High-energy cosmic-ray neutrons at sea level

Kornmayer, H.; Mielke, H.H.; Engler, J.; Knapp, J.

doi:10.1088/0954-3899/21/3/018

Cited by 19 publications

(24 citation statements)

References 16 publications

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“…By suitable weighting and co-adding of sub spectra, total absolute spectra at any position in the solar cycle and any value of the geomagnetic cutoff can be calculated. Shown in Figures 4-7 are the predicted muon, proton, pion , and neutron fluxes for no geomagnetic cutoff and average solar modulation, along with the data points from Rastin [2], Brooke and Wolfendale [3], Ashton and Saleh [4], and Kornmayer et al [5] . Figure 7: MC-generated neutron spectrum and data measured at sea level.…”

Section: Code-data Comparisonsmentioning

confidence: 99%

Monte Carlo Simulation of Proton-induced Cosimc Ray Cascades in the Atmosphere

Hagmann¹,

Lange²,

Wright³

2007

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Section: Code-data Comparisonsmentioning

confidence: 99%

Monte Carlo Simulation of Proton-induced Cosimc Ray Cascades in the Atmosphere

Hagmann¹,

Lange²,

Wright³

2007

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“…As an example, in fig. 12 we compare MonteCarlo results to the hadron flux referred to the vertical as measured with the calorimeter of the KASCADE experiment [ 44,45] with two different angular acceptances.…”

Section: Example Of Calculations Of Particles In Atmospherementioning

confidence: 99%

The FLUKA atmospheric neutrino flux calculation

Battistoni

Ferrari

Montaruli

et al. 2003

Astroparticle Physics

123

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The 3-dimensional (3-D) calculation of the atmospheric neutrino flux by means of the FLUKA Monte Carlo model is here described in all details, starting from the latest data on primary cosmic ray spectra. The importance of a 3-D calculation and of its consequences have been already debated in a previous paper. Here instead the focus is on the absolute flux. We stress the relevant aspects of the hadronic interaction model of FLUKA in the atmospheric neutrino flux calculation. This model is constructed and maintained so to provide a high degree of accuracy in the description of particle production. The accuracy achieved in the comparison with data from accelerators and cross checked with data on particle production in atmosphere certifies the reliability of shower calculation in atmosphere.The results presented here can be already used for analysis by current experiments on atmospheric neutrinos. However they represent an intermediate step towards a final release, since this calculation does not yet include the bending of charged particles in atmosphere. On the other hand this last aspect, while requiring a considerable effort in a fully 3-D description of the Earth, if a high level of accuracy has to be maintained, does not affect in a significant way the analysis of atmospheric neutrino events.

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“…Figure 5: Different parameterization of the cosmic neutron spectrum at sea-level Differences in data and models for the neutron component of cosmic rays at sea-level from different authors (Hess et al 1959), (Ziegler 1998), (Kornmayer et al 1995), (Gordon et al 2004) are evident in the figure. The experimental methods used to derive each of the parameterizations presented in Figure 5 were very different.…”

Section: Simulation Source Particle: Sea-level Cosmic Neutronsmentioning

confidence: 99%

“…The CRY parameterization is the result of a Monte-Carlo simulation of the primary particles that generate the cosmic ray shower. High energy protons are simulated to interact in the atmosphere (Kornmayer et al 1995) simulation of this high energy protons interacting in the atmosphere. The fact that reported cosmic neutron parameterizations are so different must be considered when comparing these results, since the reported cosmogenic production rate is depends strongly on the differential neutron flux.…”

Section: Simulation Source Particle: Sea-level Cosmic Neutronsmentioning

confidence: 99%

“…Monte Carlo/ Nuclear cross section tool Cosmic Neutron spectrum (Elliott et al 2010) CEM03.02 4FP60R flux (Avignone et al 1992) ISABEL simulated cross sections (Hess et al 1959) (Barabanov et al 2006) SHIELD code (Ziegler 1998) This work (User selected n spectrum) Geant4 (Kornmayer et al 1995), (Ziegler 1998), (Hess et al 1959), (Gordon et al 2004) The most modern attempt to experimentally determine cosmogenic activation in enriched germanium is reported in (Elliott et al 2010). Elliot et al irradiated a sample of enriched germanium in a neutron beam at the Los Alamos Neutron Science Center (LANSCE) Weapons Neutron Research (WNR) facility on the Target 4 Flight Path 60 Right (4FP60R).…”

Section: Papermentioning

confidence: 99%

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Optimization of the Transport Shield for Neutrinoless Double Beta-decay Enriched Germanium

Navarrete¹,

Kouzes²,

Orrell³

et al. 2012

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SummaryThis document presents results of an investigation of the material and geometry choice for the transport cosmogenic shield of enriched germanium, the active detector material used in the MAJORANA DEMONSTRATOR neutrinoless double-beta decay search. The objective of this work is to select the optimal material and geometry to minimize cosmogenic production of radioactive isotopes in the germanium material during transport. The design of such a shield is based on the calculation of the cosmogenic production rate of isotopes that are known to cause interfering backgrounds in enriched germanium neutrinoless double-beta decay searches. As part of this study, we will examine the reliability of estimates of cosmogenic activation from this study under different shielding scenarios.This study utilizes Monte Carlo techniques to simulate the transport and attenuation of the incident cosmic ray particles in the shielding material and the nuclear reactions in the germanium. This method of calculating production rates relies completely on the accuracy of the simulation model and library data. The calculated production rate of an isotope is the product of the energy-dependent cross section of the reaction of interest and the incoming cosmic ray produced flux of particles, integrated over the relevant energy range. The production of 68 Ge from the various germanium isotopes have Q values starting at approximately 20 MeV, so the energy range of interest in this study is above 20 MeV. Based on the transport shield design used by GERDA and the MAJORANA DEMONSTRATOR, we present one modification to the shield that will further reduce the production rate of undesired isotopes 68 Ge and 60 Co and still comply with requirements of official transportation standards. The conclusion, based on Monte Carlo models, is that increasing the amount of iron to the container's maximum allowable weight results in a shield that would be an order of magnitude more efficient in the attenuation of the production of isotopes of interest for neutrinoless double-beta decay searches than the current GERDA transport shield design.

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High-energy cosmic-ray neutrons at sea level

Cited by 19 publications

References 16 publications

Monte Carlo Simulation of Proton-induced Cosimc Ray Cascades in the Atmosphere

Monte Carlo Simulation of Proton-induced Cosimc Ray Cascades in the Atmosphere

The FLUKA atmospheric neutrino flux calculation

Optimization of the Transport Shield for Neutrinoless Double Beta-decay Enriched Germanium

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