On viscosity of Quark Gluon Plasma侯德富华中师范大学粒子物理所高能物理学会第八届代表大会南昌4月17----20日
1 On viscosity of Quark Gluon Plasma 侯德富 华中师范大学粒子物理所 高能物理学会第八届代表大会南昌 4月17-20日
OutlinesIntroduction and motivationViscosity from Kubo formulaViscosity from kinetic theory (Boltzmann Eg)Viscosity from AdS/CFTSummary
2 ◼ Introduction and motivation ◼ Viscosity from Kubo formula ◼ Viscosity from kinetic theory (Boltzmann Eq) ◼ Viscosity from AdS/CFT ◼ Summary Outlines
MotivationsExperiments aspect:@RHICRobust collective flows, well described by hydrowith Lattice-based EoS. This indicates verystrong interaction even at early time => sQGPsQGP seems to be the almost perfectfluid knownn/s>= .1-.2<<1
3 @ RHIC ◼ Robust collective flows, well described by hydro with Lattice-based EoS. This indicates very strong interaction even at early time => sQGP ◼ sQGP seems to be the almost perfect fluid known /s>= .1-.2<<1 Motivations Experiments aspect:
Study of dissipativeeffects on<v2>How sensitive is elliptic flow to finite n/s?Viscous HvdroCascade (2<->2,2<->3)25STAR v,(4)0.08PHOBOSTrack-basedidealn/s=0.03PHOBOSHit-based20m/s=0.08BAMPSα=0.30.06m/s=0.16BAMPSα=0.6STAR150.042100.020.000501002503003504003150200124P,[GeV]NZ.XuC.Greiner,PRL101(08)partAgreement for α.=0.3-0.6Dependence on trelaxation timeoorderexpansionn/s=0.15 - 0.08With green terms (D. Rischke)
4 Study of dissipative effects on <v2> How sensitive is elliptic flow to finite /s? Z. Xu & C. Greiner, PRL 101(08) Agreement for s=0.3 – 0.6 /s=0.15 – 0.08 Viscous Hydro Cascade (2<->2,2<->3) P. Romatschke, PRL99 (07) Dependence on tp relaxation time II0 order expansion with green terms (D. Rischke)
QCDunderextremeconditionsLattice(Fodar&Katzhep-lato402006)QGP/NQ150EarhyUniversefullQCD(?)NJL(R0steretal,hep-ph/0503184)[Aewl 100'moderale'diquarkcoupingXSB50NeutronstarsgescCFLNO200100300400COFμ [MeV]At very High T or density ( deconfined)High T (Early universe, heavy-ion collisions)High density matter ( in the core of neutron stars)5
5 QCD under extreme conditions ◼ At very High T or density ( deconfined) ◼ High T (Early universe, heavy-ion collisions) ◼ High density matter ( in the core of neutron stars)