Comparison of Models of Nucleus-Nucleus Interactions in CORSIKA
Introduction to the study on models of hadronic interactions at high energies implemented in CORSIKA, a simulation tool used to analyze cosmic ray interactions with Earth's atmosphere. The study compares four widely used models, detailing their features and variants in simulation parameters. Results from simulations involving nitrogen-nitrogen interactions at different primary energy levels are presented, showing the mean number of particles produced by each model. The study aims to analyze the distribution of secondary nucleons and other particle types to understand the behavior of cosmic ray interactions.
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Comparison of models of nucleus-nucleus interactions implemented in CORSIKA Nikolaenko R.V., Bogdanov A.G., Kokoulin R.P., Petrukhin A.A. National Research Nuclear University MEPhI (Moscow Engineering Physics Institute) 1
Introduction Program CORSIKA (COsmic Ray SImulation for KAscade) is the most common tool for the simulation of the generation and development of extensive air showers as a result of interactions of cosmic rays with the atmosphere of Earth. Results of CORSIKA simulation are used by the laboratories all over the world to make the conclusions about the primary cosmic ray spectra and composition. CORSIKA supports the set of implemented models of hadronic interactions at high and low energies. The choice of the model to be used in simulation depends only on the decision of the user. Thus the comparison of these models is of interest. In this study we consider four most widely used models of hadronic interactions at high energies implemented in CORSIKA. 2
Models of hadronic interactions at high energies implemented in CORSIKA v.77402 Model (version) Features Dual Parton Model with soft chains and multiple minijets DPMJET-III (2017.1) Improved NEXUS features. LHC data is taken into account to constrain model parameters EPOS-LHC (v3400) Combines features of the former VENUS and QGSJET NEXUS (3.97) Pomeron parameterization for the elastic hadron-nucleon scattering amplitude QGSJET-01d Includes Pomeron loop and the cross-section is tuned to LHC data QGSJET-II-04 SIBYLL (2.3d) Based on the QCD mini-jet model Developed to simulate ultra- relativistic heavy ion collisions VENUS (4.12) 3
Variants of simulation parameters for each model: Only the first interaction of cosmic rays with the atmosphere is considered. Nitrogen was picked as the target nucleus. As the primary particles, protons and nuclei of helium, nitrogen and iron were chosen. Two values of primary energy: ?0= 1014?? and ?0= 1018??. Each simulation run includes 105 events. The simulation results are used to: Get the distributions of the number of particles of different types that were created in the interaction. Also mean values of their numbers are calculated. Determine the dependence of the fraction of the collision energy carried by different types of particles on the mass of the primary particle. Perform the check for the conservation laws violation when possible. 4
Nitrogen-nitrogen interactions, ?0= 1018?? Mean number of particles Particle type EPOS-LHC QGSJET-II-04 SIBYLL-2.3d DPMJET-III 4.7 0 7.4 1835 Neutral pions 144 296 73 0.02 Charged pions 295 571 137 1495 Neutral kaons 38.7 67.7 28.9 123 Charged kaons 39.7 68.1 28.9 125 Nucleons 33.6 41.3 38.6 115 Antinucleons 18.6 30.8 26.1 88.9 Nuclei (A 2) 0.37 1.42 1.03 0 5
The distributions of secondary nucleons number, iron-nitrogen interactions, ?0= 1018?? Neutrons Protons 6
The dependences of the fraction of the energy of interaction carried by secondary particles on the mass of primary particle ?0= 1014?? SIBYLL-2.3d EPOS-LHC 70 70 , 0 +, ??0, ??0 ?+, ? 60 60 50 50 E/E0, % E/E0, % 40 40 30 30 Vector mesons 20 20 Nucleons 10 10 Nuclei 0 0 1 4 14 56 1 4 14 56 ?0= 1018?? A (log scale) A (log scale) QGSJET-II-04 , 0 +, ??0, ??0 ?+, ? DPMJET-III 70 70 60 60 50 50 E/E0, % E/E0, % 40 40 Vector mesons 30 30 Nucleons 20 20 Nuclei 10 10 0 0 1 4 14 56 1 4 14 56 A (log scale) A (log scale) 7
Electric charge conservation For each case of projectile particle and its primary energy the ????value is calculated as the average sum of charges of all secondary particles in the stack. Assuming the exclusion of the target nucleus fragments in generators used in models, the ratio ?????????? ?? 1, where ??????is the total charge of the interaction. ???? E0 = 1018 eV E0 = 1014 eV 1.4 1.4 1.2 1.2 1.0 1.0 Qsum/Qtotal Qsum/Qtotal 0.8 0.8 0.6 0.6 EPOS-LHC QGSJET-II-04 SIBYLL-2.3d DPMJET-III EPOS-LHC QGSJET-II-04 SIBYLL-2.3d DPMJET-III 0.4 0.4 0.2 0.2 1 4 A (log scale) 14 56 1 4 A (log scale) 14 56 8
Conclusion 1. Comparison of four models of hadronic interactions has shown the following major differences: DPMJET-III is radically different from other models in terms of the mean numbers of created particles for practically all types of them. The number of secondary particles (mainly pions) can differ by 2-4 times between models, which consequently causes the difference in numbers of muons. The dependences of the fraction of the energy carried by secondary nucleons and nuclei on the mass of primary particle are similar for QGSJET-II-04 and SIBYLL-2.3d models, but the results for EPOS-LHC are vastly different from them. 2. The performed test for the implementation of the charge conservation law in models shows that there are some deviations from the total charge of the interacting nuclei in EPOS-LHC, QGSJET-II-04 and DPMJET-III models, which can be explained if the fragments of target nuclei with low energies are not taken into account. However, for SIBYLL-2.3d it directly indicates the violation of the charge conservation. 9
