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Hadronization of the Quark Universe CINPP, Kolkata, 6 February 2005 Hadronization of the Quark Universe CINPP, Kolkata, 6 February 2005 [ I] Probing the Universe with Heavy Ions [ II] Recreating the early Universe in the laboratory Energy to matter: the (al)chemy of particle production: Use as a diagnostic tool of QGP formation [III] Hadronization of the Quark Universe ( i) Scale of Universe hadronization time ( ii) Formation of (visible) matter (iii) Chemical potentials in the early Universe (iv) Baryon to photon ratio, mixed phase (v) Particle populations in the early Universe [IV] Inhomogeneous Matter-Antimatter Universe? ( i) Distillation process (ii) Mass (a)symmetry? Mike Fromerth & Johann Rafelski [ V] Final Remarks University of Arizona and CERN 1 J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 2 Stages in the evolution of the Universe Visible Matter Density [g cm−3 ] 1027 1015 103 10−9 1 TeV LHC 1016 quarks combine RHIC atoms antimatter form disappears 1 GeV photons 1013 neutrinos decouple SPS decouple nuclear reactions: light nuclei formed 1 MeV era of 1010 galaxies and stars 7 Particle energy 1 keV 10 Temperature [K] OBSERVATIONAL COSMOLOGY 1 eV 104 PARTICLE/NUCLEAR ASTROPHYSICS 10 10−12 10−6 1 106 1012 1018 day year ky My today Time [s] J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 3 The study of hadronic particle production in relativistic heavy ion collision experiments at SPS, RHIC, LHC provides the knowledge required to develop the understanding of the physics of the Uni- verse at the time period THE VISIBLE MATTER AS WE KNOW IT HAS BEEN FORMED In the process ² we discover a new state of matter, the QUARK-GLUON PLASMA. ² We learn about mechanisms how energy turns into particles WHEN MATTER, ANTIMATTER AND MESON are formed ² we learn about the period of STRANGENESS AND ANTIMAT- TER DISAPPEARANCE. Little is known today about this rel- atively long lasting phase of the Universe evolution in which the Universe cools down by two orders of magnitude. J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 4 II RECREATING THE EARLY UNIVERSE IN LABORATORY Micro-Bang 135 81 Pb QGP Pb Au Au 115 47 363 353 Big-Bang Micro-Bang τ −∼ 10 µ s τ −∼ 4 10-23 s ∼ -10 ∼ NB / N − 10 NB / N − 0.1 Order of Magnitude ENERGY density ² ' 1{5GeV/fm3 = 1:8{9 1015g/cc Latent vacuum heat B ' 0:1{0.4GeV/fm3 ' (166{234MeV)4 1 30 PRESSURE P = 3² = 0:52 10 barn S{Ag Reaction at 200AGeV (by NA35) 12 TEMPERATURE T0; Tf 300{250, 175{145 MeV; 300MeV'3.5 10 K J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 5 THE EARLY UNIVERSE AT RHIC STAR . and BRAHMS, PHOBOS: How is this maze of tracks of newly produced particles telling us what we want to know about the early Universe and its properties? Study of patterns in particle production: correlations, new flavors (strangeness, charm), resonances, etc.. J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 6 (Al)chemy of particle production Ω u s s s u u g u s d d d s s s s d g d g s g u g u u s g u s s d u d s d d g d s g g u s u d s d g u s s u Ξ Hadron formation from a drop of decon¯ned matter which ¯lled the early Universe Expect creation of complex rarely seen (multi, strange, anti-) particles enabled by available populations of particles (strange quarks etc) made in independent microscopic reactions. J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 7 Strangeness: a popular laboratory QGP diagnostic tool EXPERIMENTAL REASONS ² There are many strange particles allowing to study di®erent physics questions (q = u; d): Á(ss¹); K(qs¹); K(q¹s); ¤(qqs); ¤(q¹q¹s¹); ¥(qss); ¥(q¹s¹s¹); ­(sss); ­(s¹s¹s¹) : : : resonances : : : ² Strange hadrons are subject to a self analyzing de- cay within a few cm from the point of production; π π Ξ Λ p ² Production rates hence statistical signi¯cance is high; J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 8 THEORETICAL CONSIDERATIONS ² production of strangeness in gluon fusion GG ! ss¹ strangeness linked to gluons from QGP; (a) g (b) s (c) s g s dominant processes: g GG ! ss¹ abundant strangeness g s g =evidence for gluons g s s q (d) s 10{15% of total rate: qq¹ ! ss¹ q s ² coincidence of scales: ms ' Tc ! ¿s ' ¿QGP ! strangeness a clock for QGP phase ² s¹ ' q¹! strange antibaryon enhancement at RHIC (anti)hyperon dominance of (anti)baryons. J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 9 III Hadronization of the Quark Universe What we know: Upon QGP hadronization in the early Universe there is as much matter as antimatter (to within 10¡9). This symmetry diminishes progressively during the annihilation period. Questions and Issues ² Chemical conditions in the early Universe (chemical potentials, equilibria) ² Mechanisms and conditions at hadronization (conflict of Gibbs conditions with superselection rules such as charge conserva- tion/neutrality) ² When do antinucleons, strangeness, pions disappear (chemical nonequilibrium in hadron phase)? ² How much antimatter remains in the homogeneous/non-homogeneous Universe? ² What happens to the Universe during matter-antimatter anni- hilation? Very Large Scale Structure formation? ² Influence on nucleosynthesis epoch? J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 10 Time scale in Universe hadronization The expanding Universe cools, the hot quark-gluon plasma freezes into individual hadrons. In laboratory we do this suddenly, in the early Universe slowly as seen on time scale of strong interactions. STRONG INTERACTIONS TIME CONSTANT: Nucleon size / light velocity' 10¡23s UNIVERSE HADRONIZATION TIME CONSTANT: 2 3c B0 GeV ¿U = = 36 ¹s ; B0 = 0:19 r32¼GB r B fm3 Naively, 4B is energy density inside particles like protons, and is the amount of energy required per unit of volume to decon¯ne quarks. J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 11 10{50 ¹s Hadronization Timescale in the Universe Universe has two components: luminous matter ²l and at this early time scale probably still a small `cold' dark matter ²d energy density component. The pressure is all due the luminous component: P = Pl. R ¡ 1 R Einstein Equations: ¹º 2g¹º = 8¼GT¹º comprise two dynamical equations for the size scale R(t) of the Robertson-Walker metric: dr ds2 = g¹ºdx dx = dt2 ¡ R2 + r2dθ2 + r2 sin2 θdÁ2 : ¹ º ·1 ¡ kr2 ¸ ¹º 1. Consider T ;º = 0, describing entropy conserving expansion: dV 3 dR 3dR d² dE + P dV = T dS = 0; dE = d(²V ); = ; = ¡ : V R R ² + P ' 0 3 NOTE: for ² = ²l + ²d and ²d ²d=R (cold dark matter) this reduces to exactly 3dR d²l = ¡ keep in mind Pd ¿ Pl: R ²l + P 2. We use the 0-0 component of Einstein equations R_ 2 k 8¼ + = G² R2 R2 3 In a flat (k = 0) Robertson-Walker Universe we ¯nd exactly: 2 2 ²_l = 24¼G (²l + ²d) (²l + P ) ; P = (²l ¡ 4B)=3 + Pd J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 12 10{50 ¹s Hadronization Timescale in the Universe When dark component is insigni¯cant: 2 ²l = B coth (t=¿U); and by matching at a given pressure we ¯nd the magnitude of the time the Uni- verse inflates through the mixed hadron phase. Pressure (upper) and temperature (lower part) in the Universe, as func- tion of time, in the vicinity of the phase transition from the decon¯ned phase to the con¯ned phase. Solid lines, B1=4 = 195 MeV; dotted lines, B1=4 = 170 MeV (lower part) and B1=4 = 220 MeV (upper part) all for ®s = 0:6 (reduces the active quark-gluon degrees of freedom). J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 13 Production of Matter of our Era Our objective is to understand the chemical conditions at the emergence of matter as we know it today in the early Universe period at hadronization of quark-gluon plasma. This establishes the initial particle densities which can be followed to the end of the hadron gas era. Quantitative Tasks 1) Identify the chemical conservation laws constraining potentials ¹(T ) and the pertinent conservation laws; 2) Trace out chemical potentials as function of temperature, which itself we can study separately as function of time (see above) { this separation is convenient given the lack of knowledge about dark matter; 3) Evaluate the chemical (particle) flavor composition of the Uni- verse during evolution toward the condition of neutrino decoupling at T ' 1 MeV t ' 10 s 4) Explore the quark-hadron phase transformation dynamics, and establish potential for conserved quantum (baryon, electrical charge) number distillation; J. Rafelski, Arizona and CERN Hadronization of the Quark Universe CINPP, Kolkata, 6 February, 2005, page 14 CHEMICAL POTENTIALS IN THE UNIVERSE The slow hadronization of the Universe implies chemical equilib- rium is reached for all hadronic reactions (phase space occupancy saturated), and there is full participation of electromagnetically interacting photon and lepton degrees of freedom. ² Photons in chemical equilibrium, assume the Planck distribu- tion, implying a zero photon chemical potential; i.e.: ¹γ = 0 ² Whenever chemical and thermal equilibrium is attained, reac- tions such as f + f¹ ­ 2γ are allowed, (here f and f¹ are a fermion { antifermion pair), hence: ¹f = ¡¹f¹ ² Minimization of the Gibbs free energy implies that for any re- action ºiAi = 0, where ºi are the reaction equation coe±cients of the chemical species Ai, chemical equilibrium arises for the condition: ºi¹i = 0 ² Example: weak interaction reactions lead to: ¹s = ¹d = ¹u + ¢¹l ¡ ¡ ¡ ´ ¹e ¹ºe = ¹¹ ¹º¹ = ¹¿ ¹º¿ ¢¹l J.
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