i want thank aldo covello for the 11 spring seminars on nuclear physics in nice areas of the...
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I want thank
Aldo Covello for the 11 Spring Seminars
on Nuclear Physics in nice areas of the Sorrento Peninsula and the Islands.
I was participating in 7 of them.
At places like: Sorrento, Ischia, Capri, Amalfi, Ravello, Paestum
Thanks go also to Angela Gargano and coorganizers for
the organisation of the 11th. Meeting.
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Search for the Cosmic Neutrino Background
Amand Faessler, Ischia 15. May 2014
With thanks to: Rastislav Hodak, Sergey Kovalenko, Fedor Simkovic;Publication: arXiv: 1304.5632 [nucl-th]
11. Dec. 2013.
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1) Cosmic Microwave Background Radiation
2) Cosmic Neutrino Background
3) Cosmic Gravitational Wave Background
1) Decoupling of the photons from matter about 380 000 years after the Big Bang, when the electrons are captured by the protons and He4 nuclei and the universe gets neutral. Photons move freely.
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Planck Satellite Temperature FluctuationsComic Microwave Background (Release March 21. 2013)
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Fingerprint of the Gravitational Waves of the Inflationary Expansion
of the Big Bang in the Cosmic Background Radiation.
On 18. March 2014 the BICEP2 Collaboration published in the arXiv:
1403.3985v2 [astro-ph.CO]
Gravitational Waves are Quadrupole Oscillations of Space not in Space.
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BICEP2 Detector at the South-Pole
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1.5 to 4 degrees;
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2) Estimate of Neutrino Decoupling
Universe Expansion rate: H=(da/dt)/a ~ n Interaction rate: = G ne-e+<svrelative>
H = = O( T2) [1/time]
G ~ (1/a3) <GF2 p2 c=1> ~ T3 <GF
2 T2c=1> ~ GF2 T5 [1/time]
with: Temperature = T ~ 1/a = 1/(length scale); = h/(2p) = c = 1
Stefan-Boltzmann
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(Energy=Mass)-Density of the Universe
log r
a(t)~1/T
Radiation dominated: r ~ 1/a4 ~ =Stefan-Boltzmann
Matter dominated: r ~ 1/a3 ~ T3
Dark Energy
1/Temp1 MeV~1sec n
dec.
1 eV5x104y today
3000 K380 000 yg dec.
8x109 y g 2.7255 Kn 1.95 K
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How can one detect the Cosmic Neutrino Background?
Electron-Neutrino capture on Tritium.
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3. Search for Cosmic Neutrino Background CnB by Beta decay: TritiumKurie-Plot of Beta and induced Beta Decay: n(CB) + 3H(1/2+) 3He (1/2+) + e-
Electron Energy
2xNeutrino Masses
Emitted electron
Q = 18.562 keV
Infinite good resolution
Resolution Mainz: 4 eV mn < 2.3 eV
Resolution KATRIN: 0.93 eV mn < 0.2 eV 90% C. L.
Fit parameters: mn
2 and Q value meVAdditional fit: only
intensity of CnB
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Tritium Beta Decay: 3H 3He+e-+nc
e
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Neutrino Capture: n(relic) + 3H 3He + e-
20 mg(eff) of Tritium 2x1018 T2-Molecules: Nncapture(KATRIN) = 1.7x10-6 nen/<nen> [year-1]Every 590 000 years a count! for <nen> = 56 cm-3
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Problem: 56 e-Neutrinos cm-3 too small
• Gravitational Clustering of Neutrinos estimated by Y. Wong, P. Vogel et al.:
nne(Galaxy) = 106*<nne> = 56 000 000 cm-3
1.7 counts per yearIncrease th source strength: 20 micrograms 2 milligrams
170 counts per year every second day a countSpeakers of KATRIN: Guido Drexlin and Christian Weinheimer
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20 microgram 2 milligram Tritium
• Such an Increase of the Tritium Source Intensity is
with a KATRIN Type Spectrometer is difficult,
if not impossible!
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Three important Requirements:
1) The Tritium Decay Electrons are not allowed to scatter with the Tritium Gas.
2) The Magnetic Flux must be conserved in the whole Detection System.
3) The Energy resolution must be of the order of 1 eV.
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Source
1) The decay electrons should not scatter by the Tritium gas.
Beam
Column length dBase 1 cm2
Tritium Gas
Number of Tritium-Atoms in Column d = Column-Density
Magnetic Field3.6 Tesla
Optimal Column Density slightly below r*dfree /2Troitsk: 30%; Mainz: 40%; KATRIN: 90%
Only 36% have not scattered
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2) Conservation of Magnetic Flux
If one cant increase the intensity per area, increase the area by factor 100 from 53 cm2 to 5000 cm2.
Magnetic Flux: (Ai=5000 cm2) x (Bi=3.6 Tesla) =
18 000 Tesla cm2 = Af x (3 Gauss);Af = 6 000 m2 diameter = 97 meters
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3) Energy resolution of DE~ 1 eV
Energy resolution: Ef(perpend.) = Efp = DE
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Angular Momentum of the Spiraling Electrons must be conserved
Energy resolution: Ef(perpend.) = Efp = DE = 1 eV
L = |r = m const = L ~ []i =[ Bf = 3 Gauss
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20 microgram 2 milligram Tritium
• Such an Increase of the Tritium Source Intensity with a KATRIN Type Spectrometer is difficult,
if not impossible.
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Summary 1• The Cosmic Microwave Background allows to
study the Universe 380 000 years after the BB.
• The Cosmic Neutrino Background 1 sec after the Big Bang (BB).
• The Cosmic Background of Gravitational Waves 10-31 Seconds in the Big Bang
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2xNeutrino Masses
Emitted electron
Kurie-Plot
Electron Energy
Summary 2: Cosmic Neutrino Background
1. Average Density: nne = 56 [ Electron-Neutrinos/cm-3] Katrin: 1 Count in 590 000 Years Gravitational Clustering of Neutrinos nn/<nn> < 106
and 20 micrograms Tritium 1.7 counts per year. (2 milligram 3H 170 counts per year. Impossible ?)2. Measure only an upper limit of nn
THE END