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(Primordial Nucleosynthesis*)

(Primordial Nucleosynthesis*). B. Kämpfer. Research Center Rossendorf/Dresden & Technical University Dresden. BBN. - Expanding Universe - Prior to Nucleosynthesis - First Three Minutes: Creating Light Nuclei. * Based on Ms. of W. Wustmann, July 22, 2005. 1915:.

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(Primordial Nucleosynthesis*)

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  1. (Primordial Nucleosynthesis*) B. Kämpfer Research Center Rossendorf/Dresden & Technical University Dresden BBN - Expanding Universe - Prior to Nucleosynthesis - First Three Minutes: Creating Light Nuclei * Based on Ms. of W. Wustmann, July 22, 2005

  2. 1915: Albert Einstein, 14.03.1879-18.04.1955 • - 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? 1905:

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

  4. Expanding Universe larger e,p  faster cooling: Issues: Nucleosynthesis: test of expansion dynamics CMB: 300,000 years, Now:

  5. Prior to Nucleosynthesis 1. Confinement: Hadrosynthesis BK, Bluhm, 2005

  6. 2. Strongly Interacting Matter quarks gluons confinement

  7. temperature evolution strangeness evolution strangeness changing weak interactions

  8. 3. Radiation Universe

  9. g q q q 1000 fm 5 m 1 fm 100000 fm 1 fm 1 fm -10 T = 2.3 x 10 MeV Stretching of Distances T = 170 MeV B B B Dark Matter In nuclei & neutron stars On average On Earth

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

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

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

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

  14. Survey on Data Nollett-Burles 2000

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

  16. Evolution of Abundances D mass fraction Be

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

  18. WMAP: Precision Cosmology time BBN

  19. Role of n(p,D)gamma Knowing only Photo Dissociation Data de Graeve 92 Bishop 50 Shinohara 49

  20. Knowing more Data D n S p detailed balance:

  21. Low Energy Datanp  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

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

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

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

  25. Nagai et al. 97: Hara et al. 03: Moreh et al. 89: Previous Measurements Suzuki et al. 95: Cokinos, Melkonian 77: other exps.: M1 vs. E1

  26. Xsection  R factor  Rate ENDF

  27. Using Rates in BBN123 5% lowering of 7Li (relative to SKM&EFT)

  28. Sensitivity Function measure here!

  29. Neutron Life Time nearly all n are in 4He: Y(4He) depends on and also on (other abundances are robust) 904 886.7 869 fastBBN

  30. Number of Light Neutrinos 2.5 3 3.5

  31. 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? Tensions in BB Model? BBN vs. CMB

  32. Deviations of Data and SKM(5): R Factor 13%

  33. 885.7 sec 878.5 sec Metal-poor Extragalactic H II regions BBN with eta(WMAP) Helium-4 mass fraction eta from BBN adjusted to obs. 9 orders of magnitude WMAP Mathews,Kajino,Shima 05 Steigman 05

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

  35. Impact of Changed Xsections 10% change of rate

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