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Abstract
Sibyll is one of the first microscopic interaction models that was specifically developed for interpreting cosmic ray data. It combines non-perturbative concepts of simulating hadronic particle production with predictions derived from perturbative QCD calculations, focusing on forward particle production of relevance in studying cosmic ray interactions. In this contribution we briefly recall the history of Sibyll and then, in this context, describe improvements made in the different versions of the Sibyll model. The discussion focuses on the basic concepts and ideas of these improvements rather than going into detail or giving a comprehensive description of the models. We also discuss shortcomings, conceptual problems, and uncertainties in modeling hadronic interactions and make some suggestions how to address these open questions in the future.
Highlights
Sibyll is one of the first microscopic interaction models that was developed for interpreting cosmic ray data
It combines non-perturbative concepts of simulating hadronic particle production with predictions derived from perturbative Quantum Chromodynamics (QCD) calculations, focusing on forward particle production of relevance in studying cosmic ray interactions
In the early days of cosmic ray physics the measurements of inclusive fluxes and air showers were compared to analytic and semi-analytic calculations to derive information on the energy of the primary particles, their flux, composition, and to learn about general features of hadronic multiparticle production
Summary
In the early days of cosmic ray physics the measurements of inclusive fluxes and air showers were compared to analytic and semi-analytic calculations to derive information on the energy of the primary particles, their flux, composition, and to learn about general features of hadronic multiparticle production. Today a variety of dedicated program packages is publicly available for calculating the results of cosmic ray interactions in the atmosphere These include programs in which Monte Carlo generated tables of hadronic interactions are used to numerically solve cascade equations (for example, MCEq [8]), programs in which the Monte Carlo method is combined with numerical solutions of cascade equations (for example, SENECA [9] and CONEX [10]), and fully Monte Carlo based programs (for example, AIRES [11, 12], CORSIKA [13], and COSMOS [14]). With time the complexity of hadronic interaction models increased quickly and we have very sophisticated and powerful Monte Carlo event generators available.
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