1. Fluxes of atmosperic leptons
Dmitry Chirkin
UC Berkeley

2. pion and kaon critical energies:
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:

3. cos* correction
primary interaction depth depends weakly on energy, at 1 TeV is ~ 85 g/cm2
Definition of critical energy:

4. Approximation for flat isothermal atmosphere
at zenith angles
above
isothermal approx:
result:

5. Parameterizations
quantities are weighted with

6. Parameterizations

7. Muon energy losses
decay:

8. Fits to muon flux

9. Zenith angle dependence
From LVD paper (2000)

10. Integrated muon flux

11. Result dependence on the fitted region

12. Nutrino fluxes

13. Results

14. Muon charge ratio
Neutrino charge ratio

15. 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