutions and supporting agencies supporting agencies – mid October 2010
Launching CoSymE – January 2011
More info: - https://www.irb.hr/users/mkis/pdf/Cosyme.pdf - [email protected]
Esym related activities FOPI days in Split, May 2005 LAND Collaboration Meeting, 2006 Chimera-GSI Workshop, Dec. 2006 FOPI Collaboration Meeting, Apr. 2007 Asy-EOS Workshop, Catania, June 2008 R3B Collaboration Meeting, GSI, Apr. 2009 ESF Exploratory Workshop, Zagreb, Oct. 2009 Letter of Intent, spring 2008 Proposal for GSI PAC, spring, 2009 Submitted ESF RNP CoSymE, Oct. 2009
Asy-EOS 2 Workshop, Noto/Sicily, May 2010
Esy
m(ρ
B)
(MeV
)
ρB/ρ01 2 30
?
Esy
m(ρ
B)
(MeV
)
ρB/ρ01 2 30
?Equation of Equation of sstate of tate of
aasymmetricsymmetricicic nnuclear uclear mmatteratter aat supra-t supra-
saturation densitiessaturation densities
Equation of Equation of sstate of tate of aasymmetricsymmetricicic nnuclear uclear
mmatteratter aat supra-t supra-saturation densitiessaturation densities
CBM collaboration meetingApril 15, 2010, Darmstadt, Germany
Laboratory for nuclear physicsLaboratory for nuclear physics Division of Experimental Physics Division of Experimental Physics
R Ruđeruđer Bošković Bošković Institute, Zagreb, Institute, Zagreb,
CroatiaCroatia
Zoran Basrak
1950 – 2010
Thank you Thank you for your for your
attentionattention
Thank you Thank you for your for your
attentionattention