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The GZK Neutrinos
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Why UHE neutrinos matter?
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UHE neutrinos interact in the neutrino background
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The Cosmological Neutrino Background
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The Cosmological Neutrino Background II
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The Neutrino Darkmatter
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Thermal History of Universe
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Mean free path of the interactions
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Kinematics of the collision
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The representative channels
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Energy dist. of the cascading particles
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Hadron fragmentation in the produced jets
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Horizon of Universe with neutrinos
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Predicted UHE neutrino fluxes
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Concept of the Z-burst model
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Produced photons go into EM cascades
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Numerical Caluculation on the Z-burst model:
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The assumptions
-
Calculated Flux f=300
-
Cosmological and local component can make
contributions in different energy range.
-
Calculated Flux f=20
-
Some problems remain to be reslvoed
-
GRBs might provide a solution
The GZK Neutrinos
Why UHE neutrinos matter?
UHE neutrinos interact in the neutrino background
The Cosmological Neutrino Background
The Cosmological Neutrino Background II
The Neutrino Darkmatter
Thermal History of Universe
Mean free path of the interactions
Kinematics of the collision
The representative channels
Energy dist. of the cascading particles
Hadron fragmentation in the produced jets
Horizon of Universe with neutrinos
Predicted UHE neutrino fluxes
Concept of the Z-burst model
Produced photons go into EM cascades
Numerical Caluculation on the Z-burst model:
- The assumptions
- Calculated Flux f=300
- Cosmological and local component can make contributions in different energy range.
- Calculated Flux f=20
- Some problems remain to be reslvoed
- GRBs might provide a solution
