Search for the Cosmic Neutrino Background and the Nuclear Beta Decay (KATRIN). Amand Faessler University of Tuebingen Germany Publication: Amand Faessler, Rastislav Hodak, Sergey Kovalenko, Fedor Simkovic: arXiv: [nucl-th] 20. April 2013.

Cosmic Microwave Background Radiation (Photons in the Maximum 2 mm) Decoupling of the photons from matter about years after the Big Bang, when the electrons are captured by the protons and He4 nuclei and the universe gets neutral. Photons move freely.

Penzias and Wilson; BellTelephon Nobel Price 1978 Microwave Background Radiation

4 (2002) Temperature-Fluctuations of the Cosmic Microw.-Background: 1/ COBE  WMAP COBE = Cosmic Background Explorer WMAP = Wilkinson Microwave Anisotropy Probe 2001

Planck Satellite Temperature Fluctuations Comic Microwave Background (March )

6 Curvature of the Univers flat xxx We know the size of the hot spots.

The Universe is flat. The density has the critical value:  = We can only see till the sphere of the the last photon- electron scattering: ~14 x10 12 light years

Black body radiation. Temperature adjusted (pdg 2012): T=2.7255(6) K Experiment Microwave Background Radiation T = (6) Kelvin

The relative number abundance of the light nuclei formed in the big bang allows to determine the absolute baryon density and relative to the critical density (flat universe).  Baryon =  Baryon /  critical = 0.02h -2 = 0.04 n B = 0.22 m -3 e B = 210 MeV/m -3 h = 0.71 h 2 = 0.5 Hubble-Konstant= H = 100 h [km/(sec Mpc)]  B h 2 = 0.02 h = 0.71

Planck‘s Black Body Radiation

Photons and Neutrinos   e,  W

Decoupling of Photons and Neutrinos from Matter „Re“-combination of Electrons with Protons and  -Particles (1  out of 1.7x10 9 from upper tail)  3000 Kelvin; years after Big Bang; e- + p  neutral Hydrogen-Atom 2e- +   neutral Helium-Atom Photons move freely since 14x10  years. Last sphere of scattering: Radius = 14x10 12 light years. Today T  = (6) Kelvin independent of the direction.

Neutrino Decoupling and Cosmic Neutrino Background For massless-massive Neutrinos:

Temperature of Photons and Neutrinos The Neutrinos decouple before the Photons due to te weak interaction at about: T decoupl (Neutrinos) ~ 1 MeV ~ [Kelvin] T decoupl (Photons) ~ 0.3 [eV] ~ 3000 [Kelvin] Entropy ~ g i x T i 3 = g f T f 3 = const e‘s + Photons: g i = 4x(7/8) +2 = 11/2; Photons only: g f = 2 g f /g i = 4/11 = (T i= /T f ) 3 = ( T /(T f = 2.725)) 3  T (today) = (4/11) 1/ = 1.95 Kelvin

Estimate of Neutrino Decoupling Universe Expansion rate: H=(da/dt)/a  Interaction rate:  n e-e+ H = \sqrt{8  G  total /3} = \sqrt{8   /(3 M Planck 2 )}[1/time]  ~ T 3 = T 3 G F 2 T 2 = G F 2 T 5 [Energy = 1/time] hbar = h/(2  ) = c = 1

Neutrino Decoupling   /H = ( k B T/ 1MeV) 3 ~ 1 T(Neutrinos) decoupl ~ 1MeV ~ Kelvin; today: 1.95 K Time after Big Bang: 1 Second T(Photons) decoupling = 3000 Kelvin; today: K Time(Photons) decoupling = years Below T = 1 MeV:

(Energy=Mass)-Density of the Universe log  a(t)~1/T Matter dominated:  ~ 1/a 3 ~ T 3 Dark Energy 1/Temp 1 MeV 1sec  dec. 1 eV 3x10 4 y today 3000 K y  dec. 8x10 9 y  K 1.95 K

Hamburg, March (Bild) Results from Oscillations: No Hierarchy, no absolute Mass Scale Fogli, Lisi, Marrone, Palazzo: Phys. Rev. D86 (2012)

Hamburg, March Tranformation from Mass to Flavor Eigenstates

Mass of the Electron Neutrino? Tritium decay (Mainz + Troisk) With: Hamburg, March

Measurement of the upper Limit of the Neutrino Mass in Mainz: m < 2.2 eV 95% C.L. Kurie-Plot Q = keV m 2 >0 m 2 <0 Electron Energy Eur. Phys. J. C40 (2005) 447

Negatives Squares of the Measured Neutrino Masses Ch. Kraus, B. Bornschein, L. Bornschein, J. Bonn, B. Flatt, A. Kovalik, B. Ostrick, E. W. Otten, J. P. Schall, Th. Thümmler, Ch Weinheimer: Eur. Phys. J. C40 (2005)

relic D GZK =50Mpc Neutrino E = 4x10 22 eV Energy Momentum conservation: 1 (GZK,4x10 22 eV) + 2 (CB)  Z 0 (4x10 22 eV)burst  10  0, 2 nucleons, 17  +- Anihilation of Relic Neutrinos with extreme High Energy Neutrinos > eV Z0Z0 Above GZK Anihilation below Greisen-Zatsepin-Kuzmin Radius of 50 Mpc

Cosmic Radiation from Z-Burst expected at eV

Free magnetic floating cylinder with half  absorbing material Permanent Magnet Superconducting Magnet Cylinder shaped One half  absorbing, the other sterile. Balanced. The system rotates 90 degrees. Thomas Müller pointed this out to me. A. Ringwald: arXiv:hep- ph/031157v1; 2003.

Search for Cosmic Neutrino Background C B by Beta decay: Tritium Kurie-Plot of Beta and induced Beta Decay: (CB ) + 3 H(1/2 + )  3 He (1/2 + ) + e - Electron Energy 2xNeutrino Masses Emitted electron Q = keV Infinite good resolution Resolution Mainz: 4 eV  m < 2.3 eV Resolution KATRIN: 0.93 eV  m < 0.2 eV 90% C. L. Fit parameters: m 2 and Q value meV Additional fit: only intensity of C B

Search for Cosmic Neutrino Background C B by Beta decay: 187 Re Kurie-Plot of beta and induced beta Decay: (CB ) Re 112 (5/2 + )  Os 111 (1/2 - ) + e - Electron Energy 2xNeutrino Masses Emitted electron Q = keV Infinite good resolution MARE-Genova:  E ~ 11 eV  m ~ 2 eV Milano-Bicocca:  E ~24 eV  m ~ 3-4 eV Fit parameters: m 2 and Q value meV Additional fit: only intensity of C B

28 Solution of the Nuclear Structure Problem: Pairing Quasi-Boson Approximation

Tritium Beta Decay: 3 H  3 He+e - + c e

Neutrino Capture: (relic) + 3 H  3 He + e - 20  g(eff) of Tritium  2x10 18 T 2 -Molecules: N capture(KATRIN) = 1.7x10 -6 n / [year -1 ] Every years a count!! for = 56 cm -3

Beta-Decay Re 112  Os 111 +e - + c e

Capture: e (relic) Re(5/2) +  Os(1/2) - + e grams of AgReO 4  N capture(MARE) = 6.7x10 -8 n / [year -1 ] Every 15 Million years a count!!! Main Contribution:  s(1/2); e -  p(3/2)

Kurie-Plot Electron Energy 2xNeutrino Masses Emitted electron Resolution KATRIN: 0.93 eV  m < 0.2 eV 90% C.L. Fit parameters: m 2 and Q value meV Additional fit: only intensity of C B Two Problems 1.Number of Events with average Neutrino Density of n e = 56 [ Electron-Neutrinos/cm -3 ] Katrin: 1 Count in Years Gravitational Clustering of Neutrinos!!!??? 2. Energy Resolution (KATRIN)  E ~ 0.93 eV

Gravitational Clustering of Dark Matter and Neutrinos in Galaxies Was kompensiert die Zentrifugalkraft? Dunkle Materie ? Faktum erwartet

Gravitational Clustering of Neutrinos A. Ringwald, Y. Wong: arXiv:hep-ph/ ; solved Vlasov eq. for ; Dark Matter from Navarro et al. Ap J490 (1997) 493 Circles: 1h -1 kpc; Pentagons: 10h -1 kpc; Squares: 100h -1 kpc; Triangles 1000h -1 kpc. h -1 = 2 The solar system is 8 kpc = ly from the galactic center. Virial Mass: M vir = 5v2R/G; v = velocity in sight

Gravitational Clustering of Neutrinos R.Lazauskas,P. Vogel and C.Volpe, J. Phys.g. 35 (2008) ; Light neutrinos: Gravitate only on Mpc (Galaxy Cluster) scale: n / ~ n b / ~ 10 3 – 10 4 ; = cm -3 A. Ringwald and Y. Wong: Vlasov trajectory simulations  Clustering on Galactic Scale possible n / = n b / ~ 10 6 ; (R = 30 kpc) N capture(KATRIN) = 1.7x10 -6 n / (year -1 ) = 1.7 [counts per year] Effective Tritium Source: 20 microgram  2 milligram N capture(KATRIN*) = 1.7x10 -4 n / (year -1 ) = 170 [counts per year]

Summary 1 The Cosmic Microwave Background allows to study the Universe year after the BB. The Cosmic Neutrino Background 1 sec after the Big Bang (BB): T (today) = 1.95 Kelvin. Extremly difficult to detect: Small Cross Section and low Density 56 ‘s/cm 3 and low Energies (1.95 Kelvin = 2x10 -4 eV).

2xNeutrino Masses Emitted electron Resolution KATRIN: 0.93 eV  m < 0.2 eV 90% C.L. Fit parameters: m 2 and Q value meV Additional fit: only intensity of C B Kurie-Plot Electron Energy Summary 2 1.Average Density: n e = 56 [ Electron-Neutrinos/cm -3 ] Katrin: 1 Count in Years Gravitational Clustering of Neutrinos n / < 10 6  1.7 counts per year (2 milligram 3 H  170 per year) 2. Measure only an upper limit of n ENDE