1. Helmholtz-Zentrum Dresden-Rossendorf Extreme Matter in the Universe
B. Kämpfer
Indian Summer School 2011
Extreme Matter in the Universe
(part 3)

2. LHC at CERN: searching Higgs, SUSY, the unknown
SM: masses of quarks & part
of leptons (e.g., e-)
P. Higgs 1964

3. Mystery of Mass

4. LHC at CERN: investigating the quark-gluon plasma

5. Rel. Heavy-Ion Colls.: RHIC & LHC
hydro applies:
Frankfurt HIC group

6. Thermal Model at Work chemical freeze-out densities  ratios
adjust to data
Andronic et al

7. Chemical Freeze-Out Systematics
PBM, Stachel,

8. Particles vs. Antiparticles
post- and pre-dictions
Andronic et al

9. Blast Wave Fits kinetic freeze-out chem. f.o. fit of pT spectra
by T and v
ALICE
BK 1996

10. Fluid Dynamics for urHICst
present day standard tool:
3. kinetics (transport model)
2. hydrodynamics
1. kinetics (transport model)
mid
rapidity
hydro: hadron gas
hadronization
chemical f.o.
weak decays
preequilibrium
hydro: sQGP
first contact
kinetic f.o. x t
free stream ?
fluid
free stream

11. Milne Coordinates
Bjorken flow:
Bjorken symmetry:
Gubser flow:

12. Bjorken Flow  Milne cordinates Bjorken symmetry
EoS in conformal limit: e = 3p 
 entropy in comoving volume = conserved
for every EoS
w/o dissipation
mystery:

13. Longitudinal Pressure Gradient
v = th y
initial conds: Bjorken flow
Bozek, PRC 2009
init. non-Bjorken flow:
different evolution
it is hard to modify
Bjorken‘s flow once it
is there
 origin of Bjorken flow?
Kajantie, Eskola, Russkanen, EPJC 1998

14. Soft and Hard Probes
ALICE, PLB 2011
jets

15. Hard Probes: Medium Modifications
energy loss
RHIC: disappearence
of away-side jet

16. Transverse Flow soft probes central semi-central peripheral no p
momentum space
configuration space

17. hydro  Cooper-Frye  momentum distrib.  v2(p_perp)
STAR at RHIC
Bluhm et al., PRC 2007
hydro  Cooper-Frye  momentum distrib.  v2(p_perp)

18. B. Schenke

19. U.Heinz, Crete 2011

20. U.Heinz, Crete 2011

21. Viscous Fluid Dynamics
water is good fluid, honey not, oil partially

22. bulk viscosity
shear viscosity
 rel. Navier-Stokes eqs.

27. Viscosities from Calculations
Bluhm, BK, Redlich, PRC 2011

28. A Unified Description: AdS/CFT2 1
Chesler, Yaffe, PRL 2011 1‘ 3 2‘
time
AdS/CFT: 1. solve 5d Einstein vacuum eqs. (with symmetries)
with negative cosmological constant
2. obtain 4d energy-momentum tensor from
holographic renormalization (boundary theory)

29. What remains for CBM at FAIR?
energy
frontier
SIS18
Bevalac
AGS
SPS
RHIC
LHC
SIS100/300
intensity frontier: rare probes (charm, photons, dileptons)
T = mu

30. GSI
FAIR
1.2 BEUR

31. FAIR

32. PBM, Stachel,

33. physics case
technical design
simulations & feasibility

34. Key Issues for CBM in-depth study of onset of deconfinement
EoS & transport coefficients
medium modifications hadrons
„never studied“ at SIS100/300 energies:
charm: hidden & open, charm baryons
(created early  probe dense stage)
dileptons & photons: penetrating probes
(monitoring the dense stage, looking into fireball)
fluctuations: higher moments sensitive to proxy of CEP
correlations: size (temporal & spatial) measurements

35. Strongly Coupled Systems
transport peak
 quasi-particles
AdS/CFT
weak coupling
strong coupling

36. Summary Cosmic Confinement/Hadronization: no imprints
nucleons as remainder due small excess (= accident?)
Nucleosynthesis: sensitive test of cosmic dynamics
abundancies of light elements is specific imprint
Neutron Stars: quark cores seem possible
(but hard to verify; need fine tuning of cold EoS)
RHIC & LHC: sQGP seems w/o doubts, EoS from lattice QCD,
sQGP = most perfect fluid: viscosities are small,
energy scan at RHIC gives orientation (no rare probes)
HADES&CBM at SIS100/300: exploration of phase diagram,
rare & penetrating probes, closer link to hadron physics

37. Probing the Fireball‘s Interior
PRL 2007
thermal radiation:
Gallmeister et al. PLB 2000
Rapp-Shuryak PLB 2000

38. DLS Puzzle Solved by Bremsstrahlung?
Nikola Tesla 1888
Barz et al
Bratkovskaya, Cassing
NPA 2008
C(1 AGeV) + C
DLS: PRL 1997
HADES: PLB 2008
M [GeV]
1997: bremsstrahlung ... contribution
was found to be small
2007: DLS puzzle... may be solved
when incorporating a stronger
bremsstr. contribution
Aichelin et al. 2008: w/ bremsstrahlung
Santini et al. 2008: w/o bremsstrahlung
Schmidt et al. 2009: w/o bremsstrahlung

39. CERES Pb(158 AGeV)+Au <T> = 170 MeV cocktail thermal rad.
DY thermal rad. cocktail t
pre-equ. fireball freeze-out

40. NA60: Di-Muons LMR IMR NA60 broadening no shift NA60 0907.3935

41. RHIC real photons cocktail confirmed by pp Quarks & Gluons PHENIX
Drees
PHENIX
real photons
Quarks & Gluons
Hadrons
cocktail confirmed by pp
PHENIX
PHENIX

42. Dielectrons
PHENIX data

43. Photons
PHENIX data

44. Fluid Dynamics from Gravity
FG coordinates
Bhattacharyya, Hubeny, Rangamani ... JHEP 2008
bulk near z = 0, asymp. AdS metric & black brane
strong coupling regime: universal sector in
long-wavelength solutions, isotropization
 assume as relevant d.o.f.

45. epsilon expansion: z expansion equivalent?
iterative solutions of Einstein eqs.  constitutive eqs.:
extrinsic curvature
on r = const from

46. The Janik Route Bjorken flow + symmetry, Milne coordinates e
Janik, Lecture Notes Phys. 2011
Bjorken flow + symmetry, Milne coordinates e

47. Get e(tau) from AdS/CFT
FG coordinates: 1
boundary theory: z = 0
z expansion (indices suppressed):
...
iterative solution
for n > 4
Einstein eqs.
Skenderis et al., 2000
Definition: Kretschmann

48. requirement: K = regular (no singularities in the bulk)  values of
Large tau:
requirement: K = regular (no singularities in the bulk)
 values of
the only scale
shear viscosity =
Gyulassy, Danilewicz PRD 1985
numbers
Small tau:
Einstein eqs.  constraints for A, B, C  allowed init. conds.
anisotropy measure
Beuf et al., JHEP 2009

49. 1st-order hydro stage: q = 0  F/w = 2/3
Heller, Janik, Witaszczyk 2011
1st-order hydro stage: q = 0  F/w = 2/3

50. Comparison of with Frankfurt
third-order rel. diss. hydro,
extension of Israel-Stewart
El, Xu, Greiner, PRC 2010
Denicol, Koide, Rischke, PRL 2010
shear tensor:
for Bjorken flow & symm.
Boltzmann
m = 0
transient dynamics
looks as gradient expansion

51. start from equilibrium:
start from off-equilibrium: