Abstract
Atmospheric neutrino and muon fluxes come from cosmic ray interactions with air nuclei. Prompt leptons from charmed particle decays dominate the conventional leptonic flux from pion and kaon decays at sufficiently high energies. The IceCube Collaboration has published a measurement of the atmospheric neutrino energy spectrum up to neutrino energies of 400 TeV where the prompt neutrino flux is potentially important. They also set limits on the diffuse astrophysical flux of neutrinos for which the atmospheric neutrino flux is a background. A brief discussion of charm pair production in the atmosphere, including dipole models and the parton model with fixed-order plus next-to-leading log corrections (FONLL) is presented. Ultimately, a range of theory predictions consistent with current accelerator constraints on the cross section is needed.
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