BBN Primordial Nucleosynthesis B Kmpfer Research Center RossendorfDresden

BBN (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

1915: 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?

Framework/Propositions 1. Einstein Equations Hold for Universe 2. Cosmological Principle Homogeneity & Isotropy of 3 D 3. Iso-entropic Expansion 4. --> Friedmann Equations

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 changing weak interactions

3. Radiation Universe

Stretching of Distances T = 170 Me. V g q q q 1 fm 1000 fm -10 T = 2. 3 x 10 Me. V B 5 m On average B 100000 fm On Earth B 1 fm In nuclei & neutron stars

The Universe as Reactor Friedmann: T(t) from D: baryometer 4 He: chronometer only destruction after BNN

Primordial Nuclear Network Dominant Channels (strong int. /QCD): 2. D, 4. 3 He, 8. T, 6. 4 He, 7. 7 Li T < 1 Me. V: e+ e- annihilation (QED) nu decoupling (e. w. int. )

7 Be 12 7 10 11 3 He 3 4 p 2 D 9 8 5 4 He 7 6 T 1 n Nollett-Burles Li

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

Survey on Data Nollett-Burles 2000

poor data samples: freeze-in all other parameters and consider only the impact of this reaction

Evolution of Abundances D mass fraction Be

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

WMAP: Precision Cosmology time BBN

Bi Sh sho ino p 5 ha 0 ra 49 Role of n(p, D)gamma Knowing only Photo Dissociation Data de Graeve 92

Knowing more Data D n p S detailed balance:

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

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

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

FZ Rossendorf ELBE n. TOF cave A. Junghans D n p pulsed n source: J. Klug

Previous Measurements Hara et al. 03: Nagai et al. 97: Suzuki et al. 95: Moreh et al. 89: Cokinos, Melkonian 77: other exps. : M 1 vs. E 1

Xsection R factor Rate ENDF

Using Rates in BBN 123 5% lowering of 7 Li (relative to SKM&EFT)

Sensitivity Function measure here!

Neutron Life Time nearly all n are in 4 He: Y(4 He) depends on (other abundances are robust) and also on 904 886. 7 869 fast. BBN

Number of Light Neutrinos 2. 5 3 3. 5

Conclusions more data for gamma D n p at E_gamma <, = 2. 32 Me. V: pin down primordial 7 Li 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%

Helium-4 mass fraction 885. 7 sec 878. 5 sec Metal-poor Extragalactic H II regions BBN with eta(WMAP) Mathews, Kajino, Shima 05 9 orders of magnitude WMAP eta from BBN adjusted to obs. Steigman 05

Deuteron Abundance: Observations BBN with eta_10=6. 1 X = metallicity (O, Si)

Impact of Changed Xsections 10% change of rate