Fluxes of atmosperic leptons

1. Fluxes of atmosperic leptons Dmitry Chirkin UC Berkeley

2. 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