Hadronic interaction model sibyll2.3cand inclusive lepton fluxes

Abstract

Muons and neutrinos from cosmic ray interactions in the atmosphere originate from decays of mesons in air-showers. Sibyll-2.3c aims to give a precise description of hadronic interactions in the relevant phase space for conventional and prompt leptons in light of new accelerator data, including that from the LHC. Sibyll is designed primarily as an event generator for use in simulation of extensive air showers. Because it has been tuned for forward physics as well as the central region, it can also be used to calculate inclusive fluxes. The purpose of this paper is to describe the use of Sibyll-2.3c for calculation of fluxes of atmospheric leptons.

The hadronic interaction model Sibyll 2.3c and muon production in extensive air-showers

“…Its implementation in Sibyll 2.3c is based on comparison with recent accelerator data on production of charmed hadrons and fully supports the production of charm [23][24][25]. The model of the production of charm and the application of Sibyll 2.3c to the calculation of inclusive lepton fluxes is the subject of a separate paper [25]. This paper on Sibyll 2.3c 1 and EAS has two main topics: § II introduces the changes to the microscopic interaction model; § III shows the impact of these changes on EAS observables and benchmarks the new models against other contemporary post-LHC models [28,29] and the previous Sibyll 2.1.…”

Searches for atmospheric long-lived particles

“…where R ⊕ 6370km is the Earth radius. In our calculations, we have used the Matrix Cascade Equation (MCEq) Monte Carlo software [20,21] to compute the fluxes for the parent mesons and protons in the atmosphere, with the SYBILL-2.3 hadronic interaction model [22], the Hillas-Gaisser cosmic-ray model [23] and the NRLMSISE-00 atmospheric model [24]. With this procedure, meson and proton fluxes are obtained as a function of X, E and cos θ (see Appendix B for details).…”

“…In all our calculations, the SM parent particle fluxes in the atmosphere have been computed using the MCEq software [20,21], with the SYBILL-2.3 hadronic interaction model [22], the Hillas-Gaisser cosmic-ray model [23] and the NRLMSISE-00 atmospheric model [24]. Obtaining the parent particle fluxes is however not straightforward, because only the flux for protons and unstable particles that are relatively long-lived compared to their interaction length can be directly extracted using MCEq.…”

Prompt atmospheric neutrinos in the quark–gluon string model

“…The calculation is based on the hadronic cascade model [15,20,21] and cross sections of D meson and Λ + c baryon production in pA-and πA-collisions which are computed with the updated QGSM. We compare our result with the constraint obtained in the IceCube experiment [1] as well as with predictions of the color dipole model (ERS) [22], SIBYLL 2.3c [23], the NLO pQCD models, BEJKRSS [24] and GRRST [25].…”