quark matter under extreme conditions
DESCRIPTION
Quark Matter Under Extreme Conditions. Neda Sadooghi Sharif University of Technology Tehran-Iran Munich-January 2011. F our F undamental F orces. Strong nuclear force . Electromagnetic force. Theory of Everything. Weak nuclear force . Gravitational force . Standard Model of Cosmology. - PowerPoint PPT PresentationTRANSCRIPT
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Quark Matter Under Extreme Conditions
Neda SadooghiSharif University of Technology
Tehran-IranMunich-January 2011
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Force Strength
Theory Mediator
Strong 1 Chromodynamics Gluon
Electromagnetic
10-2 Electrodynamics Photon
Weak 10-7 Flavordynamics W+, W-, Z0
Gravitational 10-39 Geometrodynamics
Graviton
Four Fundamental ForcesStrong nuclear force Electromagnetic force
Weak nuclear force Gravitational force
Theory of Everything
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Standard Model of Cosmology
Big Bang
1019 GeV 1014 GeV 100 GeV ~10-4 eV
Inflationary Epoch
QCD Phase Transition
100 MeV
QGP
EW Phase Transition
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Interaction Couples to Gauge Bosons
Mass (GeV/c2)
Strong Color charge Gluon 0
Electromagnetic
Electric charge
Photon 0
Weak Weak charge W+, W-, Z0 ~100
Standard Model of Particle Physics
Fermions
Family E- Charge
Color Weak Isospin
Spin
1 2 3 LH RH
Leptonsνe νμ ντ 0 - 1/2 - 1/2e μ τ -1 0
Quarksu c t +2/3 r g
b1/2 0 1/2
d s b -1/3 0
SU(3) x SU(2) x U(1)
Quark flavors Quark colors
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Quantum Electrodynamics (QED) describes the force between electrically charged particles in terms of exchange of massless and neutral photons
Elementary process (three point vertex):
QED vs. QCD
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Quantum Electrodynamics (QED)
QED vs. QCD
Coulomb Repulsion
Coulomb Attraction
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QED vs. QCDQuantum Chromodynamics (QCD)
Elementary process(es)
Gluons carry color-charge
Gluon-Gluon Self-Interaction
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QED vs. QCDFlux Lines
Electric flux between a pair of equal and opposite charges Dipole field pattern
Chromoelectric flux between a quark and an antiquark Flux tube
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Quantum Chromodynamics (QCD) Static potential between a quark-antiquark pair
QED vs. QCD
r 0 ↷ A(r) 0 ↷ V(r) 0
Asymptotic Freedom
rrrArV )()(
rrA
ln1)(
fmMeV /880~
Small r
Large r
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String Tensionσ~ 880 MeV/fm
A force sufficient to lift three elephants !!!
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Hadrons: Mesons and Baryons
Confining Potential Hadrons are color singlet
Color Confinement
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Helicity:
For massless particles, helicity and chirality are the same
Right handed particles have positive helicity (chirality) Left handed particles have negative helicity (chirality) Up and down quarks can be regarded as massless A
theory including only up and down quarks should be symmetric under global chiral transformation
Chiral SymmetrySpontaneous Chiral Symmetry Breaking
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QCD at low energy ∋ (u,d)
Proton
Neutron
Pion
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Spontaneous Symmetry Breaking
Spontaneous Chiral Symmetry Breaking:(Pseudo) Goldstone Mechanism: SUL(2)
x SUR(2)
SUL+R(2)π+
π-π0
The mysteries of Mexican Hat Potential
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Standard Model of Cosmology
Big Bang
QCD Phase Transition
100 MeV
QGP
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QCD phase transition at TQCD~2.4 x1012 K~ 200 MeV
Extreme Temperature
Core of our Sun ~ 1.57 x 107 K ~1.3 keV
Room temperature ~ 27 C ~ 300 K ~ 25 meV
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NTe
mpe
ratu
re
Baryonic Chemical Potential
d
u
ss
d
u u
s
d
s
d
u
u
d
s
u s
d
us
ud
sd
QCD Phase Diagram
Hadronic Phase
Quark Gluon Plasma Phase
Color Superconducting phase
Confinement-
Deconfinement phase transition
Tc~170 MeV
Chiral Symmetry Restoratio
n
Earl
y U
nive
rse
RHI
C
LHC
SP S
2SC CFL
Neutron Stars
Hadron gas Nuclear Matter
Hadronic Fluid
μc~310 MeV
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Neutron stars:Laboratories of Matter
under Extreme Conditions
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Neutron star is a type of stellar remnant that can result from gravitational collapse of a massive star during a supernova event
When a giant star dies, it can collapse into a black hole or implode into an ultra-dense neutron star
Pauli exclusion principle supports the neutron star against further collapse (they are made almost entirely of neutrons)
Neutron Stars Natural laboratory for extreme conditions
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Neutron Stars: Structure
Outer crust 0.3-0.5 kmIons and electrons
Inner crust 1-2 kmElectrons, neutrons,
nuclei
Outer core ~9 kmNeutron-proton Fermi
liquidFew % electron Fermi gas
Inner core 0.3 kmQuark-Gluon Plasma/
CFL Color Superconductor ???
0.3-0.4 ϱ0
0.5-2.0 ϱ0
>2ϱ0
Neutron star radius: 12 km
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Radius 6.4x103 km ~6.96 x105 km 12 km
Mass 6x1024 kg 2x1030 kg 2.4x 1030 kg
Density 5 g/cm3
(Mean density)
162.2 g/cm3
(Core) 2.7 x1014 g/cm3
(Core)
Surface gravity
g ~28 g 7x1011 g
Escape velocity
11 km/s 617.7 km/s 1.3x105 km/s
Temperature(Core)
5700 K 1.57 x 107 K 1011 K~ 1-10 MeV
108 x Earth
~3x106 x Earth
56 x Earth
1.2-2 Solar mass
~104 Solar T
1/3 c
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Neutron Stars
Extreme Density
kg12105.5 900
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Neutron Stars:Pulsars
Pulsars are highly magnetized, rotating neutron stars that emit a beam of electro-magnetic radiation
Because neutron stars are very dense objects, the rotation period and thus the interval between observed pulses is very regular Atomic Clocks
The observed periods of the pulses range from 1.4 msec to 8.5 sec
Extremely large magnetic fields MagnetarsSurface: B~1014-1015 GInner field: B~1018-1020 G
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0.6 G100 G
4000 G
4.5 X 105 G~ 45 T
108 G
1014-1015 G
1018-1020 G
Measured at the magnetic pole The Earth’s B fieldHand-held magnet
The magnetic field in strong sunspots
The strongest, sustained magnetic fields
achieved in the labThe strongest fields ever detected on non-neutron
stars
Typical surface magnetic fields of radio
pulsars
Magnetars: Inner fields
Like those used to stick papers on a refrigerator
Within dark, magnetized areas on the solar surface
Generated by huge electromagnets
Strongly-magnetized, compact white dwarf stars
The most familiar kind of neutron star
Soft gamma repeaters and anomalous
X-ray pulsars
Extreme Magnetism
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Vacuum Birefringence (double refraction)Polarized light waves change speed and hence wavelength when they enter a very strong magnetic field
Photon SplittingX-rays split in two or merge together. This process is important in fields stronger than 1014 G
Scattering SuppressionA light wave can glide past an electron with little hindrance if the field is large enough to prevent the electron from vibrating with the wave
Distortion of AtomsFields above 109 G squeeze electron orbitals into cigar shapes. In a 1014 G field, a hydrogen atom become 200 times narrower
Effects of Extreme Magnetism
Calcite crystal: Some letters showing the double refractionLiquid Crystal Displays are also birefringent
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NTe
mpe
ratu
re
Baryonic Chemical Potential
Effects of Extreme Magnetism on Quark Matter
Hadronic PhaseChiral-SB phase
Quark Gluon Plasma Phase
Color Superconducting phase
Tc~170 MeV
Earl
y U
nive
rse
RHI
C
LHC
Neutron Stars
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Relativistic Heavy Ion Colliders
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Center of mass energy √s=200 AGeV for Au+Au collision
Collision with 99.7% speed of light Ultra-RHIC The energy density
ε= 5.5 GeV/fm3
The pressure generated at the time of impact 1030 atmospheric pressure
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Question:Deconfinement Phase Transition
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Color Glass Condensate (CGC) sheets
Initial singularity at the time of collision
Glasma phase (Out of Equilibrium Physics)
Not expected: Strongly correlated QGP (Perfect Fluid)
Mixed phase (quarks, gluons and hadrons)
Hadron Gas
?
CGC
Initial Singularity
Glasma
sQGP
Hadron Gas
?
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Big Bang vs. Little Bang:
The evolution of matter produced in the Little Bang is comparable with the Big Bang (same evolution equations)
t=10-21-10-20sec
t=10-22-10-21sec
t=0-10-22sec
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Perfect Liquid: Strongly Correlated QGP
Electric Plasmam- strongly correlated ??Deconfinement
Dual superconductivitym-correlatione-confined
Magnetized Plasmae-strongly correlated
Confinement
sQGP
(Color) Superconductivitye-correlationm-confined ??
CS
T
μB
T~ 2 Tc
Idea supported by the conjecture of AdS/CFT duality
Tc
1101.1120 Shifman et al
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Chiral Magnetic Effect
Parity Violation in QCD Strong CP ProblemQuestion: Is the world distinguishable from its mirror image?Answer(s): Weak interaction violates P and CP Strong interaction: Experimentally: No evidence of global strong CP violation
C: Matter↔Antimatter
P: Mirror symmetry
Neutron’s EDM ~ 0Theoretically: QCD θ ≠ 0 ( topological charge)
Experimental bound for θ < 3x10-10 Strong CP problemThe existence of topological charge Matter-Antimatter asymmetry in the Early Universe !!
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Chiral Magnetic Effect
Local (event by event) P and CP Violation in QCDTheory: Fukushima, Kharzeev, Warringa, McLerran, (2007-09)Lattice: Polikarpov et al. (2009-10)B~L→ →
Charge separation stems from the interpaly between the strong magnetic field in the early stage of heavy ion collision and the presence of topological configurations in hot matter
BJ
~
Charge separation Electric current
QGP in the deconfined phase
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Chiral Magnetic Effect
Local Parity Violation in QCD Chiral magnetic Effect
B
uR
uL
p
dR
dL
dR
uR
uR
dR
0
L RCharge SeparationBJ
~
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Chiral Magnetic Effect
RHICNon-Central HIC
√sNN ~ 200 GeV b~4 fm eB ~1.3 mπ2 ↷ B~ 4x1018
G
LHCNon-Central HIC
√sNN ~ 4.5 TeV b~4 fm eB ~15 mπ2 ↷ B~ 5x1019
G
D.E. Kharzeev, L.D. McLerran, and H.J. Warringa (0711.0950)
Very Strong Magnetic FieldRHICNon-Central HIC
√sNN ~ 200 GeV b~4 fm eB ~1.3 mπ2 ↷ B ~ 4x1018
G
1019 Gauss
1014 Gauss
eB (M
eV2 )
The strength of B is comparable with Magnetic Field in Neutron Stars
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N
Tem
pera
ture
Baryonic Chemical Potential
Hadronic PhaseChiral-SB phase
Quark Gluon Plasma Phase
Color Superconducting phase
Tc~170 MeV
RHI
C
LHC
Neutron Stars
Effect of Strong Magnetic Fields on Color Superconductivity
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Effect of Strong Magnetic Fields on Color Superconductivity
QED Superconductivity vs. Color Superconductivity
q
qIngredients: (QED) A liquid of fermions with electric charge(QCD) Quarks with electric and color charges
(QED) An attractive electromagnetic interaction between the fermions (QCD) An attractive strong interaction between two quarks (QED) Low temperature: T<Tc
(QCD) Low temperature: In neutron stars T<100 MeV ≪ Big Bang T~1019GeV
(QED) QED Meissner Effect Photons acquire mass (QCD) QCD Meissner Effect Gluons acquire mass
Results:
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Effect of Strong Magnetic Fields on Color Superconductivity
Effects on QCD Phase Diagram (I):Sh. Fayazbakhsh and NS: PRD (2010)
NormalChSB CS
C
Normal
CSC
ChSB
NormalChSB
CSC
NormalNormal
ChSB
ChSB
ChSB
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Effect of Strong Magnetic Fields on Color Superconductivity
Effects on QCD Phase Diagram (II):
De Haas-van Alphen oscillations before the system enters the regime of LLL dominance
Low μ: Only chiral phase transion
2nd order phase transition from chiral SB to the Normal phase
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Effect of Strong Magnetic Fields on Color Superconductivity
Effects on QCD Phase Diagram (III):Low T: Chiral and Color phase transions
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Results1. The type of the phase transition between chiral SB and
the Normal phase changes with B: 2nd Order 1st Order
2. Increasing B has no effect on the type of phase transition between the color symmetry breaking and the normal phase (2nd order)
3. De Haas-Van Alphen oscillations CSC-Normal-CSC phase transition
4. For eB>eBt: The effect of T and μ are partly compensated by B
5. For eB>eBt ~ 0.5 GeV2: System is in the LLL dominant regime
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Effect of Strong Magnetic Fields on Color Superconductivity
Effects on QCD Phase Diagram (II):Intermediate μ: Chiral and Color phase transions
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Effect of Strong Magnetic Fields on Color Superconductivity
Effects on QCD Phase Diagram (II):Large μ: Only Color phase transion
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Effect of Strong Magnetic Fields on Color Superconductivity
Effects on QCD Phase Diagram (III):Intermediate T: Chiral and Color phase transions
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Effect of Strong Magnetic Fields on Color Superconductivity
Effects on QCD Phase Diagram (III):Large T: Only Chiral phase transion