Charm production in DPMJET

Berghaus, P.; Montaruli, T.; Ranft, J.

doi:10.1088/1475-7516/2008/06/003

Cited by 20 publications

(20 citation statements)

References 31 publications

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“…QGSJET and DPMJET [87] are slow, and charm production in QGSJET is very small compared to theoretical predictions. The core CORSIKA propagator does not handle re-interaction effects for heavy hadrons, which become important at energies approaching 10 PeV.…”

Section: Appendix A2 Construction Of Energy Observablementioning

confidence: 83%

“…The repartition between the two components at a given energy can therefore be measured from the angular distribution alone. The effect of higher order terms, such as departure of the angular distribution from a pure sec θ zen dependence due to the curvature of the Earth and deviations of the nucleon spectrum from a simple power law, have been estimated as less than 10% using a full DP-MJET [87] simulation of the prompt component.…”

Section: Angular Distributionmentioning

confidence: 99%

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Characterization of the atmospheric muon flux in IceCube

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Astroparticle Physics

101

117

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Muons produced in atmospheric cosmic ray showers account for the by far dominant part of the event yield in large-volume underground particle detectors. The IceCube detector, with an instrumented volume of about a cubic kilometer, has the potential to conduct unique investigations on atmospheric muons by exploiting the large collection area and the possibility to track particles over a long distance. Through detailed reconstruction of energy deposition along the tracks, the characteristics of muon bundles can be quantified, and individual particles of exceptionally high energy identified. The data can then be used to constrain the cosmic ray primary flux and the contribution to atmospheric lepton fluxes from prompt decays of short-lived hadrons.In this paper, techniques for the extraction of physical measurements from atmospheric muon events are described and first results are presented. The multiplicity spectrum of TeV muons in cosmic ray air showers for primaries in the energy range from the knee to the ankle is derived and found to be consistent with recent results from surface detectors. The single muon energy spectrum is determined up to PeV energies and shows a clear indication for the 2 emergence of a distinct spectral component from prompt decays of short-lived hadrons. The magnitude of the prompt flux, which should include a substantial contribution from light vector meson di-muon decays, is consistent with current theoretical predictions.The variety of measurements and high event statistics can also be exploited for the evaluation of systematic effects. In the course of this study, internal inconsistencies in the zenith angle distribution of events were found which indicate the presence of an unexplained effect outside the currently applied range of detector systematics. The underlying cause could be related to the hadronic interaction models used to describe muon production in air showers.

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Section: Appendix A2 Construction Of Energy Observablementioning

confidence: 83%

Section: Angular Distributionmentioning

confidence: 99%

Characterization of the atmospheric muon flux in IceCube

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Astroparticle Physics

101

117

View full text Add to dashboard Cite

show abstract

“…These events come exclusively from the southern sky because muons cannot penetrate the bulk of the Earth, and are sharply peaked at the deposited-energy threshold of the selection because the veto removes muons with increasing efficiency at higher energies. The flux model for penetrating atmospheric muons is taken from a parametrization of corsika [77] air-shower simulations with the cosmic ray flux parameterization of [76], using the sum of muons from the decays of light hadrons predicted in sibyll [78] and from the decays of charmed hadrons predicted in dpmjet [79] to obtain an upper bound on the underground flux of single muons. This combined model predicts a total of 14 penetrating muon events in the sample.…”

Section: Analysis Methodsmentioning

confidence: 99%

Atmospheric and astrophysical neutrinos above 1 TeV interacting in IceCube

Aartsen¹,

Ackermann²,

Adams³

et al. 2015

Phys. Rev. D

269

238

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The IceCube Neutrino Observatory was designed primarily to search for high-energy (TeV-PeV) neutrinos produced in distant astrophysical objects. A search for 100 TeV neutrinos interacting inside the instrumented volume has recently provided evidence for an isotropic flux of such neutrinos. At lower energies, IceCube collects large numbers of neutrinos from the weak decays of mesons in cosmic-ray air showers. Here we present the results of a search for neutrino interactions inside IceCube's instrumented volume between 1 TeV and 1 PeV in 641 days of data taken from 2010-2012, lowering the energy threshold for neutrinos from the southern sky below 10 TeV for the first time, far below the threshold of the previous high-energy analysis. Astrophysical neutrinos remain the dominant component in the southern sky down to a deposited energy of 10 TeV. From these data we derive new constraints on the diffuse astrophysical neutrino spectrum, Φν = 2.06−18 Eν /10 5 GeV −2.46±0.12 GeV −1 cm −2 sr −1 s −1 for 25 TeV < Eν < 1.4 PeV, as well as the strongest upper limit yet on the flux of neutrinos from charmed-meson decay in the atmosphere, 1.52 times the benchmark theoretical prediction used in previous IceCube results at 90% confidence.

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“…Since the analytical derivation of a neutrino yield factor is challenging for prompt neutrinos, the yield is calculated from air shower simulations using CORSIKA [29] with DPMJET [56,57].…”

Section: Appendix: Calculation Of the Neutrino Kneementioning

confidence: 99%

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2014

Phys. Rev. D

102

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when the array was running in its 59-string configuration. The data sample was optimized to contain muon neutrino induced events with a background contamination of atmospheric muons of less than 1%. These data, which are dominated by atmospheric neutrinos, are analyzed with a global likelihood fit to search for possible contributions of prompt atmospheric and astrophysical neutrinos, neither of which have yet been identified. Such signals are expected to follow a harder energy spectrum than conventional atmospheric neutrinos. In addition, the zenith angle distribution differs for astrophysical and atmospheric signals. A global fit of the reconstructed energies and directions of observed events is performed, including possible neutrino flux contributions for an astrophysical signal and atmospheric backgrounds as well as systematic uncertainties of the experiment and theoretical predictions. The best fit yields an astrophysical signal flux for ν μ þν μ of E 2 · ΦðEÞ ¼ 0.25 × 10 −8 GeV cm −2 s −1 sr −1 ,

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Charm production in DPMJET

Cited by 20 publications

References 31 publications

Characterization of the atmospheric muon flux in IceCube

Characterization of the atmospheric muon flux in IceCube

Atmospheric and astrophysical neutrinos above 1 TeV interacting in IceCube

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

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