Prompt neutrino fluxes from atmospheric charm

By R. Enberg, M. Reno, I. Sarcevic. 2008

276 citations recorded by the source corpus.

We calculate the prompt neutrino flux from atmospheric charm production by cosmic rays, using the dipole picture in a perturbative QCD framework, which incorporates the parton saturation effects present at high energies. We compare our results with the next-to-leading order perturbative QCD result and find that saturation effects are large for neutrino energies above 10^6 GeV, leading to a substantial suppression of the prompt neutrino flux. We comment on the range of prompt neutrino fluxes due to theoretical uncertainties.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/55eec451d70f6af5ab8f37bb064d1dffa0d25262

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Nuclear and High Energy Physics

1. Kohta Murase
2. A. Fedynitch
3. Todor Stanev
4. S. Ando
5. I. Tamborra
6. W. Rhode
7. Silvia Adrián-Martínez
8. H. Haren

Citations in the corpus

• Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector (2013, methodology): “For scale, two specific charm levels are also shown: a benchmark theoretical model (6) (green line) and the experimental 90% CL upper bound (8) (magenta line).”
• Where are we with light sterile neutrinos? (2019, background): “[112] Rikard Enberg, Mary Hall Reno, and Ina Sarcevic.”
• A COMBINED MAXIMUM-LIKELIHOOD ANALYSIS OF THE HIGH-ENERGY ASTROPHYSICAL NEUTRINO FLUX MEASURED WITH ICECUBE (2015, methodology): “While the analysis favors the absence of a prompt atmospheric neutrino component, a contribution to the flux at the level of the prediction by Enberg et al. (2008) is still allowed and would not alter the spectrum of the astrophysical component significantly, as demonstrated in Figure 2.”
• Star-forming galaxies as the origin of diffuse high-energy backgrounds: gamma-ray and neutrino connections, and implications for starburst history (2014, background): “J C A P 0 9 ( 2 0 1 4 ) 0 4 3 neutrino background from the decay of charmed mesons are too low to have a significant contribution at PeV energies [38, 39].”
• KM3MeT 2.0 Letter of intent for ARCA and ORCA (2016, methodology): “35, has been obtained assuming the maximum and minimum flux values of the prompt atmospheric neutrino component reported in [19].”
• Letter of intent for KM3NeT 2.0 (2016, methodology): “For comparison the atmospheric neutrino fluxes are also reported (Honda flux [18] for the conventional component and the Enberg flux [19] for the prompt component, see section 3.”
• OBSERVATION AND CHARACTERIZATION OF A COSMIC MUON NEUTRINO FLUX FROM THE NORTHERN HEMISPHERE USING SIX YEARS OF ICECUBE DATA (2016, methodology): “2astro astro · ( ) The prompt neutrino flux is described by the prediction taken from Enberg et al. (2008) (ERS) where the absolute normalization Fprompt is taken as free parameter.”