Space-time evolution of the Quark Gluon Plasma. Klaus Reygers / Kai Schweda Physikalisches Institut University of Heidelberg

Transcription

1 Space-time evolution of the Quark Gluon Plasma Klaus Reygers / Kai Schweda Physikalisches Institut University of Heidelberg

2 High-energy nucleus-nucleus Collisions

3 High-Energy Nuclear Collisions Time à Plot: Steffen A. Bass, Duke University CYM & LGT 1) Initial condition: 2) System evolves: PCM & clust. hadronization 3) Bulk freeze-out -Baryon transfer - parton/hadron expansion - hadronic dof - ET production -Partonic dof NFD - inel. interactions cease: NFD & hadronic TM particle ratios, Tch, µb string & hadronic TM - elas. interactions cease PCM & hadronic TM Particle spectra, Tth, <βt> 2/66

4 Space-time evolution QGP life time 10 fm/c s thermalization time 0.2 fm/c s à hydrodynamical expansion until freeze-out simplest model: only longitudinal expansion, 1d à Bjorken model Plot: courtesy of R. Stock. collision time 2R/γ = fm/c s 3/66

5 Outline Introduction Longitudinal expansion Bjorken picture Transverse expansion - transverse radial flow - transverse elliptic flow v 2 - higher harmonics, v 3, v 4, v 5, Hydrodynamical model description Summary 4/66

6 Rapidity distribution in A-A With increasing collision energy: - wider distribution, - becomes flatter around mid-rapidity 5/66

7 Bjorken model Velocity of the local system at position z at time t: z = z/t Proper time τ in this system: = t/ = t p 1 2 = p t 2 z 2 In the Bjorken model all thermodynamic quantities only depend on τ, e.g., the particle density: n(t, z) =n( ) This leads to a constant rapidity densityof the produced particles (at least atcentral rapidities): dn ch dy = const. 6/66

8 1d - Bjorken model (I) The 1D Bjorken model is based on the assumption that dnch/dy ist constant (around mid-rapidity). This means that the central region is invariant under Lorentz transformation.this implies βz = z/t and that all thermodynamic quantities depend only on the proper time τ Initial conditions in the Bjorken model: "( 0 )=" 0, u µ = 1 0 (t, 0, 0,z)= xµ Initial energy density 0 In this case the equations of ideal hydrodynamics simplify to d" d + " + p =0 7/66

9 Bjorken model (II) For an ideal gas of quarks and gluons, i.e., for " =3p, " / T 4 This leads to "( ) =" 0 0 4/3, T( ) =T 0 0 1/3 The temperature drops to the critical temperature at the proper time c = 0 T0 T c 3 And thus the lifetime of the QGP in the Bjorken model is " T0 3 QGP = c 0 = 0 1# T c 8/66

10 QGP lifetime in 1d - Bjorken model " 0 = 11 GeV/fm 3 = GeV 4 for 0 = 1fm/c 1=~c =0.197 GeV fm " 0 = g QGP 2 30 T 4! T 0 = 1/4 30 " 2 g Parameters Δτ QGP ε 0 τ = 3 GeV/fm fm/c ε 0 τ = 5 GeV/fm fm/c ε 0 τ = 11 GeV/fm2 3.9 fm/c Fixed parameters: Nf = 2, Tc = 170 MeV, τ0 = 1 fm/c 9/66

11 Quick estimate for LHC Bjorken formula: " 0 = hm T i A Transverse area in collisions with b 0: A R 2 Pb = (6.62 fm) fm 2 hp T i =0.66 GeV/c dn ch /d 1601 ± 60 dn = 3 dy y=0 2 m 2 1/2 1 hm T i {z } dn dy y=0 Estimate for the mean transverse momentum: Measured charged particle multiplicity: LHC: hm T i p (0.138 GeV) 2 +(0.66 GeV) 2 =0.67 GeV 1.02 (5% most central) dn ch d =0 = 2450 ± 92 Larger (up to 1.2) if p and K are taken into account " 0 = (11.7 ± 0.43) GeV/fm 2 (Pb+Pb@ p s NN =2.76 TeV) RHIC: 10/66 " 0 5GeV/fm 2 (Au+Au@ p s NN =0.2 TeV)

12 Energy density evolution in 1d-Bjorken τ 0 = 1 fm/c is generally considered as a conservative estimate for the use in the Bjorken formula. Other estimates yields shorter times (e.g. τ 0 = 0.35 fm/c) resulting in initial energy densities at RHIC of up to 15 GeV/fm 3 11/66

13 Transverse Expansion Transverse radial flow: particle spectra

14 2 ] c) -1 [(GeV/ dy d N dp T π 2 Particle Spectra* π π K (de/dx) p K (de/dx) p Λ Λ T th =107±8 [MeV] <β t >=0.55±0.08 [c] n=0.65±0.09 χ 2 /dof=106/90 solid lines: fit range Typical mass ordering in inverse slope from light π to heavier Λ Two-parameter fit describes yields of π, K, p, Λ T th = 90 ± 10 MeV <β t > = 0.55 ± 0.08 c Disentangle p T GeV, STAR [GeV/c] collective motion from thermal random walk 13/66

15 Thermal Model + Radial Flow Fit Source: each volume element is assumed to be in local thermal equilibrium: T fo boosted in transverse radial direction: ρ = f(β s ) E.Schnedermann, J.Sollfrank, and U.Heinz, Phys. Rev. C48, 2462(1993). σ E d 3 N dp 3 e (u µ p µ )/T fo p dσ µ dn R ( m rdrm T K T cosh ρ+ ( p 1 m T dm 0 * T ) T - I T sinhρ+ 0 * fo, ) T - fo, ( r + ρ = tanh 1 β T β T = β S * - ) R, α α = 0.5, 1, 2 random boosted 14/66

16 (anti-)protons From RHIC More central collisions m 2 T = pt + mass 2 Centrality dependence: - spectra at low momentum de-populated, become flatter at larger momentum stronger collective flow in more central collisions, <β t > = 0.55 ± 0.08 STAR: Phys. Rev. C70, (R). 15/66

17 Kinetic Freeze-out at RHIC 0) T and β T are anticorrelated 1) Multi-strange hadrons φ and Ω freeze-out earlier than (π, K, p) Collectivity prior to hadronization STAR Data: Nucl. Phys. A757, ( ), *A. Baran, W. Broniowski and W. Florkowski, Acta. Phys. Polon. B 35 (2004) ) Sudden single freezeout*: Resonance decays lower T fo for (π, K, p) Collectivity prior to hadronization Partonic Collectivity? 16/66

18 LHC: Identified particle spectra Spectra harder at LHC stronger collective flow at LHC than at RHIC 17/66

19 Collective expansion Blast wave parametrization describes spectra at 10% level Collective flow velocity increases from RHIC to LHC by 10% 18/66

20 Collective Flow - Energy Dependence Collectivity parameters <β T > and <v 2 > increase with collision energy strong collective expansion at RHIC! <β T >RHIC» 0.6 expected strong partonic expansion at LHC, <β T >LHC 0.8, T fo T ch K.S., ISMD07, arxiv: [nucl-ex]. 19/66

21 Lesson I At LHC, Initial energy density approx. 50 GeV/fm 3 much larger than critical energy density ε c = 0.7 GeV/fm 3 Strong collective expansion, <β T > = at highest collider energies Particles carrying strange quarks show that collective expansion develops before hadronization, <β T > = among quarks and gluons (?) 20/66

22 Transverse Expansion Transverse elliptic flow: event anisotropy

23 Anisotropy Parameter v 2 coordinate-space-anisotropy momentum-space-anisotropy y p y x p x ε = y 2 x 2 y 2 + x 2 v 2 = cos2ϕ, ϕ = tan 1 ( p y p x ) Initial/final conditions, EoS, degrees of freedom

24 P. Huovinen, private communications, 2004 v 2 in the low-p T Region - v 2 approx. linear in p T, mass ordering from light π to heavier Λ - characteristic of hydrodynamic flow, sensitive to EOS! 23/66

25 Elliptic flow in ALICE s NN > ~ 4 GeV:initial excentricity leads to pressure gradients that cause positive v 2 2 < s NN < 4 GeV:velocity of the nuclei is small so that presence of spectator matter inhibits in-plane particle emission ( squeeze-out ) s NN < 2 GeV:rotation of the ALICE, submitted for publication, arxiv: [nucl-ex]. collision system leads to fragments being emitted inplane 24/66

26 Non-ideal Hydro-dynamics Spectra and flow reproduced by ideal hydrodynamics calcs. Shear viscosity to entropy density ratio close to AdS/CFT bound M.Luzum and R. Romatschke, PRC (2008); P. Romatschke, arxiv: viscosity leads to decrease in v 2, ultralow viscosity sufficient to describe data Hydro-limit exceeded at LHC? 25/66

27 f(') =1+2v n cos(n') 26/66

28 Can there be v 3? figs.: courtesy of M. Luzum. reaction plane participant plane fluctuating initial state is seed for v 3 can CGC be challenged? 27/66

29 higher harmonics extract power spectrum of v n, like Planck* higher harmonics odd harmonics important v 3 : access η/s Higher harmonics strongly damped (v n, n>10 = 0) STAR, arxiv: [nucl-ex]; STAR, PRL 92 (2004) ; A. Mocsy and P. Sorensen, NPA 855 (2011) 241; B. Alver and G. Roland, PRC 81 (2010) ; Planck data: EAS and the Planck collaboration QGP plot: B. Schenke, S. Jeon, and C. Gale, arxiv: /66

30 Lesson II Geometrical anisotropy is seed for elliptic flow v 2 Elliptic flow v 2 sensitive to QGP equation of state Triangular flow v 3 due to fluctuations, e.g. in initial energy density Triangular flow v 3 especially sensitive to shear viscosity / entropy density ratio Higher harmonics v 4, v 5, strongly damped 29/66

31 Hydrodynamical model description Some basic concepts

32 Relativistic Hydrodynamics (I) The energy-momentum tensor T µυ is the four-momentum component in the µ direction per three-dimensional surface area perpendicular to the ν direction. p =( E, p x, p y, p z ) x =( t, x, y, z) µ = =0: T 00 R = µ = =1: T 11 R = E x y z = E V = " p x t y z force in x direction acting on an surface Δy Δz perpendicular to the force pressure T µ = energy density energy flux density momentum density momentum flux density " ~j " ~g 31/66

33 Relativistic Hydrodynamics (II) Isotropy in the fluid rest implies that the energy flux T 0j and the momentum density T j0 vanish and that Π ij = P δ ij T µ R = 0 1 " B0 P P 0 A P Off-diagonal elements 0 in case of viscous hydrodynamics, not considered here à ideal (perfect) fluid. See also Ollitrault, arxiv: /66

34 Relativistic Hydrodynamics (III) Energy-momentum tensor (in case of local thermalization) after Lorentz transformationto the lab frame: T µ =(" + P ) u µ u Pg µ Energy density 4-velocity: and pressure in the co-moving system u µ =dx µ /d = (1,~v) metric tensor diag(1,-1,-1,-1) Energy and momentum µ T µ =0, ~ r) in " + ~ r~j " = 0 g i + r j ij = 0 (momentum conservation) Conserved quantities, e.g., baryon number: j µ B (x) =n B(x) u µ µ j µ B N B + ~ r(n B ~v )=0 continuity equation N B = n B 33/66

35 Ingredients of Hydro - models Equation of motion and baryon number µ T µ µ j µ B (x) =0 5 equations for 6 unknowns: (u x,u y,u z,",p,n B ) Equation of state: P (", n B ) (needed to close the system) Initial conditions, e.g., from Glauber calculation Freeze-out condition EOS I: ultra-relativistic gas P = ε/3 EOS H: resonance gas, P 0.15 ε EOS Q: phase transition, QGP resonance gas 34/66

36 LHC: Identified particle spectra Initial conditions fixed by pion abundance Protons overestimated Annihilation of protons and anti-protons in the hadron phase? 35/66

37 Elliptic flow in Hydro - models Elliptic flow is selfquenching :The cause of elliptic flow, the initial spacial anisotropy, decreases as the momentum anisotropy increases 36/66

38 Anisotropy in momentum space Anisotropy in coordinate space Anisotropy in momentum space Ulrich Heinz, Peter Kolb, arxiv:nucl-th/ In hydrodynamic models the momentum anisotropy develops in the early (QGP)phase of the collision. Thermalization times of less then 1 fm/c are neededto describe the data. 37/66

39 Cold atomic gases Li-6 atoms in an highly anisotropic trap (aspect ratio 29:1) Very strong interactions between atoms (Feshbach resonance) Once the atoms are released the one observed a flow pattern similar to elliptic flow in heavyion collisions 38/66

40 Lesson III First results from ALICE at LHC show large increase in energy density (factor 2-3 compared to RHIC) longer life-time of qgp larger collective flow effects anisotropic flow comparable to ultra-low viscosity triangular flow sensitive to initial energy density fluctuations and viscosity/entropy ratio Hydrodynamical model provides framework to characeterize QGP, i.e. equation of state, viscosity/entropy ratio