1. Hadronic Interaction Model Analysis Air Shower Development
Comparison Of High Energy Hadronic Interaction Models
G. Battistoni, R. Ganugapati, A.Karle,J. L. Kelley, T. Montaruli
Zenith Angle Spectrum
Hadronic Interaction Model Analysis
The hadronic interaction models used in cosmic ray air shower Monte Carlo codes are built based on various theoretical scenarios. These can be checked by accelerator experiments up to collider energies but must be extrapolated to higher energies. The L3+C data (Private Communication, Ralph Engel) at lower energy shows that the the muon flux predicted using different interaction models can differ by up to 30%.
Differences of the model predictions when confronted with measurements are observed this could be due to differences in the Physics of Interaction models and how the extrapolations are made up to cosmic ray energies. Therefore more checking and improvements of the hadronic interaction models are necessary.
During the development of air showers, in the most forward region a large fraction of the collision energy is taken by the secondary particles. Here we show the Feynman-X distributions of various particle species (charged pions, kaons, and charmed particles) after the first interaction.
Detecting Extra-Terrestrial Neutrinos and understanding Atmospheric Neutrino/Muon Fluxes
Air Shower Development
The main backgrounds for the detection of extraterrestrial neutrino fluxes are the atmospheric muons and neutrinos produced from the interaction of cosmic rays with the atmosphere. The predicted atmospheric neutrino and muon fluxes depend on the models used to describe these interactions, and discrepancies become very large at higher energies. We have produced a detailed analysis of the interaction models.
Zenith Angle Spectrum of down going muons
From ICRC 2003 (Paolo Desiati ). The simulated data using the QGSJET interaction model is multiplied by 1.3 in this plot and excess of experimental data is observed at very large zenith angles and a possibility of charm cannot be discounted. The mismatch is studied in detail for several other Interaction models by investigating the number of mesons and baryons that are produced that decay subsequently into muons
Transverse Momentum Plot
10TeV Fixed Primary Energy
100TeV Fixed Primary Energy
1PeV Fixed Primary Energy
Pions
Kaons
Pions
Kaons
Pions
Kaons
Transverse Momentum (GeV)
Charm (Meson+Baryon)
Charm (Meson+Baryon)
Charm (Meson+Baryon)
Mean (MeV) RMS (MeV)
Pions
Kaons
Charm Meson
Charm Baryon
E/Eprimary>0
E/Eprimary>0.05
E/Eprimary>0.1
The plot shows lateral separation of down going muon tracks from the shower core at AMANDA depth for the hypothetical case of 1st interaction only and after the shower is developed for the case of conventional muons (Pions,kaons) and for the case prompt muons (Charmed particles) using the DPMJET interaction model for a fixed 1PeV energy primary and 65 degrees Zenith Angle
Z-Moment
Average Multiplicity
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