Phenomenological Description of the QuarkGluonPlasma B Kmpfer HelmholtzZentrum
Phenomenological Description of the Quark-Gluon-Plasma B. Kämpfer Helmholtz-Zentrum Dresden-Rossendorf Technische Universität Dresden M. Bluhm, R. Schulze, R. Yaresko, F. Wunderlich, M. Viebach K. Rajagopal, T. Schafer, U. Wiedemann . . . : s. QGP has no quasi-particle description 1. QGP parametrization: Eo. S, viscosities (obituary or revival of QPM? ) 2. bottom-up approach within Ad. S/QCD page Member of the Helmholtz Association Kampfer I I Instituteofof. Radiation. Physics I I www. hzdr. de B. B. Kampfer
hadro ns page 2 LHC RHIC SPS AGS SIS Andronic, PBM, Stachel: * qu ar ks & glu on s universe Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Scales Confinement in Early Universe no specific relics (unless p + n) (contrary to BBN: 25% He) Milne coordinates HICs puzzle = entropy production (thermal. ) Neutron Stars proto-star in core collapse: t ~ 1 sec, T < 50 Me. V quark cores? Steiner et al. , 1205. 6871 page 3 - bursting NSs + photosperic expansion - transiently accreting NSs in Member quiescence of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Quasi-Particle Model Landau & Fermi liquids: adiabaticity & Pauli‘s exclusion principle Fermi gas Fermi liquid no interaction keeps spin, charge, momenta. . . but modifies masses. . . does not apply always: Luttinger fluid, . . . in this spirit: QGP = Bose + Fermi gases masses = self-energies m(T) ~ T G(T), page 4 large T: G g(p. QCD) Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
2 -Loop Approximation to CJT/Phi Funct. 1 -loop self-energies + HTL self-energies gauge invariance page 5 finite widths: Peshier-Cassing, Member of the Bratkovskaya Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Going to High Temperatures Fodor et al. Boyd et al. region of fit M. Bluhm page 6 Aoki et al. Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Peshier‘s Flow Equation given form Cauchy problem: initial values page 7 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Susceptibilities: Test of mu Dependence 10% problem page 8 data: Allton et al. , Nf = 2 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
data: Allton et al. , Nf = 2 page 9 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
also good agreement with Gavai-Gupta data for data: Allton et al. , Nf = 2 sensible test of flow eq. & baryon charge carriers (no di-quarks etc. needed) F. Karsch: cumulants & fluctuations HRG & QPM page 10 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Purely Imaginary mu Nf = 4 M. P. Lombardo et al. QPM T=3. 5, 2. 5, 1. 1 Tc cont. to real mu: polyn. cont. Roberge-Weiss Z 3 symmetry page 11 I = II, I‘ = inflected I‘‘ Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
adjust QPM parameterization at to get 1. phase border line (= characteristic trought Tc) 2. p(T) data: Engels et al. PLB 1997 tests Peshier‘s flow eq. (chem. pot. degree of freedom), at least for Nf = 4 deg. quarks page 12 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Viscous Fluids Intro: V. Greco water: Gluon Plasma AMY 2003 data: Meyer Nakamura, Sakai QPM page 13 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
QPM Viscosities Decomposition: Eo. S transp. Kinetic eq. : e. m. tensor: Relaxation time approx. : page 14 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Eo. S p. QCD: ad hoc strong coupling: Gubser, Buchel further details: Bluhm, BK, Redlich, PLB 2012, PRC 2011 2 page 15 Vosresensky et al. (2011): ambiguity of rel. time ansatz Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
data: Boyd et al. Okoamoto et al. KSS page 16 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Ad. S/YM instead of QCD Maldacena 1998 Witten 1998 Gubser et al. 1998 Ad. S 5/CFT 4 common symmetry group SO(2, d) super YM gravity 5 holography Einstein + scalar field QCD 4 large-Nc YM bottom-up approach: adjust V(phi) to Eo. S for free: drag & jet quentching, chir. symm. spectra of glueballs, hadrons. . . quantitytive matching to QCD is difficult page 17 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
non-pert. Panero: mild/no dependence Eo. S SU(3) YM 4 I/T 4 = T (p/T 4)‘ e = I + 3 p s = (I + 4 p)/T cs 2 = p‘ / (T p‘‘) page 18 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Einstein 4 Riemann space-time: glk; n = 0 Rij + gij R/2 = k Tij gravity/geometry matter Gubser, Kajantie, Kiritsis Li et al. maximally symmetric Ad. S: , constant curvature negative L in Lorentz inv. vacuum: Tij = (e + p) uiuj + p gij -> - L gij =0 (e < 0, p > 0) Einstein‘s GRG is well tested (PPN coefficients fit observations) page 19 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Black Holes, e. g. Schwarzschild ds 2 = f(r)-1 dr 2 + r 2 d. O 22 – f(r) dt 2 f(r) = 1 – 2 M/r: r H = 2 M horizon (simple zero) Hawking temperature Hawking-Bekenstein entropy Hawking‘s hairless theorem: M, Q, J s(T) Eo. S Schwarzschild vacuole in Friedmann-Walker-Lemaitre universe BH Schwarzschild page 20 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
z = 1/r z. H horizon, IR z=0 Ad. S, UV t, x 1 st ansatz: 2 nd ansatz: 3 rd ansatz: boundary conds. : Ad. S BH page 21 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
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Transport Coefficients: Gubser 2008 fluctuations: linearize Einstein eqs. Kubo formulae shear mode: with phi as holographic coordinate (instead of r or z) bulk mode: page 25 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
mimicks Eo. S page 26 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Summary QPM parametrization of Eo. S: YM + QGP: mu = 0 T dep. susceptibilities: mu > 0, mu_u, d imaginary mu T 0, mu > 0: quark stars? Ad. S/YM: holographic improvement needed (Eo. S vs. V(phi) or As(z); pert. regime? eta = s / 4 pi vs. pert. Regime zeta(T), zeta/eta vs. (1/3 – vs^2) ) No specific relicts of cosmic confinement (memory loss) contrary to BBN next steps: fine tuning of V or As robustness of zeta? et al. spectral functions (no transport peaks) Kajantie. . . et al. quarks, mu > 0 page 27 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Quark Matter in Neutron Stars? 1054 AD: supernova radio pulsar page 28 X ray source Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Neutron Stars & White Dwarfs 2. 0 M / M_sun stable 1. 4 unstable Chandrasekhar n, (p, e-) e-, nuclei p e, n 10 page 29 20 10, 000 R [km] Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Neutron Stars with Quark Cores (1) 2. 0 M / M_sun q stable 1. 4 unstable Chandrasekhar n, (p, e-) e-, nuclei q p e, n 10 page 30 20 10, 000 R [km] Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Neutron Stars with Quark Cores (2) 2. 0 M / M_sun density jump e 2/e 1 is - very small: 1) - < 1. 5: 2) - > 1. 5: 3) 1) 2) 1. 4 unstable T 3) CEP p mix q Nf = 3 mix e, n e 1 e 2 10 page 31 n 20 10, 000 R [km] Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
The Third Island 2. 0 M / M_sun density jump is - small and Eo. S(q) stiff: 1) - larger and/or Eo. S(q) soft: 2) 1) 1. 4 BK, PLB 1982 Stocker, Schaffner-B. 2000 2) T CEP p mix q Nf = 3 mix e, n e 1 e 2 10 page 32 n 20 10, 000 R [km] Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Pure Quark Stars fit to Bielefeld & Wuppertal. Bp data hybrid stars: sensitive to matching of Eo. S page 33 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
Examples of Side Conditions T = 1. 1 Tc d u e solid: pure Nf=2 quark matter, electr. neutr. dashed: Nf=2 quark matter + electrons in beta equilibrium page 34 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
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Gubser: V page 36 Li: As(z) Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
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mild increase (Gubser, Kiritsis) strong increase (Kharzeev, Tuchin Karsch et al. ) page 38 Member of the Helmholtz Association B. Kampfer I Institute of Radiation Physics I www. hzdr. de
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