B. Kämpfer | Institut für Strahlenphysik | Hadronenphysik | Helmholtz-Zentrum Dresden-Rossendorf...

B. Kämpfer | Institut für Strahlenphysik | Hadronenphysik | www.hzdr.de

Helmholtz-Zentrum Dresden-Rossendorf

B. Kämpfer

Indian Summer School 2011

Extreme Matter in the Universe(part 1)


when where what

1) t ~10^-6 s everywhere hadronization small

2) t ~ 10^2 s everywhere nucleosynthesis large neutrino decoupl.

e+ e- annihilation

3) now neutron stars cbm large

4) now CERN hadronization small

5) 2018 AD FAIR CBM large

www questions

aft

er

Big

Ba

ng


What is Extreme?

(i) hot: T ~ 100 MeV ~ 10^12 K

(ii) dense: rho ~ 10^15 g/cm^3 ~ 5 rho_0

(iii) fast: dt < 10 fm/c ~ 30 ys = 30x10^-24 s

RX J185635-3754

UrQMD + GEANT4


Numerology

in nuclei


2) = rather normal, but interesting playground

1 2 3 4 5 T x x xrho x x dt x x

un

ive

rse

ha

dro

niz

atio

n

un

ive

rse

nu

cle

osy

nth

esi

s

ne

utr

on

sta

rs

LH

C,

RH

IC

FA

IR C

BM

What are our Questions?

QCD hadrons (structure + interactions)phase diagram of SIMdeconfined SIM = sQGP = ?

hot

dense

short


Barz et al., PLB 1987

TCEP

Nf = 3

T

n

CEP

mixNf = 3

T

Nf = 3

Phase Diagram of SIM


or

n

T

phase diagramof water


Gauge Theories w/o SSB Abelian (QED) non-Abelian (QCD)

E E

1/137

1

sQCD pQCD

Land

au p

ole

UV

sla

very

asymp. freedom

non-trivial vacuum:condensates

not neccessarily weak-coupling:alpha too large

0


Columbia plot Wuppertal-Bp plot

O(4) vs. Ising


Hadron Resonance Gas

T < Tc: hadrons Dashen-Ma-Bernstein theorem

Wuppertal-Bp


Gluon Gas: Nf = 0QCD trace anomaly: e – 3p = 0


Trace Anomaly/Interaction Measure

quasi-particle model: adjustment to lattice QCD results susceptibilities, transport coeff.

Bielefeld lattice QCD: Tc puzzle


Bielefeld-Swansea data

c0

c2

c4

c6

D=1.15

neglect strong interaction

QPM

lQCD


Tools: (1) Fluid Dynamicslong-wavelength modes T(x), mu(x), u(x) and their gradients

currents

1) 2nd law of thermodynamics: 2) conserved charges: 3) EoM:

1st law of thermodyn.

Euler/Navier-Stokes

curvilinear coordinates/Riemann space-time:


1) = control eq. (seldom constructive eq.)2) = local charge conservation3) = 4 eqs. for 4 components of

constitutive eqs.:

perfect fluid dissipation

What is flow? Choice of 4-velocity (3 independent components)

a) Eckart: flow of net chargeb) LL: flow of energy

LL condition:

t

x


even when neglecting dissipative effects: EoS is needed

p(e,n) or p(T,mu) or s(e,n) or ...

first-principle calculations (lattice QCD, large-T expans.)phenomenology, measurements

V, E, N_i: extensives e, n_iT, mu_i: intensivesentropy density s, pressure p ...

applicability of hydro: container > gradients

large enough


Tools (2): Thermodynamics

Gibbs-Duham:

Euler:

susceptibilities:

Taylor expansion (Bielefeld):


Example: Cosmic Confinementperfect fluid + cosmological principle

homogeneity + isotropy in 3D Robertson-Walker metric (coordinates)

Einstein eqs. expanding universe (matter cools and becomes dilute)

comoving volume

ES

ES

R(t1)

R(t2)


Friedmann eqs. EoS


Bag Model EoS: too simplepi

T

pqg

Tc

Gibbs criteria for phase equilibrium(maximum entropy)

p_qg = p_pi T_qg = T_pimu_qg=mu_pi

-p = free energy

1st order pt(nucleation,bubbles etc.)

p

T

e,s

T

mix

T

t10

Tc


Cosmic Swing (1): SIMfrom small mu to large mu

hadronization


Driving the Cosmic Swing: etamystery: 5year WMAP CDM

God given init. cond. or via baryogenesis (sphalerons)

specific entropy conserved:

T > Tc: relativistic quarks carry baryon numberT < Tc: non-relativistic nucleons carry baryon numberT ~ 45 MeV: annhilation of baryons, excess (~ eta) remains

why is baryon excess so small OR why is entropy so large?


B

B

disapparence of anti-matter (1)


Boltzmann approx.:

Densities

high/low temperature approx.:


Stretching of Distances

T = 170 MeV

5 m 1 fm100000 fm

1 fm

q

q

1 fm

g

1000 fm

q

T = 2.3 x 10 MeV-10

On average On Earth In nuclei & neutron stars

B B B


- cosmic confinement is too slow

- gradual matter conversion in qg h cross over- if confinement would be 1st order pt: bubble growth, supercooling, inhomogeneities

- uncertainty: neutrino degeneracy

Relics of Cosmic Confinement?

after 30 years research: none

Jenkowski, BK, Z. Phys. 1990


Primordial Nucleosynthesisthe first three minutes

four fundamental forces in concert: - gravity expansion of universe - electromagnetic e+ e- annihilation - weak neutrino decoupling - strong/nuclear cooking the leight elements: specific abundances for given cosmic expansion + reaction rates

charge neutrality:


e-, e+

e- - e+e-e+

e- - e+

e-, e+


e-


Big Bang e+ e- Annihilation

t ~ 0.3 s: neutrino decoupling

t ~ 15 s, T ~ 3 x 10^9 K: e+ e- annhilation

Kolb-Turner

disappearance of last antimatter in universeonly excess electrons survive „reheating“ of photons, nucleons

e-

e+


e+ e- Nano Droplets

Yaresko, Munshi, BK, Phys. Plasma 2010Munshi, BK, PRA 2009

first

est

ima

tes:

S

he

n,

Me

yer-

ter-

Ve

hn

, P

RE

65


The Universe as Reactor

Friedmann: T(t) from

D: baryometer4He: chronometer

only destruction after BNN


Primordial Nuclear Network

2. D, 4. 3He, 8. T, 6. 4He, 7. 7Li

Dominant Channels (strong int./QCD):


p

n

D T

He He

Be

Li

1

2

5

63 4 8

9

10

12

11

7

7

7

3 4

Nollett-Burles


Rate Equations for 2 2 Processes

rates (T)

Init. Conds.: earlier equilibrium values

add decays

integrate up to freeze-out

T(t)


Evolution of Abundances

D

Be

mass fraction


Cosmic Concordance?

new physics beyond Standard Model?Xdimensions, more neutrinos, axions, SUSY particles, G(t), ...


Neutron Life Time

nearly all n are in 4He: Y(4He) depends on(other abundances are robust) and also on

fastBBN

886.7869

904


Number of Light Neutrinos

3

3.5

2.5


Cosmic Interim Summary

Cosmic Confinement/Hadronization

T > Tc = 170 MeV, t < 10^-6 s: mu small, q + g T < Tc, t > 10^-6 s: hadrons emerge and decay, no relics T ~ 40 MeV: nucleons annihilate (up to the excess) no relics

Primordial Nucleosynthesis

concides with neutrino decoupling and e+ e- annihilation abundancies of light nuclei are sensitive to expansion history = relics

B. Kämpfer | Institut für Strahlenphysik | Hadronenphysik | Helmholtz-Zentrum Dresden-Rossendorf...

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