Fluxes of atmosperic leptons
description
Transcript of Fluxes of atmosperic leptons
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