Fluxes of atmosperic leptons

Dmitry Chirkin

UC Berkeley

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:

cos* correction• primary interaction depth depends weakly on energy, at 1 TeV is ~ 85 g/cm2

Definition of critical energy:

Approximation for flat isothermal atmosphere

at zenith angles

above

isothermal approx:

result:

Parameterizations

quantities are weighted with

Parameterizations

Muon energy losses

decay:

Fits to muon flux

Zenith angle dependence

From LVD paper (2000)

Integrated muon flux

Result dependence on the fitted region

Nutrino fluxes

Results

Muon charge ratioNeutrino charge ratio

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