Download - Fluxes of atmosperic leptons
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Fluxes of atmosperic leptons
Dmitry Chirkin
UC Berkeley
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Formula from Gaisser
• works for the flat atmosphere• gives muon flux at the point of production, to describe flux on the surface, need to correct for:• muon energy losses• muon decay
pion and kaon critical energies:
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cos* correction• primary interaction depth depends weakly on energy, at 1 TeV is ~ 85 g/cm2
Definition of critical energy:
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Approximation for flat isothermal atmosphere
at zenith angles
above
isothermal approx:
result:
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Parameterizations
quantities are weighted with
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Parameterizations
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Muon energy losses
decay:
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Fits to muon flux
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Zenith angle dependence
From LVD paper (2000)
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Integrated muon flux
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Result dependence on the fitted region
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Nutrino fluxes
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Results
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Muon charge ratioNeutrino charge ratio
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Conclusions
• cos* correction is important at zenith angles above 70o
• Muon energy losses and decay are important for flux description in the whole range of zenith angles
• Muon fluxes, muon and neutrino charge ratios produced with CORSIKA+QGSJET disagree with other calculations