Hot and Dense QCD - Istituto Nazionale di Fisica...
Transcript of Hot and Dense QCD - Istituto Nazionale di Fisica...
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Hot and Dense QCD
T. Hatsuda (Univ. Tokyo)
Present (2001-):Two major experimentsto probe the early Universe
WMAP (2001-)
RHIC (2001- )
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Future (2007-):LHC (CERN) & Planck (ESA)
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Outline of this talkOutline of this talk
1. Origin of masses– a major challenge in modern physics
2. Recent progress in hot QCD– strongly interacting plasma
3. Recent progress in dense QCD– new phases dense matter
4. Summary
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Origin of masses
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“Origin of masses” Structure of the vacuum“Origin of masses” Structure of the vacuum
Cosmological constantEinstein (1917)
Universe
baryons
QCD condensateNambu (1960)
baryon
quark
EW condensateAnderson (1963)Englert-Brout, Higgs (1964)
quark
barequark
WMAP (2001-), Planck (2007-) RHIC (2001-), LHC (2007-) LHC(2007-)
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Birth of QCDBirth of QCD
’65 SUc(3) YM theory as a model of strong interactionNambu (’65)
(Nobel foundation)
’65-’72 First indication of asymptotic freedomVanyashin & Terenteev (’65), Khriplovich (’69), ’t Hooft (’72)
Late ’60-early ’70 Discovery of quarks in DIS Friedman, Kendall & Tayler Nobel Prize 1990
’73 Discovery of asymptotic freedomGross & Wilczek, Politzer Nobel Prize 2004
’74 Discovery of heavy QCD bound state (J/ψ)Richter, Ting Nobel Prize 1976
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Asymptotic freedom Asymptotic freedom
qqmqAtiqGGL aaa
a g −−∂+−= )(41
µµµµν
µν γ
Energy scale (GeV)
Effective coupling(αs = g2/4π)
αs
ColorConfinement
Asymptotic freedom
(int)/(kin) << 1
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Asymptotic freedom = Pauli para-magnetismAsymptotic freedom = Pauli para-magnetism Nielsen (’81)Hughes (’81)
Electric property Magnetic property
QED > 1 (screening) < 1 (dia-magnetism)
QCD < 1 (anti-screening) > 1 (para-magnetism)
sum of Landau levels
BVacuum energy under uniform B
Pauli para-magnetismvs Landau dia-magnetism
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Color confinement
Nobel foundation
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Seven Prize Problems ($1 million allocated to each)
Important classic questions in mathematics that have resisted solution over the years (Clay Mathematics Institute, May 24, 2000)
1. Birch and Swinnerton-Dyer Conjecture2. Hodge Conjecture 3. Navier-Stokes Equations4. P vs NP5. Poincare Conjecture6. Riemann Hypothesis7. Yang-Mills Theory
Official description by A. Jaffe and E. Witten
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Lattice QCD approach to confinementLattice QCD approach to confinement
Wilson (’74)
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Lattice QCD simulationsLattice QCD simulations
Quenched QCDFull QCD
Integration : Monte Carlo with importance sampling
hypercube
slab
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Why lattice ?
• Well defined QM (finite a and L) • Gauge invariant • Fully non-perturbative
0.1 fm 2-3 fm
Continuum and thermodynamic limits
• Equation of state of hot plasma• Phase transition (critical temperature, order etc)• Static and dynamic correlations near equilibrium
What one can do in principle
• Cold degenerate plasma • Phenomena far from equilibrium
What one cannot do (at present)
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Examples (quenched QCD)Examples (quenched QCD)
R
0.5 fm 1.0 fm
Linear confining string
Bali, Phys. Rep. 343 (’01) 1
Heavy-quark bound states
CP-PACS, Phys. Rev. D65 (’02) 094508
2S+1LJ
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Color Deconfinementn
T<Tc T~Tc T>Tc
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http://boojum.hut.fi/research/theory/typicalpt.html
4HeH2Oλ
-line
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QCD Phase DiagramQCD Phase Diagram
T
μB
Quark-Gluon Plasma
ColorSuperconductor
Hadronic Fluid
Vacuum
CriticalEnd point
Triplepoint ?
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Equation of State at finite T (full QCD)Equation of State at finite T (full QCD)
Black-body radiation for massless particles :
Karsch, Lect.Notes Phys.583 (’02) 209
SB limit
Nf = 2
Nf = 2+1
Nf = 3
Tc = 173±8 MeV (Nf=2)= 154±8 MeV (Nf=3)
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Fate of the color string (full QCD)Fate of the color string (full QCD)
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Karsch, Laermann, Peikert, Nucl. Phys.B605 (’01) 579
T=0
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Order of the finite T transitionOrder of the finite T transitionPisarski and Wilczek (’84)
Yaffe & Svetizky (’83)
m u,d
ms
1st
1st
cross over
2nd
∞
∞
Nf=3
Nf=2
Nf=1
Nf=0∞
0
(Quenched QCD)
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μB QCD Phase DiagramQCD Phase Diagram
Colorsuperconductor
Quark-gluon plasma
~ 1 GeV
Hadronic fluid
Vacuum T ~ 170 MeV
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Static plasma properties at T > Tc
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QGP for g << 1 ( T >> 100 GeV )QGP for g << 1 ( T >> 100 GeV )
Inter-particledistance
Electric screening
Magneticscreening
1/T
1/gT
1/g2T
Relativistic plasma :
“Coulomb” coupling parameter :
Debye number :
S. Ichimaru, Rev. Mod. Phys. 54 (’82) 1071
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Problems of high T perturbation
I. Strong coupling problem
g ~ 2 for T=200-400 MeV
badly behaved perturbation series
soft magnetic gluons are always non-perturbativeeven if g 0
pertubation theory
II. Non-Abelian magnetic problem
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I. Strong coupling problemI. Strong coupling problem
T=100GeV T=1 GeV T=0.2 GeVQCD Pressure (Nf=4)
naive perturbation: meaningful only for T>100 GeV
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II. Non-Abelian magnetic problem II. Non-Abelian magnetic problem
EOS : A. Linde, Phys. Lett. B96 (’80) 289
μ ν
magnetic screening :
“Debye” screening :
Kraemmer & Rebhan, Rept.Prog.Phys.67 (’04)351
QCD is non-perturbative even at T =∞ ( L3x(1/T) L3 )
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soft magnetic gluons are always non-perturbativeeven if g 0 (T ∞)
pertubation theory from O(g6)
(mmag~ g2T)
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Screening masses at T>Tc on the lattice Screening masses at T>Tc on the lattice
Quenched SU(3)20×20×32×6Lorenz gauge
m = gT
Nakamura, Saito & Sakai, Phys.Rev.D69 (’04) 014506
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8133 ⊕=⊗
3633 ⊕=⊗
0.5fm0.25fm
243×6Lorenz gauge
T/Tc=3.04
Heavy quark “potentials” at T>Tc (quenched)Heavy quark “potentials” at T>Tc (quenched)
Nakamura & Saito, Prog.Theor.Phys.111, 112 (’04) hep-lat/0406038, 0404002
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Heavy quark “potentials” at T>Tc (quenched)Heavy quark “potentials” at T>Tc (quenched)
8133 ⊕=⊗ 3633 ⊕=⊗
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Dynamic plasma properties at T > Tc
Dynamic structure factor of the vacuumvacuum
γ*
PDG(’04)
plasma
γ*Dynamic structure factor of the plasma
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system
probeMethod in lattice QCDMethod in lattice QCD
∫∫
=
= +
ωωωτ
ττ
dpAK
xdeJxJpD xpi
),(),(
)0,0(),(),( 3
r
rr rr
Maximum Entropy Method
latticeQCD data
knownkernel
spectral function= dynamic structure factor
Asakawa, Nakahara & T.H, Phys. Rev. D60 (’99) 091503 Prog. Part. Nucl. Phys. 46 (’01) 459
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D = K×A
D A D A
Image reconstruction by MEM
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D = K×A
D A D A
Image reconstruction by MEM
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Quark-anti-quark ound state above Tc ? Quark-anti-quark ound state above Tc ?
charmstrange
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Spec
tral
func
tion ρ
(ω)
J/ψ(3.1GeV)
1. J/ψ survivesup to 1.6 Tc
2. J/ψ disappears in 1.6 Tc < T < 1.7 Tc
see also,Umeda et al, hep-lat/0401010Datta et al., PRD 69 (’04) 094507
Asakawa & T.H., PRL 92 (’04) 012001
cc bound state above Tc (quenched) cc bound state above Tc (quenched)
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Spec
tral
func
tion ρ
(ω)
J/ψ(3.1GeV)
1. J/ψ survivesup to 1.6 Tc
2. J/ψ disappears in 1.6 Tc < T < 1.7 Tc
see also,Umeda et al, hep-lat/0401010Datta et al., PRD 69 (’04) 094507
Asakawa & T.H., PRL 92 (’04) 012001
cc bound state above Tc (quenched) cc bound state above Tc (quenched)
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ss bound state above Tc (quenched) ss bound state above Tc (quenched) A
(ω)/ω
2Mφ(T=0)=1.03 GeV
T/Tc= 1.4
Asakawa & T.H., Prog. Theor. Phys. Suppl. 149 (‘03) 42
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Possible mechanisms of supporting “hadrons” above Tc
Possible mechanisms of supporting “hadrons” above Tc
1. Strong correlationsin JP=0+ (σ) and JP=0- (π) channels above Tc
Kunihiro and T.H., Phys. Rev. Lett. 55 (’85) 88
2. Dynamical confinementin all color singlet channels above Tc
DeTar, Phys. Rev. D32 (’85) 276
3. Strong Coulomb interactionin color singlet and non-singlet bound statesabove Tc
Shuryak and Zahed, Phys. Rev. D70 (2004) 054507Brown, Lee, Rho and Shuryak, Nucl. Phys.A740 (’04) 171
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Shear viscosity (quenched)Shear viscosity (quenched)
1.0 1.5 2.0 2.5 3.0 T/Tc
Nakamura and Sakai, PRL 94 (’05) 072305
Baym, Monien,Pethick & Ravenhall (’90)
Arnold, Moore & Yaffe, (’03)
Kovtun, Son & Starinets (’04)
Viscous fluidR << 1
Perfect fluidR >> 1
“Reynolds number”
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Possible structure of QCD plasmaPossible structure of QCD plasma
Chiral dynamics pQCDLattice QCD
RHIC, LHC
Weakly int.pion plasma
Strongly int.Resonanceplasma
Strongly int.q+g+”hadron”plasma
weakly int.q+g plasma
q+g plasma
viscous fluid ?perfect fluid ?
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Relativistic Hydrodynamcsfor High-Energy Hadron Collisions
Relativistic Hydrodynamcsfor High-Energy Hadron Collisions
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Expansion
Freezeout(T = 1.95 K neutrino)T = 2.73 K photon
Tchem = 170 MeVTtherm = 120 MeV
ObservablesCMB & anisotropy(CνB, CGB & anisotropy)
Collective flow & anisotropyJets, leptons, photons
Big Bang Mini Bang
Initial state Inflation ? (10-35 sec) Color glass ? (10-1 fm)
Thermalization Inflaton decay decoherence
Parametersto be
determined
8~10 cosmological parameters・ Initial density fluctuation・ Cosmological const. Λ etc
QGP parameters・ Initial energy density・ Equation of state etc
Evolution Code e.g. CMBFAST 3D-hydro ?
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WMAP: Astrophys. J. Suppl. 148 (2003) 1, 175
Precision cosmologyPrecision cosmology
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CGC + 3D-hydro + jet simulationCGC + 3D-hydro + jet simulation Hirano and Nara, nucl-th/0404039
-- First complete & sucessful study from intial to final --
Au+Au sNN1/2 = 200 GeV
Extract QGP parameters with errors
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Dense QCD
10 km
?
?
N. Itoh (’70), E. Witten (’84)Baade-Zwicky (’34)
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T
μB
Quark-gluon plasma
~ 1 GeV
Hadronic fluid
Vacuum
Colorsuperconductor
High density QCD High density QCD
~ 170 MeV
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Color Superconductivity in Quark MatterColor Superconductivity in Quark Matter
Variety of phasesCFL, 2SC, dSC, uSCgapless phase, …
1. Highly relativisiticLong range magnetic int.
2. Color-flavor entanglement
Major differences from BCS
High Tc superconductorTc/pF ~ 0.1
Compact Cooper pairsize ~ 1-10 fm
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Three fundamental phases in quark matterThree fundamental phases in quark matter
∆ 3
∆1
∆ 2
CFLdSC
2SC
(ds)
(us)
(du)
⎟⎟⎟
⎠
⎞
⎜⎜⎜
⎝
⎛
∆∆
∆=∆
3
2
1
000000
ia
2SC: Bailin, Love, Phys. Rep. 107 (’84)CFL : Alford, Rajagopal, Wilczek, Nucl. Phys. B537 (’99)dSC: Iida, Matsuura, Tachibana & Hatsuda, Phys. Rev. Lett. 93 (’04)
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T
μB
~ 1 GeV
Hadronic fluid
Vacuum
High Density QCDHigh Density QCD
CFL
2SC
dSC
~ 170 MeV
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μBdq
ξc
Abuki, Itakura & T.H., PRD65 (’02)
100
101
102
103
104
105
⌧ c/d
q
103 104 105 106
[MeV]
to BEC ?
BCS
pF(MeV)
ξc/dq
BCS BEC RBECcrossovers ?
Nishida and Abukihep-ph/0504083 (’05)
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40K : JILA, PRL 92 (2004) 0404036Li : Innsbruck, PRL 92 (2004) 120401
MIT, PRL 92 (2004) 120403
40KCond. of Fermionic-Atom Pairs
N0/N = 1% 5% 10%
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Neutron Star StructureNeutron Star Structure
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M-R relation in APR EoSM-R relation in APR EoS (ρmax ~ 6ρ0)
Vela-X1Cyg-X2
PSR1913+16
J0751+1807
Neutron starbinary
X-ray binaries
Neutron star- WD binary
EXO0748-676(X-ray bursts)
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astro-ph/0411207 i
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Nature 420 (’02)
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M-R relation in APR EoS + CFL quark matter M-R relation in APR EoS + CFL quark matter
Free QM
Int. QM
Alford et al., nucl-th/0411016
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Cooling of neutron stars Cooling of neutron stars St
anda
rdEx
otic
quen
chin
g
n superfluidityQ color super
exp(-Δ/T)
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Cooling of neutron stars Cooling of neutron stars St
anda
rdEx
otic
quen
chin
g
n superfluidityQ color super
exp(-Δ/T)
log (time/yr)
log (Ts /K
)log
(Ls /(e
rg/s
))
Weber, astr-ph/0407155 (’04)
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Future Experimental Facilities for hot/dense QCDFuture Experimental Facilities for hot/dense QCD
LHC (2007-)
2.8 TeV/A
・ Hottest matter ・ Precision QGP
J-PARC (2007-)
50 GeV PS
Phase I・ Dense mesic nuclei・ Exotic hadrons
Phase II・ Primary beam phys.
SIS100/300 (201? -)
90 GeV PS
・ Densest matter ・ In-medium hadrons
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SummarySummary
Hot QCD is becoming a mature field
(3+1)-dim.Hydro. Code
pQCD (jet, CGC)
LQCD (EoS, SPF)
Heavy Ion data
Key questions
1. Why & how thermalization happens? Perfect fluid ?
2. How complex is QGP ? How we can characterize it ?
3. Direct evidence of the evaporation of QCD condensates ?
RHIC LHC : temperature scan, precision QGP
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Big Bang
(1992-)
SPS (1994-)
(2001-)
RHIC (2001-)
Planck (2007-)
LHC (2007-)
Q.G
.P.
Little Bang
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Dense QCD is still an open field
BoseNova (JILA)BCS-BEC (JILA)
1. New phases in color superconductor, e.g. CFL, 2SC, dSC (how to access?)
2. Transition from HM QM still unclear(need new idea to solve dense QCD)
3. Obs. progresses in studying M and R of the neutron stars (2 solar mass?)
4. Common physics with atomic condensates (e.g. BCS-BEC crossover)
Present and future
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1. What is quark-gluon plasma
Part I. Basic Concept of Quark-Gluon Plasma:
2. Introduction to QCD3. Physics of quark-hadron phase transition 4. Field theory at finite temperature 5. Lattice gauge approach to QCD phase transitions 6. Chiral phase transition 7. Hadronic states in hot environment
Part II. QGP in Astrophysics:
8. QGP in the early universe9. Compact stars
Part III. QGP in Relativistic Heavy Ion Collisions:
10. Introduction to relativistic heavy ion collisions 11. Relativistic hydrodynamics for heavy ion collisions 12. Transport theory for pre-equilibrium process 13. Formation and evolution of QGP 14. Fundamentals of QGP diagnostics 15. Results from CERN-SPS experiments 16. First results from BNL-RHIC 17. Detectors in relativistic heavy ion experiments
Appendices A-H: 120 Exercises
to appear in a few months
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Дякую !
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Back up slides
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Quark flavorsQuark Flavors Quark Flavors
Heavy quarks mc~1.5 GeVmb~5 GeVmt~178 GeV
Light quarks
mu~3MeVmd~7MeVms~100MeV
Tc ~ 170 MeVμc ~ 400 MeVms~100MeV
same order
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More on QCD Phase Transition at finite T (full)More on QCD Phase Transition at finite T (full)
(i) String fluctuation and breaking(ii) Restoration of broken symmetries
)1()3()3( BRL USUcSU ×× +
0≠qq
low D : Hadronic phase
Low T
2)3( ZSU RLC ×++
0≠qq
high D : color supercond.
Low T
)1()]3()3([)3( BRLC USUSUSU ×××Quark gluon plasma
High T
?
Pisarski & Wilczek, PRD29 (’84) e.g. Matsuura, Iida, Baym and T.H.,PRD69 (’04)
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H2O
4He 3He
PhaseDiagrams
PhaseDiagrams
http://boojum.hut.fi/research/theory/typicalpt.html
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sign problem:
Dense QCD (T~0, μ large)Dense QCD (T~0, μ large)
Complex
Complete new idea necessary
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History of our Universe
History of our Universe