Axel Maas. 6 th of January 2005 RHI Seminar WS 2004/2005
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1 QCD Phase Transition(s) & The Early Universe Axel Maas 6 th of January 2005 RHI Seminar WS 2004/2005
2 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe - Summary Overview Aspects of QCD QCD at finite temperature Theoretical ideas Experimental investigations Unsettled issues QCD phase transition in the early universe Summary
3 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe - Summary Part I: Aspects of QCD
4 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe - Summary Quantumchromodynamics (QCD) (Quantized) Theory of strong interactions Describes the structure of hadrons and (ultimately) nuclei Elementary degrees of freedom are quarks and gluons Carry new charge: Color charge Quarks come in red, green, blue, and anticolors
5 Overview QCD: Degrees of Freedom Finite Temperature QCD Unsettled Issues Early Universe - Summary QCD degrees of freedom I DOF # Mass Bound state mass Spin El.charge Up quark MeV 300 MeV ½ 2/3 Down quark MeV 300 MeV ½ -1/3 Strange quark MeV450 MeV ½ -1/3 Charm quark MeV 1800 MeV ½ 2/3 Bottom quark MeV 4800 MeV ½ -1/3 Top quark MeVNo bound states ½ 2/3 Gluon 8 0 MeV Not applicable 1 0
6 Overview QCD: Degrees of Freedom Finite Temperature QCD Unsettled Issues Early Universe - Summary QCD degrees of freedom I DOF # Mass Bound state mass Spin El.charge Up quark MeV 300 MeV ½ 2/3 Down quark MeV 300 MeV ½ -1/3 Strange quark MeV450 MeV ½ -1/3 Charm quark MeV 1800 MeV ½ 2/3 Bottom quark MeV 4800 MeV ½ -1/3 Top quark MeVNo bound states ½ 2/3 Gluon 8 0 MeV Not applicable 1 0 Quark species ( flavor ) conserved in strong and electromagnetic but not in weak interactions Existence of quarks and gluons experimentally established Quarks in ep-scattering and gluons by event topologies
7 Overview QCD: Degrees of Freedom Finite Temperature QCD Unsettled Issues Early Universe - Summary QCD degrees of freedom II Baryon: 3 (valence-)quarks
8 Overview QCD: Degrees of Freedom Finite Temperature QCD Unsettled Issues Early Universe - Summary QCD degrees of freedom II Baryon: 3 (valence-)quarks Meson: 1 quark and 1 antiquark
9 Overview QCD: Degrees of Freedom Finite Temperature QCD Unsettled Issues Early Universe - Summary QCD degrees of freedom II Baryon: 3 (valence-)quarks Meson: 1 quark and 1 antiquark Interactions mediated by gluons
10 Overview QCD: Degrees of Freedom Finite Temperature QCD Unsettled Issues Early Universe - Summary QCD degrees of freedom II Baryon: 3 (valence-)quarks Meson: 1 quark and 1 antiquark Interactions mediated by gluons Gluons are also charged Pure glue theory: Yang-Mills Theory
11 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD Weakly interacting at high energies (> a few GeV) Asymptotic freedom Accessible by perturbation theory
12 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD Weakly interacting at high energies (> a few GeV) Asymptotic freedom Accessible by perturbation theory Strongly interacting at low energies Perturbation theory fails Genuine non-perturbative effects Seem to be generated by gluon interaction
13 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD II Chiral symmetry Connection of left- and right-handed quarks Exact symmetry if quarks are massless (Weak) explicit breaking by quark masses
14 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD II Chiral symmetry Connection of left- and right-handed quarks Exact symmetry if quarks are massless (Weak) explicit breaking by quark masses Chiral symmetry spontaneously broken Nucleon mass of ~1 GeV although bare quark masses ~5-10 MeV Constituent or bound state quark masses larger by ~300 MeV
15 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD III Confinement Free quarks and gluons not observed In general: No colored objects observed Measured for quarks at 1: Unique signature due to fractal electric charge
16 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD III Confinement Free quarks and gluons not observed In general: No colored objects observed Measured for quarks at 1: Unique signature due to fractal electric charge Not yet understood ( millennium problem ) Recent progress Collective (topological) gluon excitations?
17 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD IV Inter-quark potential confining ( Cornell potential ): V=a/r+σr (σ string tension) [Figures from Sommer et al., 2001]
18 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Properties of QCD IV Inter-quark potential confining ( Cornell potential ): V=a/r+σr (σ string tension) Flattened by string breaking [Figures from Sommer et al., 2001 (left) and from Greensite, 2003 (right)]
19 Overview QCD: Properties Finite Temperature QCD Unsettled Issues Early Universe - Summary Chiral symmetry and confinement Connection between chiral symmetry and confinement Removal of confining properties removes also chiral symmetry breaking Seem to be linked by collective (topological) excitations Not understood But some progress in the last years
20 Overview QCD: Formulation Finite Temperature QCD Unsettled Issues Early Universe - Summary Formulation of QCD Gauge Theory with classical Lagrangian L= 1 4 F a F, a id m, : Quarks A a F a = A a A a gf abc A b A c D = iea a a : Gluons Upon quantization commonly auxiliary fields to described quantum fluctuations ( Ghosts ) are introduced
21 Overview QCD: Theoretical Methods Finite Temperature QCD Unsettled Issues Early Universe - Summary Theoretical Methods Lattice gauge theory Massive numerical calculations
22 Overview QCD: Theoretical Methods Finite Temperature QCD Unsettled Issues Early Universe - Summary Theoretical Methods Lattice gauge theory Massive numerical calculations Functional methods Equations of motions, renormalization group
23 Overview QCD: Theoretical Methods Finite Temperature QCD Unsettled Issues Early Universe - Summary Theoretical Methods Lattice gauge theory Massive numerical calculations Functional methods Equations of motions, renormalization group Effective theories Systematic expansion, e.g. Chiral perturbation theory Ad hoc models
24 Overview QCD: Theoretical Methods Finite Temperature QCD Unsettled Issues Early Universe - Summary Theoretical Methods Lattice gauge theory Massive numerical calculations Functional methods Equations of motions, renormalization group Effective theories Systematic expansion, e.g. Chiral perturbation theory Ad hoc models Many other methods and attempts
25 Overview QCD: Theoretical Methods Finite Temperature QCD Unsettled Issues Early Universe - Summary Theoretical Methods Lattice gauge theory Massive numerical calculations Functional methods Equations of motions, renormalization group Effective theories Systematic expansion, e.g. Chiral perturbation theory Ad hoc models Many other methods and attempts No method yet successful alone combinations needed
26 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe - Summary Part II: Finite Temperature
27 Overview QCD Finite Temperature QCD: Introduction Unsettled Issues Early Universe - Summary Finite Temperature QCD I Can the properties of QCD change?
28 Overview QCD Finite Temperature QCD: Introduction Unsettled Issues Early Universe - Summary Finite Temperature QCD I Can the properties of QCD change? Old Idea: QCD weakly coupled at high temperature Perturbation theory Chiral restoration and deconfinement
29 Overview QCD Finite Temperature QCD: Introduction Unsettled Issues Early Universe - Summary Finite Temperature QCD I Can the properties of QCD change? Old Idea: QCD weakly coupled at high temperature Perturbation theory Chiral restoration and deconfinement Phase diagram of QCD Phase transition at high temperature and densities
30 Overview QCD Finite Temperature QCD: Introduction Unsettled Issues Early Universe - Summary Finite Temperature QCD I Can the properties of QCD change? [Figure from Karsch et al., 2003] Old Idea: QCD weakly coupled at high temperature Perturbation theory Chiral restoration and deconfinement Phase diagram of QCD Phase transition at high temperature and densities
31 Overview QCD Finite Temperature QCD: Introduction Unsettled Issues Early Universe - Summary Finite Temperature QCD II Relevant for the early universe and neutron-stars (?)
32 Overview QCD Finite Temperature QCD: Introduction Unsettled Issues Early Universe - Summary Finite Temperature QCD II [Figure from Andronic et al., 2004] Relevant for the early universe and neutron-stars (?) Experimentally investigated in heavy-ion collisons
33 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Temperature from Experiment Temperature and chemical potential cannot be measure directly
34 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Temperature from Experiment Temperature and chemical potential cannot be measure directly Indirect extraction from a fit of the hadron production ratios Idealized model of a free hadron gas
35 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Research centers for Heavy-Ion physics [Earth picture from NASA]
36 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Research centers for Heavy-Ion physics [Earth picture from NASA, research center picture from the homepage]
37 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Research centers for Heavy-Ion physics [Earth picture from NASA, research center pictures from their respective homepages]
38 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Research centers for Heavy-Ion physics [Earth picture from NASA, research center pictures from their respective homepages]
39 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experiments [From CERN press release]
40 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experiments SIS: ~1 GeV/A (Kaos, Fopi, Hades) Ongoing [From CERN press release]
41 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experiments AGS: 5 GeV/A (E802/864,E917, E810,E814/877, E864,E895) Completed SIS: ~1 GeV/A (Kaos, Fopi, Hades) Ongoing [From CERN press release]
42 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experiments AGS: 5 GeV/A (E802/864,E917, E810,E814/877, E864,E895) Completed SPS: <17 GeV/A (WA80/98, NA35/49, NA 38/50/60, NA 44, CERES, WA97, NA57, NA52) Nearly completed SIS: ~1 GeV/A (Kaos, Fopi, Hades) Ongoing [From CERN press release]
43 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experiments AGS: 5 GeV/A (E802/864,E917, E810,E814/877, E864,E895) Completed RHIC: 200/130 GeV/A (Star, Phenix, Brahms, Phobos) Ongoing SPS: <17 GeV/A (WA80/98, NA35/49, NA 38/50/60, NA 44, CERES, WA97, NA57, NA52) Nearly completed SIS: ~1 GeV/A (Kaos, Fopi, Hades) Ongoing [From CERN press release]
44 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experiments LHC: 2700 GeV/A (Alice, CMS, Atlas) Under construction AGS: 5 GeV/A (E802/864,E917, E810,E814/877, E864,E895) Completed RHIC: 200/130 GeV/A (Star, Phenix, Brahms, Phobos) Ongoing SPS: <17 GeV/A (WA80/98, NA35/49, NA 38/50/60, NA 44, CERES, WA97, NA57, NA52) Nearly completed SIS: ~1 GeV/A (Kaos, Fopi, Hades) Ongoing [From CERN press release]
45 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experiments LHC: 2700 GeV/A (Alice, CMS, Atlas) Under construction AGS: 5 GeV/A (E802/864,E917, E810,E814/877, E864,E895) Completed RHIC: 200/130 GeV/A (Star, Phenix, Brahms, Phobos) Ongoing FAIR: High density (CMB) Under construction SPS: <17 GeV/A (WA80/98, NA35/49, NA 38/50/60, NA 44, CERES, WA97, NA57, NA52) Nearly completed SIS: ~1 GeV/A (Kaos, Fopi, Hades) Ongoing [From CERN press release]
46 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Hevay-Ion Experiments I NA45/CERES, fixed CERN SPS Second generation, special purpose detector [From the CERES homepage]
47 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Heavy-Ion Experiments II ALICE, CERN LHC Fourth generation, omnipurpose detector [From the ALICE homepage]
48 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experimental signatures... Many observables available
49 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experimental signatures... Many observables available Hard probes Perturbative QCD applicable, e.g. Jet quenching
50 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experimental signatures... Many observables available Hard probes Perturbative QCD applicable, e.g. Jet quenching Hadronic probes Strangness or charm enhancement/suppression
51 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experimental signatures... Many observables available Hard probes Perturbative QCD applicable, e.g. Jet quenching Hadronic probes Strangness or charm enhancement/suppression Leptonic probes Dilepton or (direct) photon spectra enhancement
52 Overview QCD Finite Temperature QCD: Experiment Unsettled Issues Early Universe - Summary Experimental signatures... Many observables available Hard probes Perturbative QCD applicable, e.g. Jet quenching Hadronic probes Strangness or charm enhancement/suppression Leptonic probes Dilepton or (direct) photon spectra enhancement Many other observables HBT interferometry, hadron yields, event-by-event fluctuations of observables,...
53 Overview QCD Finite Temperature QCD: Experiement Unsettled Issues Early Universe - Summary Jet quenching Jets are a collimated spray of hadrons Originated from a (hard) production of two colored objects
54 Overview QCD Finite Temperature QCD: Experiement Unsettled Issues Early Universe - Summary Jet quenching Jets are a collimated spray of hadrons Originated from a (hard) production of two colored objects One can be stooped by the medium [From the STAR collaboration, 2002]
55 Overview QCD Finite Temperature QCD: Theory Unsettled Issues Early Universe - Summary...and theoretical problems Euqilibrium properties of the quark-gluon plasma Bound state physics of hadrons Hadron formation in a medium Phase transition: Non-equilibrium Heavy-Ion collision: Finite size etc. Propagation of probes in a heavy-ion collision
56 Overview QCD Finite Temperature QCD: Chiral transition Unsettled Issues Early Universe - Summary Finite Temperature on the Lattice I Numerical calculation in a finite volume Thermodynamic limit reached by extrapolation Phase transition deduced from peaks in susceptibilities
57 Overview QCD Finite Temperature QCD: Chiral transition Unsettled Issues Early Universe - Summary Finite Temperature on the Lattice I Numerical calculation in a finite volume Thermodynamic limit reached by extrapolation Phase transition deduced from peaks in susceptibilities Main observables are the chiral condensate and thermodynamic quantities Energy density, pressure, entropy,... Calculated directly from the partition sum [Figure from Karsch, 2001]
58 Overview QCD Finite Temperature QCD: Chiral transition Unsettled Issues Early Universe - Summary Finite Temperature on the Lattice II First order phase transition or crossover Yang-Mills Theory: First order at 269 MeV Approaches Stefan-Boltzmann limit slowly Strong residual interactions at least up to several times T c [Figure from Karsch et al., 2003]
59 Overview QCD Finite Temperature QCD: Order of the phase transition Unsettled Issues Early Universe - Summary Order of the phase transition Order of the phase transition depends on the quark masses Currently not possible to calculate at physical quark masses [Figure from Karsch et al., 2003]
60 Overview QCD Finite Temperature QCD: Hadrons Unsettled Issues Early Universe - Summary The fate of hadrons Hadrons broaden [Figure from Karsch et al., 2003] Observable in spectral function Dissolving? Consequences on (production) cross-sections Experimental consequences (?)
61 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe - Summary Part III: Unsettled issues Deconfinement The non-triviality of the high-temperature phase
62 Overview QCD Finite Temperature QCD Unsettled Issues: Deconfinement Early Universe - Summary Deconfinement I [From Karsch et al., 2003] String tension vanishes at phase transition Not observable in full QCD
63 Overview QCD Finite Temperature QCD Unsettled Issues: Deconfinement Early Universe - Summary Deconfinement II Polyakov line order [From Karsch, 2001] parameter in pure glue Well defined? Not well defined with quarks Used anyway Same transition temperature as for chiral transition Not understood as in the vacuum
64 Overview QCD Finite Temperature QCD Unsettled Issues: Trace anomaly Early Universe - Summary Trace anomaly θ=ε-3p=0 for a Stefan-Boltzmann gas Significantly different from 0 at phase transition and beyond [Left: From Karsch et al. 2000, Right: From Karsch 2001]
65 Overview QCD Finite Temperature QCD Unsettled Issues: Trace anomaly Early Universe - Summary Origin of the Trace Anomaly [Following Zwanziger, 2004] Only one independent thermodynamic quantity p= T V ln Z =T 2 T p T = 3 p=t 5 T p T 4
66 Overview QCD Finite Temperature QCD Unsettled Issues: Trace anomaly Early Universe - Summary Origin of the Trace Anomaly [Following Zwanziger, 2004] Only one independent thermodynamic quantity p= T V ln Z =T 2 T Re-express everything by trace anomaly p T = 3 p=t 5 T p T 4 p dt T 4 =c SB T T 5 1 dt T 4 =3c SB T T 3 T T
67 Overview QCD Finite Temperature QCD Unsettled Issues: Trace anomaly Early Universe - Summary Origin of the Trace Anomaly [Following Zwanziger, 2004] Only one independent thermodynamic quantity p= T V ln Z =T 2 T Re-express everything by trace anomaly p T = 3 p=t 5 T p T 4 p dt T 4 =c SB T T 5 1 dt T 4 =3c SB T T 3 T T Only a term linear in T can contribute to p but not to ε
68 Overview QCD Finite Temperature QCD Unsettled Issues: Trace anomaly Early Universe - Summary Origin of the Trace Anomaly [Following Zwanziger, 2004] Only one independent thermodynamic quantity p= T V ln Z =T 2 T Re-express everything by trace anomaly p T = 3 p=t 5 T p T 4 p dt T 4 =c SB T T 5 1 dt T 4 =3c SB T T 3 T T Only a term linear in T can contribute to p but not to ε Perturbation theory cannot provide such a term
69 Overview QCD Finite Temperature QCD Unsettled Issues: Failure of perturbation theory Early Universe - Summary Non-trivial High-Temperature Phase Perturbation theory fails Infrared divergences Similar to the vacuum Most problems for chromomagnetic sector Also spatial string tension cannot be explained by perturbation theory [Figure from Rischke, Prog.Part.Nucl. 2004] High temperature phase cannot be perturbative Likely not even at infinite temperature
70 Overview QCD Finite Temperature QCD Unsettled Issues: Picture Early Universe - Summary Picture of the high-temperature phase How does the high-temperature phase look?
71 Overview QCD Finite Temperature QCD Unsettled Issues: Picture Early Universe - Summary Picture of the high-temperature phase How does the high-temperature phase look?
72 Overview QCD Finite Temperature QCD Unsettled Issues: Picture Early Universe - Summary Picture of the high-temperature phase How does the high-temperature phase look?
73 Overview QCD Finite Temperature QCD Unsettled Issues: Picture Early Universe - Summary Picture of the high-temperature phase How does the high-temperature phase look?
74 Overview QCD Finite Temperature QCD Unsettled Issues: Picture Early Universe - Summary Picture of the high-temperature phase How does the high-temperature phase look?
75 Overview QCD Finite Temperature QCD Unsettled Issues: Picture Early Universe - Summary Picture of the high-temperature phase How does the high-temperature phase look? Strongly interacting ( ionic ) liquid with delocalized quarks and gluons
76 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe - Summary Part IV: The Early Universe - t=+6µs
77 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Phase transition - Summary Physical situation Unclear if a phase transition
78 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Phase transition - Summary Physical situation Unclear if a phase transition Even if not a drastic change occurs Large jump in energy
79 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Phase transition - Summary Physical situation Unclear if a phase transition Even if not a drastic change occurs Large jump in energy Practical very similar effects Assume a 1st order transition
80 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Inflation- Summary QCD inflation Chiral symmetry restoration similar to inflation transition Allows in principle for an inflationary era with reheating
81 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Inflation- Summary QCD inflation Chiral symmetry restoration similar to inflation transition Allows in principle for an inflationary era with reheating QCD phase transition not strong enough to give a measurable effect too small surface tension ( ?) [Figure from Kämpfer, 2000]
82 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Inflation- Summary QCD inflation Chiral symmetry restoration similar to inflation transition Allows in principle for an inflationary era with reheating QCD phase transition not strong enough to give a measurable effect too small surface tension ( ?) [Figure from Kapusta, 2001]
83 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Nucleosynthesis- Summary Impact on Nucleosynthesis I Baryon-to-photon ratio is influenced by QCD phase transition Quarks electrically charged Baryon distribution can also be influenced Baryon density in the high-temperature phase higher Light quarks vs. heavy baryons 1st order phase transition leads to bubble formation
84 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Nucleosynthesis - Summary Impact on Nucleosynthesis II Baryon number conservation requires highest baryon density in the last bubbles to freeze: High nucleon density Neutrons diffuse faster due to electric neutrality: Isopsin inhomogeneities Spatial inhomogeneities in nucleosynthesis
85 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Nucleosynthesis - Summary Impact on Nucleosynthesis II Baryon number conservation requires highest baryon density in the last bubbles to freeze: High nucleon density Neutrons diffuse faster due to electric neutrality: Isopsin inhomogeneities Spatial inhomogeneities in nucleosynthesis Effect starts at ~150 m initial average bubble separation Likely only ~0.01 m [Figure from Kainulainen, 1999]
86 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Exotics - Summary Exotic Consequences Much stronger nucleations: Primordial black hole formation Hawking flashes, gravitational micro-lensing, dark matter candidate
87 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Exotics - Summary Exotic Consequences Much stronger nucleations: Primordial black hole formation Hawking flashes, gravitational micro-lensing, dark matter candidate Strangelets: Nuggets of strange matter Unlikely as strange matter is likely not stable
88 Overview QCD Finite Temperature QCD Unsettled Issues Early Universe: Exotics - Summary Exotic Consequences Much stronger nucleations: Primordial black hole formation Hawking flashes, gravitational micro-lensing, dark matter candidate Strangelets: Nuggets of strange matter Unlikely as strange matter is likely not stable Large scale chromomagnetic walls Similar to cosmic walls Would be observable in CMB for l>1000
89 Introduction QCD Vacuum Results QCD Phase Diagram Finite Temperature Results Summary Summary QCD describes strong interactions
90 Introduction QCD Vacuum Results QCD Phase Diagram Finite Temperature Results Summary Summary QCD describes strong interactions Non-perturbative theory non-perturbative effects Chiral symmetry breaking and confinement
91 Introduction QCD Vacuum Results QCD Phase Diagram Finite Temperature Results Summary Summary QCD describes strong interactions Non-perturbative theory non-perturbative effects Chiral symmetry breaking and confinement Undergoes a phase change at high temperatures Details are yet unclear
92 Introduction QCD Vacuum Results QCD Phase Diagram Finite Temperature Results Summary Summary QCD describes strong interactions Non-perturbative theory non-perturbative effects Chiral symmetry breaking and confinement Undergoes a phase change at high temperatures Details are yet unclear Can in principle have significant impact on the evolution of the early universe QCD parameters lead only to a weak effect Strong and cosmological scales have already been to different
93 Introduction QCD Vacuum Results QCD Phase Diagram Finite Temperature Results Summary Summary QCD describes strong interactions Non-perturbative theory non-perturbative effects Chiral symmetry breaking and confinement Undergoes a phase change at high temperatures Details are yet unclear Can in principle have significant impact on the evolution of the early universe QCD parameters lead only to a weak effect Strong and cosmological scales have already been to different QCD directly not relevant but indirectly: Nucleosynthesis
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