(Primordial Nucleosynthesis*)

B. Kämpfer

Research Center Rossendorf/Dresden & Technical University Dresden

- Expanding Universe- Prior to Nucleosynthesis- First Three Minutes: Creating Light Nuclei

* Based on Ms. of W. Wustmann, July 22, 2005

BBN

Albert Einstein, 14.03.1879-18.04.1955

1905:

- Über einen die Erzeugung und Verwandlung des Lichtes betreffenden heuristischen Gesichtspunkt- Die von der molekularkinetischen Theorie der Wärme geforderten Bewegung von in ruhenden Flüssigkeiten suspendierten Teilchen- Elektrodynamik bewegter Körper - Ist die Trägheit eines Körpers von seinem Energieinhalt abhängig?

1915:

Framework/Propositions

1. Einstein Equations Hold for Universe

2. Cosmological PrincipleHomogeneity & Isotropy of 3D

4. --> Friedmann Equations

3. Iso-entropic Expansion

Expanding Universe

larger e,p faster cooling:

Issues:

Nucleosynthesis: test of expansion dynamics

CMB: 300,000 years, Now:

Prior to Nucleosynthesis

1. Confinement: Hadrosynthesis

BK, Bluhm, 2005

2. Strongly Interacting Matterquarks

gluons

confinement

temperature evolution

strangeness evolution

strangeness changingweak interactions

3. Radiation Universe

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

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):

T < 1 MeV: e+ e- annihilation (QED) nu decoupling (e.w. int.)

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

doneT(t)

Survey on Data Nollett-Burles 2000

freeze-in all other parametersand consider only the impact of thisreaction

poor data samples:

Evolution of Abundances

D

Be

mass fraction

Cosmic Concordance?

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

WMAP: Precision Cosmology

time

BBN

Knowing only Photo Dissociation Data

Bisho

p 50

Shino

hara

49 de Graeve 92

Role of n(p,D)gamma

Knowing more Data

detailed balance:

Sn

p

D

error bars suppressed

EFT: the toolof strong interactionat low energiesadjusted to Cox 65

low energy:high energy:

N isovector mag. moment

Low Energy Data np D gamma

Bethe 49

data too scarce forprecision cosmology

new measurements at ELBEGrosse, Beyer & Co

„GamoW window“

FZ RossendorfELBEBremsstrahlung cave:

p

nD

1. D at rest: T_p, T_n

2. Superposition ofvarious beam energies thermal spectrum

A. Wagner

FZ RossendorfELBEnTOF cave

np

D

pulsed n source:

A. Junghans

1.E-02

1.E-01

1.E+00

1.E+01

1.E+02

1.E+03

1.E+04

1.E+05

1.E+06

1.E+07

1.E

-11

1.E

-10

1.E

-09

1.E

-08

1.E

-07

1.E

-06

1.E

-05

1.E

-04

1.E

-03

1.E

-02

1.E

-01

1.E

+00

1.E

+01

1.E

+02

En / MeV

Flu

x d

ensi

ty /

cm-2

s-1

No absorber5 cm PE + 5 mm Cd10 cm PE + 5 mm Cd2 mm PE + 0.5 mm Cd1 cm PE + 0.5 mm Cd

f = 1.6 MHzE = 210 keVt = 615 ns

J. Klug

Previous Measurements

Suzuki et al. 95:

Hara et al. 03:

Moreh et al. 89:

Nagai et al. 97:

Cokinos, Melkonian 77:

other exps.: M1 vs. E1

Xsection R factor Rate

ENDF

Using Rates in BBN123

5% lowering of 7Li (relative to SKM&EFT)

Sensitivity Function

measure here!

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

Conclusions

more data for gamma D n pat E_gamma <,= 2.32 MeV:pin down primordial 7Li abundancebelow a 5% level

more precise data for other reactions& more precise observational data: NEW PHYSICS?

BBN vs. CMB

Deviations of Data and SKM(5): R Factor

13%

WM

AP

885.7 sec878.5 sec

Mathews,Kajino,Shima 05 Steigman 05

9 o

rder

s o

f m

agn

itu

de

BBN with eta(WMAP)

Hel

ium

-4

mas

s fr

actio

n

eta from BBNadjusted to obs.

Metal-poorExtragalactic H II regions

Deuteron Abundance: Observations

BBN witheta_10=6.1

X = metallicity (O,Si)

Impact of Changed Xsections10%

change of rate