Probing very high energy prompt muon and neutrino fluxes and the cosmic ray knee via underground muons

Abstract

We calculate event rates and demonstrate the observational feasibility of very high energy muons (1 TeV-1000 TeV) in a large mass underground detector operating as a pair-meter. This energy range corresponds to surface muon energies of ∼(5 TeV -5000 TeV) and primary cosmic ray energies of ∼ (50 TeV -5 ×10 4 TeV). Such measurements would significantly assist in an improved understanding of the prompt contribution to ν e , ν µ and µ fluxes in present and future ultra-high energy neutrino detectors. In addition, they would shed light on the origin of and possible compositional changes at and around the observed 'knee' in the cosmic ray spectrum.

https://www.omicsgroup.org/journals/combined-effects-of-radiation-and-oblateness-on-the-existence-and-stabilityof-equilibrium-points-in-the-perturbed-restricted-fourb-2329-6542-1000139.php?aid=88537

“…The differential pair production cross section can be calculated by taking some approximation of relative energy transfer and threshold energy is given by [4,5,12,13].…”

“…Uncontrollable fluxes have been produced, which is the major disadvantage of cosmic rays. The study of cosmic ray spectrum enhances our knowledge about both astrophysics and particle physics [1][2][3][4][5], and also gives a signature of the existence of the new particles and some physics behind it, which was confirmed by some accelerator experiments. These experiments provide us to understand the structure of matter and interaction between its building blocks.…”

The Physics Role and Potential of future Atmospheric Detectors

“…Its charge identification capability gives it an edge for hierarchy determination and CP, CPT studies. The high Z medium also allows a studies of very high energy cosmic-ray (CR) muons using the pair-meter method, allowing a probe of the CR flux at energies around the "knee" and beyond [20].…”

High-Energy Atmospheric Muon Flux Expected at India-Based Neutrino Observatory

“…1 Number of the muon events per steradian per year expected at INO detector near direction cos θ = 0.7 is presented in Table III (see details in Ref. [12]). Last three columns in Table III represent the ratio of the conventional muon flux to the prompt muon one due to three charm production models, GGV01, GGV05 and QGSM, respectively.…”