1. Suggested Course Layout
Move class from 3 days a week to 2 days a week
Proposal: Mo 2-4 p.m., Tu 11 a.m.-1 p.m.
Jan8,9: week1 – Intro and kinematic variables
Jan15,16: Bormio Winter Workshop, no class
Jan 22,23: weeks 2 & 3 – Spacetime evolution of asymptotic freedom
Jan 29,30: week 4 – thermal and hydromodels
Feb 5,6: week 5 – pQCD in QGP physics
Feb 12,13: Big Sky Winter Workshop, no class
Feb 19,20: week 6 – lattice QCD
Feb 26,27: weeks 7 & 8 – initial conditions and complete modeling
Mar 5,6: week 9 – bulk signatures and properties
Mar 12,13: Spring Break, no class
Mar 19,20: week 10 – rare particle production
Mar 26,27: week 11 – high momentum probes
Apr 2,3: week 12 – RHIC and its detectors
Apr, 9,10: week 13 – essays (I)
Apr 16,17: week 14 – essays (II)
Apr 23: overflow

2. Motivation for Relativistic Heavy Ion Collisions
Two big connections: cosmology and QCD

3. The phase diagram of QCD
Early universe
quark-gluon plasma
critical point ? Tc
Temperature
colour
superconductor
hadron gas
nucleon gas
nuclei
CFL r0
Neutron stars
vacuum
baryon density

4. Evolution of Forces in Nature

5. RHIC, LHC & FAIR RIA & FAIR Going back in time…
Age Energy Matter in universe
GeV grand unified theory of all forces
10-35 s GeV 1st phase transition
(strong: q,g + electroweak: g, l,n)
10-10 s 102 GeV 2nd phase transition
(strong: q,g + electro: g + weak: l,n)
10-5 s 0.2 GeV 3rd phase transition
(strong:hadrons + electro:g + weak: l,n)
3 min MeV nuclei
6*105 years 0.3 eV atoms
Now 3*10-4 eV = 3 K
(15 billion years)
RHIC, LHC & FAIR
RIA & FAIR

6. Connection to Cosmology
Baryogenesis ?
Dark Matter Formation ?
Is matter generation in cosmic medium (plasma) different than matter generation in vacuum ?

7. Sakharov (1967) – three conditions for baryogenesis
Baryon number violation
C- and CP-symmetry violation
Interactions out of thermal equilibrium
Currently, there is no experimental evidence of particle interactions where the conservation of baryon number is broken: all observed particle reactions have equal baryon number before and after. Mathematically, the commutator of the baryon number quantum operator with the Standard Model hamiltonian is zero: [B,H] = BH - HB = 0. This suggests physics beyond the Standard Model
The second condition — violation of CP-symmetry — was discovered in 1964 (direct CP-violation, that is violation of CP-symmetry in a decay process, was discovered later, in 1999). If CPT-symmetry is assumed, violation of CP-symmetry demands violation of time inversion symmetry, or T-symmetry.
The last condition states that the rate of a reaction which generates baryon-asymmetry must be less than the rate of expansion of the universe. In this situation the particles and their corresponding antiparticles do not achieve thermal equilibrium due to rapid expansion decreasing the occurrence of pair-annihilation.

8. Dark Matter in RHI collisions ? Possibly (not like dark energy)
The basic parameters: mass, charge

9. Isentropic Adiabatic Basic Thermodynamics
Hot
Sudden expansion, fluid fills empty space without loss of energy.
dE = 0 PdV > 0 therefore dS > 0
Hot
Hot
Gradual expansion (equilibrium maintained), fluid loses energy through PdV work.
dE = -PdV therefore dS = 0
Hot
Isentropic Adiabatic
Cool

10. Nuclear Equation of State

11. Nuclear Equation of State

12. Golden Rule 1: Entropy per co-moving volume is conserved
Golden Rule 2: All entropy is in relativistic species
Expansion covers many decades in T, so typically either T>>m (relativistic) or T<<m (frozen out)
Golden Rule 3: All chemical potentials are negligible
Golden Rule 4:

13. g*S Start with light particles, no strong nuclear force 1 Billion oK
1 Trillion oK
Start with light particles, no strong nuclear force

14. g*S Now add hadrons = feel strong nuclear force 1 Billion oK
1 Trillion oK
Previous Plot
Now add hadrons = feel strong nuclear force

15. g*S Keep adding more hadrons…. 1 Billion oK 1 Trillion oK
Previous Plots
Keep adding more hadrons….

16. How many hadrons?
Density of hadron mass states dN/dM increases exponentially with mass.
TH ~ 21012 oK
Broniowski, et.al. 2004
Prior to the 1970’s this was explained in several ways theoretically
Statistical Bootstrap Hadrons made of hadrons made of hadrons…
Regge Trajectories Stretchy rotators, first string theory

17. Ordinary statistical mechanics
For thermal hadron gas (somewhat crudely):
Energy diverges as T --> TH
Maximum achievable temperature?
“…a veil, obscuring our view of the very beginning.” Steven Weinberg, The First Three Minutes (1977)
Rolf Hagedorn German
Hadron bootstrap model and limiting temperature (1965)

18. QCD to the rescue! Replace Hadrons (messy and numerous)
D. Gross
H.D. Politzer
F. Wilczek
Replace Hadrons (messy and numerous)
by Quarks and Gluons (simple and few)
American
QCD Asymptotic Freedom (1973)
e/T4
 g*S
Thermal QCD ”QGP” (Lattice)
“In 1972 the early universe seemed hopelessly opaque…conditions of ultrahigh temperatures…produce a theoretically intractable mess. But asymptotic freedom renders ultrahigh temperatures friendly…” Frank Wilczek, Nobel Lecture (RMP 05)
Hadron gas
Karsch, Redlich, Tawfik, Eur.Phys.J.C29: ,2003

19. Nobel prize for Physics 2005
“Before [QCD] we could not go back further than 200,000 years after the Big Bang. Today…since QCD simplifies at high energy, we can extrapolate to very early times when nucleons melted…to form a quark-gluon plasma.” David Gross, Nobel Lecture (RMP 05)
g*S
Thermal QCD -- i.e. quarks and gluons -- makes the very early universe tractable; but where is the experimental proof?
n Decoupling
Nucleosynthesis
e+e- Annihilation
Heavy quarks and bosons freeze out
QCD Transition
Mesons freeze out
Kolb & Turner, “The Early Universe”

20. The main features of Quantum Chromodynamics (QCD)
Confinement
At large distances the effective coupling between quarks is large, resulting in confinement.
Free quarks are not observed in nature.
Asymptotic freedom
At short distances the effective coupling between quarks decreases logarithmically.
Under such conditions quarks and gluons appear to be quasi-free.
(Hidden) chiral symmetry
Connected with the quark masses
When confined quarks have a large dynamical mass - constituent mass
In the small coupling limit (some) quarks have small mass - current mass

21. Quarks and Gluons

22. Basic Building Blocks ala Halzen and Martin

23. Quark properties ala Wong

24. What do we know about quark masses ?
Why are quark current masses so different ?
Can there be stable (dark) matter based on heavy quarks ?

25. Elementary Particle Generations

26. Some particle properties

27. Elemenary particles summary

28. Comparing QCD with QED (Halzen & Martin)

29. Quark and Gluon Field Theory == QCD (I)

30. Quark and Gluon Field Theory == QCD (II)

31. Quark and Gluon Field Theory == QCD (III)
Boson mediating the q-qbar interaction is the gluon.
Why 8 and not 9 combinations ? (analogy to flavor octet of mesons)
R-Bbar, R-Gbar, B-Gbar, B-Rbar, G-Rbar, G-BBar
1/sqrt(2) (R-Rbar - B-Bbar)
1/sqrt(6) (R-Rbar + B-Bbar – 2G-Gbar)
Not: 1/sqrt(3) (R-Rbar + G-Gbar + B-Bbar) (not net color)

32. Hadrons

33. QCD – a non-Abelian Gauge Theory

34. Particle Classifications

35. Quarks

36. Theoretical and computational (lattice) QCD
In vacuum:
- asymptotically free quarks have current mass
- confined quarks have constituent mass
- baryonic mass is sum of valence quark constituent masses
Masses can be computed as a function of the evolving coupling
Strength or the ‘level of asymptotic freedom’, i.e. dynamic masses.
But the universe was not a vacuum at the time of hadronization, it was likely a plasma of quarks and gluons. Is the mass generation mechanism the same ?

37. Confinement Represented by Bag Model

38. Bag Model of Hadrons

39. Comments on Bag Model

40. Still open questions in the Standard Model

41. Why RHIC Physics ?

42. Why RHIC Physics ?