355 research outputs found
Comparison of the FLUKA calculations with CAPRICE94 data on muons in atmosphere
In order to benchmark the 3-dimensional calculation of the atmospheric neutrino flux based on the FLUKA Monte Carlo code, muon fluxes in the atmosphere have been computed and compared with data taken by the CAPRICE94 experiment at ground level and at different altitudes in the atmosphere. For this purpose only two additions have been introduced with respect to the neutrino flux calculation: the specific solar modulation corresponding to the period of data taking and the bending of charged particles in the atmosphere. Results are in good agreement with experimental data, although improvements in the model are possible. At this level, however, it is not possible to disentangle the interplay between the primary flux and the interaction model.In order to benchmark the 3-dimensional calculation of the atmospheric neutrino flux based on the FLUKA Monte Carlo code, muon fluxes in the atmosphere have been computed and compared with data taken by the CAPRICE94 experiment at ground level and at different altitudes in the atmosphere. For this purpose only two additions have been introduced with respect to the neutrino flux calculation: the specific solar modulation corresponding to the period of data taking and the bending of charged particles in the atmosphere. Results are in good agreement with experimental data, although improvements in the model are possible. At this level, however, it is not possible to disentangle the interplay between the primary flux and the interaction model.In order to benchmark the 3-dimensional calculation of the atmospheric neutrino flux based on the FLUKA Monte Carlo code, muon fluxes in the atmosphere have been computed and compared with data taken by the CAPRICE94 experiment at ground level and at different altitudes in the atmosphere. For this purpose only two additions have been introduced with respect to the neutrino flux calculation: the specific solar modulation corresponding to the period of data taking and the bending of charged particles in the atmosphere. Results are in good agreement with experimental data, although improvements in the model are possible. At this level, however, it is not possible to disentangle the interplay between the primary flux and the interaction model.In order to benchmark the 3-dimensional calculation of the atmospheric neutrino flux based on the FLUKA Monte Carlo code, muon fluxes in the atmosphere have been computed and compared with data taken by the CAPRICE94 experiment at ground level and at different altitudes in the atmosphere. For this purpose only two additions have been introduced with respect to the neutrino flux calculation: the specific solar modulation corresponding to the period of data taking and the bending of charged particles in the atmosphere. Results are in good agreement with experimental data, although improvements in the model are possible. At this level, however, it is not possible to disentangle the interplay between the primary flux and the interaction model.In order to benchmark the 3-dimensional calculation of the atmospheric neutrino flux based on the FLUKA Monte Carlo code, muon fluxes in the atmosphere have been computed and compared with data taken by the CAPRICE94 experiment at ground level and at different altitudes in the atmosphere. For this purpose only two additions have been introduced with respect to the neutrino flux calculation: the specific solar modulation corresponding to the period of data taking and the bending of charged particles in the atmosphere. Results are in good agreement with experimental data, although improvements in the model are possible. At this level, however, it is not possible to disentangle the interplay between the primary flux and the interaction model
Progresses in the validation of the FLUKA atmospheric neutrino flux calculations
The FLUKA calculation of the atmospheric neutrino fluxes have been
cross-checked by comparing predictions on lepton fluxes in atmosphere to
experimental data. The dependence of predicted neutrino fluxes on the shape and
normalization of primary spectrum is also investigatedComment: Presented at TAUP2001 (Sep. 8-12, Assergi, Italy). 5 pages, 1 figur
A 3-Dimensional Calculation of Atmospheric Neutrino Flux
An extensive 3-dimensional Monte Carlo calculation of the atmospheric
neutrino flux is in progress with the FLUKA Monte Carlo code. The results are
compared to those obtained under the 1-dimensional approximation, where
secondary particles and decay products are assumed to be collinear to the
primary cosmic ray, as usually done in most of the already existing flux
calculations. It is shown that the collinear approximation gives rise to a
wrong angular distribution of neutrinos, essentially in the Sub-GeV region.
However, the angular smearing introduced by the experimental inability of
detecting recoils in neutrino interactions with nuclei is large enough to wash
out, in practice, most of the differences between 3-dimensional and
1-dimensional flux calculations. Therefore, the use of the collinear
approximation should have not introduced a significant bias in the
determination of the flavor oscillation parameters in current experiments.Comment: 27 pages, 14 figures. To be submitted to Astroparticle Physics. To be
submitted to Astroparticle Physic
A Monte Carlo approach to study neutron and fragment emission in heavy-ion reactions
Quantum Molecular Dynamics models (QMD) are Monte Carlo approaches targeted
at the description of nucleon-ion and ion-ion collisions. We have developed a
QMD code, which has been used for the simulation of the fast stage of ion-ion
collisions, considering a wide range of system masses and system mass
asymmetries. The slow stage of the collisions has been described by statistical
methods. The combination of both stages leads to final distributions of
particles and fragments, which have been compared to experimental data
available in literature. A few results of these comparisons, concerning neutron
double-differential production cross-sections for C, Ne and Ar ions impinging
on C, Cu and Pb targets at 290 - 400 MeV/A bombarding energies and fragment
isotopic distributions from Xe + Al at 790 MeV/A, are shown in this paper.Comment: 12 pages, 3 figures, submitted for publication in Adv. Space Re
Heavy-ion collisions described by a new QMD code interfaced to FLUKA: model validation by comparisons with experimental data concerning neutron and charged fragment production
A new code, based on the Quantum Molecular Dynamics theoretical approach, has been developed and interfaced to the FLUKA evaporation/fission/Fermi break-up module. At present, this code is undergoing a series of validation tests. In this paper its predictions are compared to measured charged fragment yields and double differential neutron spectra in thin target heavy-ion reactions, at bombarding energies of about 100 MeV/A. The comparisons with the predictions of a modified version of RQMD 2.4 originally developed in Frankfurt, already available in the FLUKA code, are presented and potential improvements are briefly sketched.A new code, based on the Quantum Molecular Dynamics theoretical approach, has been developed and interfaced to the FLUKA evaporation/fission/Fermi break-up module. At present, this code is undergoing a series of validation tests. In this paper its predictions are compared to measured charged fragment yields and double differential neutron spectra in thin target heavy-ion reactions, at bombarding energies of about 100 MeV/A. The comparisons with the predictions of a modified version of RQMD 2.4 originally developed in Frankfurt, already available in the FLUKA code, are presented and potential improvements are briefly sketched
The FLUKA atmospheric neutrino flux calculation
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.Comment: Papper has been corrected since the cosine of Zenith angle in flux
tables was erraneously inverted. Also, fig. 17 and 18 have been correcte
The hadronic models for cosmic ray physics: the FLUKA code solutions
FLUKA is a general purpose Monte Carlo transport and interaction code used
for fundamental physics and for a wide range of applications. These include
Cosmic Ray Physics (muons, neutrinos, EAS, underground physics), both for basic
research and applied studies in space and atmospheric flight dosimetry and
radiation damage. A review of the hadronic models available in FLUKA and
relevant for the description of cosmic ray air showers is presented in this
paper. Recent updates concerning these models are discussed. The FLUKA
capabilities in the simulation of the formation and propagation of EM and
hadronic showers in the Earth's atmosphere are shown.Comment: 8 pages, 9 figures. Invited talk presented by M.V. Garzelli at
ISVHECRI2006, International Symposium on Very High Energy Cosmic Rays,
Weihai, China, August 15 - 22 200
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