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THE FUTURE of RELATIVISTIC HEAVY ION COLLISIONS Workshop on “Future of Nuclear Collisions at High Energy”, Kielce, October 14-17, 2004

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THE FUTURE of RELATIVISTIC HEAVY ION COLLISIONS Workshop on “Future of Nuclear Collisions at High Energy”, Kielce, October 14-17, 2004 THE FUTURE OF RELATIVISTIC HEAVY ION COLLISIONS Workshop on \Future of Nuclear Collisions at High Energy", Kielce, October 14-17, 2004 This is not a workshop summary. I describe major accomplishments (some not yet mentioned) and o®er implied and/or explicit challenges. +50% of content is for STUDENTS who ARE actually THE FUTURE of relativistic heavy ion nuclear collisions. [ I] Why and How: decon¯nement [ II] Where and what we do p6 [III] Flavor QGP Signatures p11 [IV] Particle production Resonances p16 [V] Onset of decon¯nement QGP p24 [VI] Flavor at LHC p28 Supported by a grant from the U.S. Department of Energy, DE-FG02-04ER41318 Johann Rafelski Department of Physics University of Arizona TUCSON, AZ, USA 1 J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 2 The origin of this research program to move on with other issues in fundamental understanding of the world around us, we need to make this `next step' STRUCTURED VACUUM: Melt the vacuum structure and demonstrate mobility of quarks { `decon¯nement'. This demonstrates that the vacuum is a key component in the understanding of what we observe in terms of the fundamental laws of nature. This leads to understanding of the origin of 99% of the rest mass present in the Universe { The Higgs mechanism covers the remaining 1% (or less). EARLY UNIVERSE: Recreate and understand the high energy density conditions pre- vailing in the Universe when nucleons formed from elementary de- grees of freedom (quarks, gluons) at about 10-40¹s after big bang. Hadronization of the Universe led to nearly matter-antimatter sym- metric state, the sequel annihilation left the small 10¡10 matter asymmetry, the world around us. J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 3 What is decon¯nement? A domain of (space, time) much larger than normal hadron size in which color-charged quarks and gluons are propagating, con- strained by external `frozen vacuum' which abhors color. We expect a pronounced boundary in temperature and density be- tween con¯ned and decon¯ned phases of matter: phase diagram. Decon¯nement expected at both: high temperature and at high matter density. In a ¯nite size system not a singular boundary, a `transformation'. THEORY FUTURE What we need as background knowledge: 1) Hot QCD in/out of equilibrium (QGP from QCD-lattice) 2) Understanding from ¯rst principles and not as descriptive method of hadronization dynamics and ¯nal hadron yields, 3) More sensitive (hadronic and other) signatures of decon¯nement beware: ¯nal particles always hadrons, many decay into leptons DECONFINEMENT NOT A `NEW PARTICLE', there is no answer to journalists question: How many new vacuua have you produced today? J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 4 Vacuum structure Quantum vacuum is polarizable: see atomic vac. pol. level shifts Quantum structure of gluon-quark fluctuations: glue and quark condensate evidence from LGT, 'onium sum rules Permanent fluctuations/structure in `space devoid of matter': a 2 a ¹º ~ 2 ~ 2 even though hV jG¹ºjV i = 0; with G ´ G¹ºGa = 2 [Ba ¡ Ea ] ; a a ® X X we have hV j sG2jV i ' (2:3 § 0:3)10¡2GeV4 = [390(12) MeV]4 ; ¼ and hV juu¹ + dd¹ jV i = ¡2[225(9) MeV]3 : Vacuum and Laws of Physics Vacuum structure controls early Universe properties Vacuum determines inertial mass of `elementary' particles by the way of the Higgs mechanism, mi = gihV jhjV i ; Vacuum is thought to generate color charge con¯nement: hadron mass originates in QCD vacuum structure. Vacuum determines interactions, symmetry breaking, etc..... DO WE REALLY UNDERSTAND HOW THE VACUUM CON- TROLS INERTIA (RESISTANCE TO CHANGE IN VELOCITY)?? J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 5 Do we really understand how annihilation of almost all matter-antimatter occurs? 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 The future of RHI Collisions Kielce, October 17, 2004, page 6 EXPERIMENTAL HEAVY ION PROGRAM | LHC AT CERN: LHC opens after 2007 and SPS resumes after 2009 J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 7 ...and at BROOKHAVEN NATIONAL LABORATORY Relativistic Heavy Ion Collider: RHIC J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 8 BROOKHAVEN NATIONAL LABORATORY 12:00 o’clock PHOBOS BRAHMS 10:00 o’clock 2:00 o’clock RHIC PHENIX 8:00 o’clock STAR 4:00 o’clock 6:00 o’clock Design Parameters: Beam Energy = 100 GeV/u U-line 9 GeV/u No. Bunches = 57 High Int. Proton Source BAF (NASA) µ g-2 9 Q = +79 No. Ions /Bunch = 1×10 LI NAC T = 10 hours BOOSTER store L = 2 × 1026 cm-2 sec -1 Pol. Proton Source ave AGS HEP/NP 1 MeV/u Q = +32 TANDEMS Relativistic Heavy Ion Collider: RHIC J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 9 CERN SPS: THE FIRST LOOK AT DECONFINED UNIVERSE IN THE 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 Peter Seyboth, NA35 1986: S{Ag at 200AGeV 12 TEMPERATURE T0; Tf 300{250, 175{145 MeV; 300MeV'3.5 10 K J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 10 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 The future of RHI Collisions Kielce, October 17, 2004, page 11 Tasks for hadronic/flavor QGP signatures 1. New directions: LHC Flavor signatures = Signatures of flavor * Mixed charm-bottom states Bc(bc¹) etc. will be made extremely abundantly (comparing to pp) in the quark soup at LHC, this opens up precision laboratory of atomic QCD * Charm and bottom yield at LHC: in depth tests of small-x structure functions 2. Search for onset of decon¯nement as function of energy and of system size Marek Ga¶zdzicki with NA49 3. Resonances, statistical hadronization, bulk matter dynamics, critical (phase boundary) chemical nonequilibrium Furthermore: recall 1) J=ª suppression turns into enhancement as soon as `enough' charm pairs per reaction available. 2) Hard parton jets: is it absorption of decay products, or energy stopping or both; relation to QGP physics? 3) Dileptons and photons are predominantly produced in ¯nal state meson decays J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 12 TWO STEP HADRON FORMATION MECHANISM IN QGP Ω 1. GG ! ss¹ GG ! cc¹ u s s s u u g s reaction gluon dominated u d d d s s s s 2. hadronization of pre-formed d g d g s g u g u s; s;¹ c; c¹ quarks u s g s s d u u Formation of complex rarely d g s d d produced (multi)exotic flavor d s g g u (anti)particles from QGP enabled s s u d by coalescence between s; s;¹ c; c¹ d g u quarks made in di®erent microscopic s s u reactions; this is signature of quark Ξ mobility and independent action, thus of decon¯nement. Enhance- ment of flavored (strange, charm) antibaryons progressing with `exotic' flavor content. AVAILABLE RESULT (SPS, RHIC): Enhancement of strange (anti)baryons progresses with strangeness content. J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 13 (MULTI)STRANGE (ANTI)HYPERON ENHANCEMENT WA97: central 158 A GeV Pb - Pb 10 Enhancement 1 - 0 ± ± ± h KS Λ Ξ Λ Ξ Ω+Ω 0 1 2 1 2 3 Strangeness Enhancement GROWTH with strangeness antiquark content. Enhancement is here de¯ned with respect to the yield in p{Be col- lisions, scaled up with the number of collision `wounded' nucleons. 0 1 2 3 4 5 6 J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 14 ENHANCEMENT AS FUNCTION OF REACTION VOLUME > < > < pT 0, |y-ycm| 0.5 NA57 158 A GeV pT 0, |y-ycm| 0.5 NA57 158 A GeV Ω-+Ω+ 10 10 Ξ- Ξ+ Λ Λ Particle / event / wound. nucl. relative to pBe Particle / event / wound. nucl. relative to pBe Particle 1 1 pBe pPb PbPb pBe pPb PbPb 2 3 2 3 1 10 10 10 1 10 10 10 < > < > Nwound Nwound Note the gradual onset of enhancement with reaction volume. \Canonical enhancement" (a hadronic equilibrium model) is grossly inconsistent with these results. Gradual enhancement shown pre- dicted by kinetic strangeness production. J. Rafelski, Arizona The future of RHI Collisions Kielce, October 17, 2004, page 15 ENHANCEMENT at low SPS Energy > < > < pT 0, |y-ycm| 0.5 NA57 40A GeV pT 0, |y-ycm| 0.5 NA57 40A GeV Ξ- 10 10 Ξ+ Λ Λ Particle / event / wound.
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