phenomenological description of the quark-gluon-plasma
DESCRIPTION
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 ...: sQGP has no quasi-particle description. - PowerPoint PPT PresentationTRANSCRIPT
B. Kampfer I Institute of Radiation Physics I www.hzdr.deMember of the Helmholtz Associationpage 1
B. Kampfer I Institute of Radiation Physics I www.hzdr.de
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 ...: sQGP has no quasi-particle description
1. QGP parametrization: EoS, viscosities (obituary or revival of QPM?) 2. bottom-up approach within AdS/QCD
B. Kampfer I Institute of Radiation Physics I www.hzdr.deMember of the Helmholtz Associationpage 2
hadrons
quar
ks &
glu
ons
LHC RHIC SPSAGS
SIS
universe
An
dro
nic
, P
BM
, S
tach
el:
*
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Scales
Confinement in Early Universe
no specific relics (unless p + n)(contrary to BBN: 25% He)
HICs
puzzle = entropy production (thermal.)
Neutron Stars proto-star in core collapse: t ~ 1 sec, T < 50 MeVquark cores?
Milne coordinates
Steiner et al., 1205.6871 - bursting NSs + photosperic expansion- transiently accreting NSs in quiescence
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Landau & Fermi liquids: adiabaticity & Pauli‘s exclusion principle
Fermi gas Fermi liquid
no interaction interaction keeps spin, charge, momenta ...but modifies masses ...
in this spirit: QGP = Bose + Fermi gases masses = self-energies
m(T) ~ T G(T), large T: G g(pQCD)
Quasi-Particle Model
does not apply always: Luttinger fluid, ...
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2-Loop Approximation to CJT/Phi Funct.
1-loop self-energies
+ HTL self-energies gauge invariance
finite widths: Peshier-Cassing, Bratkovskaya
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Going to High Temperatures
Boyd et al.
Fodor et al.
Aoki et al.
region of fit
M.Bluhm
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Peshier‘s Flow Equation given form
Cauchy problem: initial values
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Susceptibilities: Test of mu Dependence
data: Allton et al., Nf = 2
10% problem
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data: Allton et al., Nf = 2
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data: Allton et al., Nf = 2
also good agreement with Gavai-Gupta data for
sensible test of flow eq. & baryon charge carriers (no di-quarks etc. needed)
F. Karsch: cumulants & fluctuations HRG & QPM
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Purely Imaginary mu
M.P. Lombardo et al.
polyn. cont.
Roberge-Weiss Z3 symmetry
T=3.5,2.5,1.5,1.1 Tc
Nf = 4
cont. to real mu:
I = II, I‘ = inflected I‘‘
QPM
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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
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water:
Gluon Plasma
Viscous Fluids
data: Meyer Nakamura, Sakai
AMY 2003
QPM
Intro: V. Greco
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QPM Viscosities
Decomposition:
Kinetic eq.:
e.m. tensor:
Relaxation time approx.:
EoS
transp.
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further details: Bluhm, BK, Redlich, PLB 2012, PRC 2011
EoS
strong coupling:Gubser, Buchel
pQCD:
ad hoc
2 Vosresensky et al. (2011): ambiguity of rel. time ansatz
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KSS
data: Boyd et al. Okoamoto et al.
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AdS/YMinstead of QCD
Maldacena 1998Witten 1998Gubser et al. 1998
AdS5/CFT4
super YM
gravity5
holographyQCD4
Einstein + scalar field large-Nc YM
bottom-up approach: adjust V(phi) to EoS for free: drag & jet quentching, chir. symm. spectra of glueballs, hadrons ...
quantitytive matching to QCD is difficult
common symmetry group SO(2,d)
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EoS SU(3) YM4 Panero: mild/no dependence
I/T4 = T (p/T4)‘
e = I + 3ps = (I + 4p)/Tcs
2 = p‘ / (T p‘‘)
non-pert.
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Einstein4
Riemann space-time: glk;n = 0
Rij + gij R/2 = k Tij
gravity/geometrygravity/geometry
mattermatter
Gubser, Kajantie, Kiritsis
Li et al.
AdS: , constant curvature negative L in
Lorentz inv. vacuum: Tij = (e + p) uiuj + p gij -> - L gij
= 0Einstein‘s GRG is well tested (PPN coefficients fit observations)
maximally symmetric
(e < 0, p > 0)
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Black Holes, e.g. Schwarzschild ds2 = f(r)-1 dr2 + r2 dO2
2 – f(r) dt2
f(r) = 1 – 2M/r: r H = 2M horizon (simple zero)
Hawking temperature Hawking-Bekenstein entropyHawking‘s hairless theorem: M, Q, J
s(T) EoS
Schwarzschild vacuole in Friedmann-Walker-Lemaitre universe
BH
Schwarzschild
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z = 1/r
t, xAdS, UV
horizon, IR
z = 0
zH
1st ansatz:
2nd ansatz:
3rd ansatz:
boundary conds.: AdS
BH
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Transport Coefficients: Gubser 2008
fluctuations:
linearize Einstein eqs.
shear mode:
with phi as holographic coordinate (instead of r or z) Kubo formulae
bulk mode:
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mimicks EoS
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next steps: fine tuning of V or As robustness of zeta? spectral functions (no transport peaks) quarks, mu > 0
Summary
QPM parametrization of EoS: YM + QGP: mu = 0 T dep. susceptibilities: mu > 0, mu_u,d imaginary mu T 0, mu > 0: quark stars?
AdS/YM: holographic improvement needed (EoS 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
Kajantie et al.... et al.
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Quark Matter in Neutron Stars?
1054 AD: supernova radio pulsar
X ray source
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Neutron Stars & White Dwarfs
R [km]
M / M_sun
1.4
2.0
10 20 10,000
unstable
stable
e, n
p
Chandrasekhar
e-, nuclei
n, (p, e-)
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Neutron Stars with Quark Cores (1)
R [km]
M / M_sun
1.4
2.0
10 20 10,000
unstable
stable
e, n
p
Chandrasekhar
e-, nuclei
n, (p, e-)
q
q
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Neutron Stars with Quark Cores (2)
R [km]
M / M_sun
1.4
2.0
10 20 10,000
unstable
1)2)
3)
density jump e2/e1 is- very small: 1)- < 1.5: 2)- > 1.5: 3)
T
n
CEP
mixNf = 3
e, n
p qmix
e1 e2
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The Third Island
R [km]
M / M_sun
1.4
2.0
10 20 10,000
T
n
CEP
mixNf = 3
e, n
p qmix
e1 e2
1)
2)
density jump is- small and EoS(q) stiff: 1)- larger and/or EoS(q) soft: 2)
BK, PLB 1982Stocker, Schaffner-B. 2000
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Pure Quark Starsfit to Bielefeld & WuppertalBp data
hybrid stars:sensitive tomatching of EoS
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Examples of Side Conditions
T = 1.1 Tc
solid: pure Nf=2 quark matter, electr.neutr.dashed: Nf=2 quark matter + electrons in beta equilibrium
d
u
e
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Gubser: VLi: As(z)
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mild increase (Gubser, Kiritsis)strong increase (Kharzeev, Tuchin Karsch et al.)
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