早期宇宙强相互作用物质演化 的非微扰 QCD 研究 刘玉鑫 （ Yuxin Li u ） 北京大学物理学院理论物理研究所 Department of Physics, Peking University, China 第十四届全国核结构大会，湖州师院， 2012 年 4 月 12 日 Outline I. Introduction Ⅱ. The Approach Ⅱ. The Approach Ⅲ. The Evolution in Phase Transition View Ⅲ. The Evolution in Phase Transition View Ⅳ. Possible Observables Ⅳ. Possible Observables V. Summary V. Summary

I. Introduction  Content of the Long Rang Plan of Nuclear Science in USA

 早期宇宙物质的组分及演化涉及的基本问题 不束缚的夸克、 胶子及电子等 夸克、 胶子 囚禁 强子 核 合 成 原 子 核 复 合 时 期 原 子 星系形成星系形成 现 在 宇宙现 在 宇宙 “ 已知 ” 明亮物质 ： 原子、分子 ( 强子 ) 物质 高度对称, m q = 0. m q > 0 ， 呈 6 味 3 代. 如何禁闭 ? 为何禁闭 ? 明亮物质 ~ 5%. > 95% ? ? 暗物质？ 暗能量？ 手征对称性硬破缺, Higgs 机制, Higgs 粒子 ？ 测量 LHC 信号 ？ M u,d >= 100m u,d, 如何产生 ？ 强作用非微扰效应 ！ ? 全 “ 新 ” 形态物质： QPG ? sQGP ?

 Fundamental Process: Phase Transitions Schematic QCD Phase Diagram Items Influencing the Phase Transitions: Medium ： Temperature T, Density (CheP.) Size Intrinsic ： Current mass, Coupling Strength, Color-Flavor Stru. Phase Transitions involved ： Deconfinement–confinement DCS – DCSB Flavor Sym. – FSB Chiral Symmetric Quark deconfined  SB SB, Quark confined sQGP Approaches: Expt. ： RHIC 、 Ast-Obs. Theor. ： Disc FT 、 ContFT, Compt. ： Theor., Simulation

Thin Pancakes Lorentz  =100 Nuclei pass thru each other < 1 fm/c Huge Stretch Transverse Expansion High Temperature (?!) The Last Epoch: Final Freezeout-- Large Volume We measure the “final” state, we are most interested in the “intermediate” state, we need to understand the “initial” state… Experimental Aspects ： （ 1 ） Relativistic Heavy Ion Collisions （ 2 ） Compact Star ObservationsObservations

 Theoretical Approaches ： Two kinds - Continuum & Discrete (lattice)  Lattice QCD ： Running coupling behavior ， Vacuum Structure ， Temperature effect ， “Small chemical potential” ；     Continuum ： (1) Phenomenological models (p)NJL 、 (p)QMC 、 QMF 、 (2) Field Theoretical Chiral perturbation, Renormalization Group, QCD sum rules, Instanton(liquid) model, DS equations, AdS/CFT, HD(T)LpQCD,    The approach should manifest simultaneously: (1) DCSB & its Restoration, (2) Confinement & Deconfinement.

Slavnov-Taylor Identity Dyson-Schwinger Equations axial gauges BBZ covariant gauges QCDQCD Ⅱ. The Dyson-Schwinger Equation Approach C. D. Roberts, et al, PPNP 33 (1994), 477; 45-S1, 1 (2000); EPJ-ST 140(2007), 53; R. Alkofer, et. al, Phys. Rep. 353, 281 (2001); C.S. Fischer, JPG 32(2006), R253; .

 Practical Algorithm at Present Stage  Quark equation at zero chemical potential where is the effective gluon propagator, can be conventionally decomposed as  Quark equation in medium  with

 Models of the Vertex (1) Bare Vertex (2) Ball-Chiu Vertex (3) Curtis-Pennington Vertex (Rainbow-Ladder Approx.) (4) BC+ACM Vertex (Chang, Liu, Roberts, PRL 106, (‘11) ) 满足 W-T 恒等式, 对纵向分量给出标准. 满足相乘性重整化 。

 Effective Gluon Propagators (3) Model (1) MN Model (2) (4) Realistic model Maris-Tandy Model (2) Point Interaction: (P) NJL Model Cuchieri, et al, PRD, 2008 A.C. Aguilar, et al., JHEP (3) Infrared Constant Model Qin, Chang, Liu, et al., PRC 84, (R), (‘11); 85, , (‘12). Taking in the coefficient of the above expres.

Dynamical chiral symmetry breaking (  SB) generates the mass of Fermion  SB 0 ~ - (240 MeV) 3 DSE approach meets the requirements! Dynamical Mass In DSE approach

parameters are taken from Phys. Rev. D 65, (1997), with fitted as  Effect of the Running Coupling Strength on the Chiral Phase Transition (W. Yuan, H. Chen, Y.X. Liu, Phys. Lett. B 637, 69 (2006)) Lattice QCD result PRD 72, (2005) (BC Vertex: L. Chang, Y.X. Liu, R.D. Roberts, et al., Phys. Rev. C 79, (2009)) Bare vertex CS phase CSB phase

 Part of the QCD Phase Diagram in terms of the Current Mass and Coupling Strength  The one with multi-node solutions is more complicated and more interesting. One Solution (ECSB) Three Solutions (ECSB + DCSB)

Slavnov-Taylor Identity Dyson-Schwinger Equations axial gauges BBZ covariant gauges QCDQCD  A comment on the DSE approach in QCD C. D. Roberts, et al, PPNP 33 (1994), 477; 45-S1, 1 (2000); EPJ-ST 140(2007), 53; R. Alkofer, et. al, Phys. Rep. 353, 281 (2001); C.S. Fischer, JPG 32(2006), R253; .

I II. The Evolution in Phase Transition View  Special Topic (1) : I II. The Evolution in Phase Transition View  Special Topic (1) : Critical EndPoint (CEP) The Position of CEP is a highly debated problem! What’s the criterion of PT when not knowing the ETP? Why different models give distinct results ?  (p)NJL model & others give quite large  E /T E (> 3.0) Sasaki, et al., PRD 77, (2008); Costa, et al., PRD 77, (2008); Fu & Liu, PRD 77, (2008); Ciminale, et al., PRD 77, (2008); Fukushima, PRD 77, (2008); Kashiwa, et al., PLB 662, 26 (2008); Abuki, et al., PRD 78, (2008); Schaefer, et al., PRD 79, (2009); Costa, et al., PRD 81, (2010);  Hatta, et al., PRD 67, (2003); Cavacs, et al., PRD 77, (2008);   Lattice QCD gives smaller  E /T E ( 0.4 ~ 1.1) Fodor, et al., JHEP 4, 050 (2004); Gavai, et al., PRD 71, (2005); Gupta, arXiv:~ [nucl-ex]; Li, et al., NPA 830, 633c (2009); Gupta & Xu, et al., Science 332, 1525 (2011);   RHIC Exp. Estimate hints quite small  E /T E (  1) R.A. Lacey, et al., nucl-ex/ ;   Simple DSE Calculations with Different Effective Gluon Propagators Generate Different Results (0.0, 1.3) Blaschke, et al, PLB 425, 232 (1998); He, et al., PRD 79, (2009);  

 Special topic (2): Coexistence region (Quarkyonic ? ) claim that there exists a quarkyonic phase. and General (large-N c ) Analysis McLerran, et al., NPA 796, 83 (‘07); NPA 808, 117 (‘08); NPA 824, 86 (‘09),   Lattice QCD Calculation de Forcrand, et al., Nucl. Phys. B Proc. Suppl. 153, 62 (2006) ;   Can sophisticated continuous field approach of QCD give the coexistence (quarkyonic) phase ?  What can we know more for the coexistence phase?  Inconsistent with Coleman-Witten Theorem !! quarkyonic

 Chiral susceptibility can be the criterion! Phase diagram is given, CEP is fixed. S.X. Qin, L. Chang, H. Chen, Y.X. Liu, et al, PRL 106, (‘11) S.X. Qin, L. Chang, H. Chen, Y.X. Liu, et al, PRL 106, (‘11) Phase diagram in bare vertexPhase diagram in BC vertex

Small σ  long range in coordinate space  Dif. of CEP come from dif. Confin. Length MN model  infinite range in r-space NJL model  “zero” range in r-space Longer range Int.  Smaller  E /T E S.X. Qin, L. Chang, H. Chen, Y.X. Liu, et al, PRL 106, (‘11) S.X. Qin, L. Chang, H. Chen, Y.X. Liu, et al, PRL 106, (‘11)

 Special Topic (3): Quark Matter at T above but near T c HTL Cal. (Pisarski, PRL 63, 1129(‘89); Blaizot, PTP S168, 330(’07)), Lattice QCD ( Karsch, et al., NPA 830, 223 (‘09); PRD 80, (’09) ) NJL (Wambach, et al., PRD 81, (2010)) & Simple DSE Cal. (Fischer et al., EPJC 70, 1037 (2010) ) show: there exists thermal & Plasmino excitations in hot QM. Other Lattice QCD Simulations ( Hamada, et al., Phys. Rev. D 81, (2010) ) claims: No No qualitative difference between the quark propagators in the deconfined and confined phases near the T c. RHIC experiments ( Gyulassy, et al., NPA 750, 30 (2005); Shuryak, PPNP 62, 48 (2009); Song, et al., JPG 36, (2009); … … ) indicate: the matter is in sQGP state.  What’s the nature of the matter in npQCD?

Solving quark’s DSE  Quark’s Propagator  Property of the matter above but near the T c Maximum Entropy Method ( Asakawa, et al., PPNP 46,459 (2001) ; Nickel, Ann. Phys. 322, 1949 (2007) )  Spectral Function In M-Space, only Yuan, Liu, etc, PRD 81, (2010). Usually in E-Space, Analytical continuation is required. Qin, Chang, Liu, et al., PRD 84, (2011)

T = 3.0T c Disperse Relation and Momentum Dependence of the Residues of the Quasi-particles’ poles T = 1.1T c S.X. Qin, L. Chang, Y.X. Liu, C.D. Roberts, PRD 84, (‘11) S.X. Qin, L. Chang, Y.X. Liu, C.D. Roberts, PRD 84, (‘11) Normal T. Mode Plasmino M. Zero Mode  The zero mode exists at low momentum (<7.0T c ), and is long-range correlation ( ~   1 > FP ).  The quark at the T where  S is restored involves still rich phases. And the matter is sQGP.

 Effect of the Chemical Potential on the Chiral Phase Transition Diquark channel: ( W. Yuan, H. Chen, Y.X. Liu, Phys. Lett. B 637, 69 (2006) ) Chiral channel: ( L. Chang, H. Chen, B. Wang, W. Yuan,Y.X. Liu, Phys. Lett. B 644, 315 ( L. Chang, H. Chen, B. Wang, W. Yuan, and Y.X. Liu, Phys. Lett. B 644, 315 (2007) ) Chiral Susceptibility of Wigner-Vacuum in DSE Some Refs. of DSE study on CSC 1. D. Nickel, et al., PRD 73, (2006); 2. D. Nickel, et al., PRD 74, (2006); 3. F. Marhauser, et al., PRD 75, (2007); D. Nickel, et al., PRD 77, (2008); …………

“QCD” Phase Transitions may Happen Ⅳ. Possible Observables General idea ， Phenom. Calc.,Calc. Sophist.Sophist. Calc.,Calc. quark may get deconfined (QCD PT) at high T and/or  Signals for QCD Phase Transitions: In Lab. Expt. Jet Q., v 2, Viscosity, , CC Fluct. & Correl., Hadron Prop.,··· In Astron. Observ.. M-R Rel., Rad. Sp., Inst. R. Oscil., Freq. G. Oscil., ··· QCD Phase Transitions s

 Density & Temperature Dependence of some Properties of Nucleon in DSE Soliton Model (Y. X. Liu, et al., NP A 695, 353 (2001); NPA 725, 127 (2003); NPA 750, 324 (2005) ) ( Y. Mo, S.X. Qin, and Y.X. Liu, Phys. Rev. C 82, (2010) )

( Wei-jie Fu, and Yu-xin Liu, Phys. Rev. D 79, (2009) )   T-dependence of some properties of  &  -mesons and  -  S-L. in the model with contact interaction

 Fluctuation & Correlation of Conserved Charges Recent Lattice QCD results agree with ours excellently! W.J. Fu, Y.X. Liu, & Y.L. Wu, PRD 79, (2010) 。 HotQCD Collaboration,

 Gravitational Mode Pulsation Frequency can be an Excellent Astronomical Signal W.J. Fu, H.Q. Wei, and Y.X. Liu, arXiv: ,1084 Phys. Rev. Lett. 101 ， (2008) Neutron Star: RMF, Quark Star: Bag Model Frequency of g-mode oscillation

Taking into account the  SB effect

Ott et al. have found that these g-mode pulsation of supernova cores are very efficient as sources of g-waves (PRL 96, (2006) ) DS Cheng, R. Ouyed, T. Fischer, ····· g-mode pulsation frequency can be a signal identifying the QCD phase transitions in high density matter ( compact star matter).

 Only the star matter including deconfined quarks can give the one with M  2.0M sun  Hadron-star’s mass can not be larger than 1.8M sun G.Y. Shao, Y. X. Liu, Phys. Rev. D 82, (2010).  Quark-star’s mass can be larger than 2.0M sun （ Nature 467, 1081 (2010) reported ） H.S. Zong, et al., PRD 82, (2010); MPL 25, 47 (2010); PRD 83, (2011); PRD 85, (2012); etc;

 Dynamical Mass is Generated by DCSB;  Phase Diagram is given;  CEP is fixed & Coexisting Phase is discussed;  Some observables are proposed.  Observables ?!  Mechanism ?! Process ?!    Thanks !!  Far from Well Established ! V. Summary & Remarks  Discussed some aspects of the Early Universe Matter Evolution in view of the QCD phase transitions in the DS equation approach of QCD