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 ratio
Neutrino 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 CORSIKAQGSJET disagree with other
  calculations