(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, : - 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 Principle Homogeneity & 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 Matter quarks gluons confinement

temperature evolution strangeness evolution strangeness changing weak interactions

3. Radiation Universe

Stretching of Distances T = 170 MeV 5 m1 fm fm1 fm q q g 1000 fm q T = 2.3 x 10 MeV -10 On averageOn Earth In nuclei & neutron stars BBB

The Universe as Reactor Friedmann: T(t) from D: baryometer 4He: 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 DT He Be Li Nollett-Burles

Rate Equations for 2  2 Processes rates (T) Init. Conds.: earlier equilibrium values add decays integrate up to freeze-out done T(t)

Survey on Data Nollett-Burles 2000

freeze-in all other parameters and consider only the impact of this reaction 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 Bishop 50 Shinohara 49 de Graeve 92 Role of n(p,D)gamma

Knowing more Data detailed balance: S n p D

error bars suppressed EFT: the tool of strong interaction at low energies adjusted to Cox 65 low energy: high energy: N isovector mag. moment Low Energy Data np  D gamma Bethe 49

data too scarce for precision cosmology new measurements at ELBE Grosse, Beyer & Co „GamoW window“

FZ Rossendorf ELBE Bremsstrahlung cave: p n D 1. D at rest: T_p, T_n 2. Superposition of various beam energies  thermal spectrum A. Wagner

FZ Rossendorf ELBE nTOF cave n p D pulsed n source: A. Junghans 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

Number of Light Neutrinos

Conclusions more data for gamma D  n p at E_gamma <,= 2.32 MeV: pin down primordial 7Li abundance below 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%

WMAP sec sec Mathews,Kajino,Shima 05 Steigman 05 9 orders of magnitude BBN with eta(WMAP) Helium-4 mass fraction eta from BBN adjusted to obs. Metal-poor Extragalactic H II regions

Deuteron Abundance: Observations BBN with eta_10=6.1 X = metallicity (O,Si)

Impact of Changed Xsections 10% change of rate