Статті в журналах: "Atmospheric muon"

1

Yanchukovsky, Valery. "MUON INTENSITY VARIATIONS AND ATMOSPHERIC TEMPERATURE." Solar-Terrestrial Physics 6, no. 1 (April 1, 2020): 108–15. http://dx.doi.org/10.12737/stp-61202013.

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Muons in the atmosphere are formed during the decay of pions resulting from nuclear interactions of cosmic rays with nuclei of air atoms. The resulting muons are also unstable particles with a short lifetime. Therefore, not all of them reach the level of observation in the atmosphere. When the atmospheric temperature changes, the distance to the observation level changes too, thus leading to variations in the intensity of muons of temperature origin. These variations, caused by atmospheric temperature variations, are superimposed on continuous observations of muon telescopes. Their exclusion is, therefore, extremely necessary, especially in the data from modern muon telescopes whose statistical accuracy is very high. The contribution of various atmospheric layers to the total temperature effect is not the same for muons. This contribution is characterized by the distribution of the density of temperature coefficients for muons in the atmosphere. Using this distribution and the continuous intensity observations from the muon telescope in Novosibirsk, the inverse problem has been solved, from the solution of which the atmospheric temperature variations over a long period from 2004 to 2011 have been found. The results obtained are compared with aerological sounding data.

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2

Yanchukovsky, Valery. "MUON INTENSITY VARIATIONS AND ATMOSPHERIC TEMPERATURE." Solnechno-Zemnaya Fizika 6, no. 1 (March 30, 2020): 134–41. http://dx.doi.org/10.12737/szf-61202013.

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Muons in the atmosphere are formed during the decay of pions resulting from nuclear interactions of cosmic rays with nuclei of air atoms. The resulting muons are also unstable particles with a short lifetime. Therefore, not all of them reach the level of observation in the atmosphere. When the atmospheric temperature changes, the distance to the observation level changes too, thus leading to variations in the intensity of muons of temperature origin. These variations, caused by atmospheric temperature variations, are superimposed on continuous observations of muon telescopes. Their exclusion is, therefore, extremely necessary, especially in the data from modern muon telescopes whose statistical accuracy is very high. The contribution of various atmospheric layers to the total temperature effect is not the same for muons. This contribution is characterized by the distribution of the density of temperature coefficients for muons in the atmosphere. Using this distribution and the continuous intensity observations from the muon telescope in Novosibirsk, the inverse problem has been solved, from the solution of which the atmospheric temperature variations over a long period from 2004 to 2011 have been found. The results obtained are compared with aerological sounding data.

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3

Kajita, Takaaki. "Atmospheric Neutrinos." Advances in High Energy Physics 2012 (2012): 1–24. http://dx.doi.org/10.1155/2012/504715.

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Atmospheric neutrinos are produced as decay products in hadronic showers resulting from collisions of cosmic rays with nuclei in the atmosphere. Electron-neutrinos and muon-neutrinos are produced mainly by the decay chain of charged pions to muons to electrons. Atmospheric neutrino experiments observed zenith angle and energy-dependent deficit of muon-neutrino events. It was found that neutrino oscillations between muon-neutrinos and tau-neutrinos explain these data well. This paper discusses atmospheric neutrino experiments and the neutrino oscillation studies with these neutrinos.

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4

Cecchini, S., and M. Spurio. "Atmospheric muons: experimental aspects." Geoscientific Instrumentation, Methods and Data Systems Discussions 2, no. 2 (August 20, 2012): 603–41. http://dx.doi.org/10.5194/gid-2-603-2012.

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Abstract. We present a review of atmospheric muon flux and energy spectrum measurements over almost six decades of muon momentum. Sea-level and underground/water/ice experiments are considered. Possible sources of systematic errors in the measurements are examinated. The characteristics of underground/water muons (muons in bundle, lateral distribution, energy spectrum) are discussed. The connection between the atmospheric muon and neutrino measurements are also reported.

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5

Cecchini, S., and M. Spurio. "Atmospheric muons: experimental aspects." Geoscientific Instrumentation, Methods and Data Systems 1, no. 2 (November 21, 2012): 185–96. http://dx.doi.org/10.5194/gi-1-185-2012.

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Abstract. We present a review of atmospheric muon flux and energy spectrum measurements over almost six decades of muon momentum. Sea level and underground/water/ice experiments are considered. Possible sources of systematic errors in the measurements are examined. The characteristics of underground/water muons (muons in bundle, lateral distribution, energy spectrum) are discussed. The connection between the atmospheric muon and neutrino measurements are also reported.

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6

Янчуковский, Валерий, Valery Yanchukovsky, Василий Кузьменко, and Vasiliy Kuzmenko. "Atmospheric effects of the cosmic-ray mu-meson component." Solar-Terrestrial Physics 4, no. 3 (September 28, 2018): 76–82. http://dx.doi.org/10.12737/stp-43201810.

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Variations in the intensity of cosmic rays observed in the depth of the atmosphere include the atmospheric component of the variations. Cosmic-ray muon telescopes, along with the barometric effect, have a significant temperature effect due to the instability of detected particles. To take into account atmospheric effects in muon telescope data, meteorological coefficients of muon intensity are found. The meteorological coefficients of the intensity of muons recorded in the depth of the atmosphere are estimated from experimental data, using various methods of factor analysis. The results obtained from experimental data are compared with the results of theoretical calculations.

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7

Янчуковский, Валерий, Valery Yanchukovsky, Василий Кузьменко, and Vasiliy Kuzmenko. "Atmospheric effects of the cosmic-ray mu-meson component." Solnechno-Zemnaya Fizika 4, no. 3 (September 28, 2018): 95–102. http://dx.doi.org/10.12737/szf-43201810.

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Variations in the intensity of cosmic rays observed in the depth of the atmosphere include the atmospheric component of the variations. Cosmic-ray muon telescopes, along with the barometric effect, have a significant temperature effect due to the instability of detected particles. To take into account atmospheric effects in muon telescope data, meteorological coeffi-cients of muon intensity are found. The meteorological coefficients of the intensity of muons recorded in the depth of the atmosphere are estimated from experi-mental data, using various methods of factor analysis. The results obtained from experimental data are com-pared with the results of theoretical calculations.

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8

SANUKI, TOMOYUKI. "REVIEW OF BALLOONS MUON MEASUREMENT IN THE ATMOSPHERE." International Journal of Modern Physics A 17, no. 12n13 (May 20, 2002): 1635–44. http://dx.doi.org/10.1142/s0217751x02011138.

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In order to study neutrino oscillation phenomena using atmospheric neutrinos, it is crucially important to calculate their absolute fluxes and spectral shapes accurately. Since production and decay processes of muons are accompanied by neutrino production, observations of atmospheric muons give fundamental information about atmospheric neutrinos. Atmospheric muons have been measured at various sites; from a ground level to a balloon floating altitude. Very precise measurement has been carried out on the ground. Muon growth curves are measured during balloon ascending periods. These data can be used to investigate hadronic interaction models. Investigations of atmospheric muons will improve accuracy of the neutrino calculations. Statistics in the muon measurement during balloon experiments are still insufficient. In order to improve the statistics drastically, dedicated muon experiments are very important.

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9

MITRA, MALA, and D. P. BHATTACHARYYA. "ESTIMATION OF UPWARD MUON ENERGY SPECTRA IN THE EARTH INDUCED BY DIFFUSE MUON NEUTRINOS EMITTED FROM THE ATMOSPHERIC, GALACTIC AND ACTIVE GALACTIC NUCLEAR SOURCES." International Journal of Modern Physics A 13, no. 02 (January 20, 1998): 209–21. http://dx.doi.org/10.1142/s0217751x98000081.

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The energy spectra of upward muons in the Earth emitted by atmospheric, galactic and AGN diffuse muon neutrinos incident on the Earth have been estimated using the standard formulation developed by Gaisser based on charge–current interactions in rock along with the QED-based energy loss formulation. The derived primary-cosmic-nucleus–air interaction yield neutrino-induced muon spectrum in the vertical direction is in accord with the recent data available from MACRO, IMB, KAMIOKA and BAKSAN underground experiments for energies below 3 GeV. The TeV muon energy spectra initiated by atmospheric, galactic and AGN diffuse muon neutrinos of Stecker et al. and Szabo and Protheroe have also been estimated. The estimated atmospheric neutrino-induced muon fluxes at 0° and 89° above 2 TeV energy do not cross the observed upper limit detected by Meyer using the underground Frejus muon detector.

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10

Кузьменко, Василий, Vasiliy Kuzmenko, Валерий Янчуковский, and Valery Yanchukovsky. "Determination of density of temperature coefficients for the Earth’s atmosphere muons." Solnechno-Zemnaya Fizika 1, no. 2 (June 17, 2015): 91–96. http://dx.doi.org/10.12737/10403.

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When studying variations of cosmic ray intensity, by the use of muon telescopes located deep in the atmosphere it is necessary to take into account changes in atmospheric parameters, mainly pressure and temperature. The density distribution of temperature coefficients of the atmosphere muon intensity needs to be estimated from observations. To this purpose, the method of principal components regression and meth-ods of projection to latent structures (PLS-1 and PLS-2). We used data of continuous recording of muons, as well as Novosibirsk 2004–2010 aerological data. As shown by comparing results, PLS-2 method allows us to esti-mate the density distribution of muon intensity temperature coefficients with minimal errors.

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11

Briki, I., M. Mazouz, and L. Ghedira. "Angular distribution of low momentum atmospheric muons at ground level." Journal of Cosmology and Astroparticle Physics 2023, no. 04 (April 1, 2023): 025. http://dx.doi.org/10.1088/1475-7516/2023/04/025.

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Abstract We report measurements of the angular distributions of low momentum atmospheric muons at 38 m above sea level for zenith angles θ between -60 and 60 degrees in the south-north direction. The muon detection was performed with two NaI(Tl) scintillation detectors mounted in coincidence. An adjustable lead thickness placed between the detectors allowed to select muons with a minimal momentum ranging from 0.3 to 0.9 GeV/c. The integrated and the differential muon flux were determined by analyzing the deposited energy spectra in the scintillators backed up by a Geant4 simulation of the experimental setup. The results are consistent with the cos n (θ) distribution in good agreement with the literature. These data contribute to fill the gap in the geomagnetic cutoff rigidity interval 8 GV < Pc < 14 GV where no similar measurements were performed before. We found that n = 1.88 - 0.12 Pμ c in this domain of muon momenta cutoff Pμ c < 1 GeV/c. The present measurements are useful for many muon studies requiring an accurate integrated flux.

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12

Rigozo, Nivaor Rodolfo, and Adriano Petry. "THE ATMOSPHERIC PRESSURE EFFECT ON MUON DATA NORMALIZATION BY SPECTRAL ANALYSIS STUDIES." Revista Brasileira de Geofísica 31, no. 3 (September 1, 2013): 507. http://dx.doi.org/10.22564/rbgf.v31i3.324.

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ABSTRACT. This paper presents a study of the atmospheric pressure effects on ground cosmic ray muon time series, using the iterative regression spectral analysis method. Along the study, it was observed that the 34 periods present in the atmospheric pressure amplitude spectrum are present in the muon data amplitude spectra as well. It was concluded that the normalization of muon data is only efﬁcient for periods shorter than nine days, in order to eliminate the atmospheric effects.Keywords: cosmic rays, time series, spectral analysis. RESUMO. Este artigo apresenta um estudo dos efeitos da pressão atmosférica nas series temporais de raios cósmicos, usando a metodologia da análise espectral pela iteração regressiva. Foi observado um total de 34 periodicidades presentes no espectro de amplitude da pressão atmosférica que também estão presentes no espectro de amplitude dos dados de muons. Conclui-se que a padronização dos dados de muons para eliminar os efeitos da pressão atmosférica é eﬁciente somente para períodos abaixo de 9 diasPalavras-chave: raios cósmicos, série temporal, análise espectral.

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13

Scapparone, E. "Energy Estimate of Neutrino Induced Upgoing Muons." International Journal of Modern Physics A 18, supp01 (February 2003): 340–47. http://dx.doi.org/10.1142/s0217751x03016719.

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An estimate of the energy of neutrino-induced muons in MACRO is provided by a multiple Coulomb scattering measurement. The MACRO original upward-muon data sample has been subdivided according to the reconstructed muon energy. Data in each subset are then compared with expected fluxes from atmospheric neutrinos. The results are interpreted in terms of neutrino oscillations.

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14

Ismail, A. Haj, and A. AbdelKader. "Optimizing the zenith angle dependence of cosmic ray muons from Charm particles in the knee region: simulation study." Journal of Physics: Conference Series 2429, no. 1 (February 1, 2023): 012013. http://dx.doi.org/10.1088/1742-6596/2429/1/012013.

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Abstract The muonic component of air showers is one of the most abundant component of charged particles arriving at the Earth’s surface, and able to penetrate deeply underground, and is very sensitive to the primary mass and energy of the initial cosmic particle. Atmospheric muons are produced in the propagation of different components of extensive air showers. Therefore, variations in the muon ratio, defined as the number of positive over negative charged muons, must be well understood. In this paper, we study the variation of the muon charge ratio of cosmic muons at different zenith angles, and we study the contribution of charm particles in producing atmospheric muons using Monte Carlo showers initiated by two cosmic primaries, proton and iron, with four energies [10 PeV, 100 PeV, 1 EeV, 10 EeV], in the zenith range of [0° to 60°].

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15

Cohu, Amélie, Matias Tramontini, Antoine Chevalier, Jean-Christophe Ianigro, and Jacques Marteau. "Atmospheric and Geodesic Controls of Muon Rates: A Numerical Study for Muography Applications." Instruments 6, no. 3 (August 4, 2022): 24. http://dx.doi.org/10.3390/instruments6030024.

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Muon tomography or muography is an innovative imaging technique using atmospheric muons. The technique is based on the detection of muons that have crossed a target and the measurement of their attenuation or deviation induced by the medium. Muon flux models are key ingredients to convert tomographic and calibration data into the 2D or 3D density maps of the target. Ideally, they should take into account all possible types of local effects, from geomagnetism to atmospheric conditions. Two approaches are commonly used: semi-empirical models or Monte Carlo simulations. The latter offers the advantage to tackle down many environmental and experimental parameters and also allows the optimization of the nearly horizontal muons flux, which remains a long-standing problem for many muography applications. The goal of this paper is to identify through a detailed simulation what kind of environmental and experimental effects may affect the muography imaging sensitivity and its monitoring performance. The results have been obtained within the CORSIKA simulation framework, which offers the possibility to tune various parameters. The paper presents the simulation’s configuration and the results obtained for the muon fluxes computed in various conditions.

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16

CURRAT, CHARLES A. "Measuring Cosmic Ray and Atmospheric Neutrinos in the Sudbury Neutrino Observatory." International Journal of Modern Physics A 20, no. 14 (June 10, 2005): 3106–9. http://dx.doi.org/10.1142/s0217751x05025863.

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High energy muons and neutrinos are produced by the interaction of primary cosmic rays in the Earth's upper atmosphere. These primary interactions produce mesons that decay into muons and neutrinos. SNO is in a unique position amongst underground experiments in the world. At the depth of over 6 km water equivalent, it is the deepest underground laboratory currently in operation. SNO can make a number of novel measurements using muons. First, SNO is sensitive to the downward muon rate coming from primary cosmic ray interactions. Second, SNO's great depth makes possible the detection of atmospheric neutrinos (via the detection of neutrino induced muons) from the nadir to inclinations as large as cos (θ zenith ) ≃ 0.4 above the horizon. Although SNO is a modest-size Cherenkov detector, SNO's unique niche allows it to make important model-independent checks of atmospheric neutrino oscillations.

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17

Venere, L. Di, G. Giavitto, F. Giordano, R. López-Coto, and R. Pillera. "A fast muon tagger method for Imaging Atmospheric Cherenkov Telescopes." Journal of Physics: Conference Series 1548, no. 1 (May 1, 2020): 012036. http://dx.doi.org/10.1088/1742-6596/1548/1/012036.

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Abstract The Cherenkov Telescope Array (CTA) will be the next major observatory for Very High Energy gamma-ray astronomy. Its optical throughput calibration relies on muon Cherenkov rings. This work is aimed at developing a fast and efficient muon tagger at the camera level for the CTA telescopes. A novel technique to tag muons using the capabilities of silicon photomultiplier Compact High-Energy Camera CHEC-S, one of the design options for the camera of the small size telescopes, has been developed, studying and comparing different algorithms such as circle fitting with the Taubin method, machine learning using a neural network and simple pixel counting. Their performance in terms of efficiency and computation speed was investigated using simulations with varying levels of night sky background light. The application of the best performing method to the large size telescope camera has also been studied, to improve the speed of the muon preselection.

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18

TIMASHKOV, D. A., M. B. AMELCHAKOV, D. V. CHERNOV, V. V. KINDIN, R. P. KOKOULIN, K. G. KOMPANIETS, R. V. KONOPATOV, et al. "ALBEDO MUONS: NEW DATA AND CALCULATIONS." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 6977–79. http://dx.doi.org/10.1142/s0217751x0503065x.

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Data on near-horizontal muons obtained with experimental complex NEVOD-DECOR are analyzed. More than 1.5 × 103 atmospheric muons scattered into upper hemisphere with energy above 7 GeV were registered. Calculations show that the main process forming albedo muon flux near horizon is multiple Coulomb scattering.

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19

Dorman, L. I., and I. V. Dorman. "Cosmic-ray atmospheric electric field effects." Canadian Journal of Physics 73, no. 7-8 (July 1, 1995): 440–43. http://dx.doi.org/10.1139/p95-063.

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Experimental data on the atmospheric electric field effect in the cosmic-ray muon component are discussed on the basis of the general theory of cosmic-ray meteorological effects. In this framework, we develop the theory of atmospheric electric field effects in the hard- and soft-muons of secondary cosmic rays and in the neutron-monitor counting rates as well. We show that the experimental results can be understood on the basis of this theory. We also show that a sufficient atmospheric electric field effect in the cosmic-ray neutron component is to be expected because the neutron monitors work as analyzers of soft muons and really detect only negative muons as well as neutrons.

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20

SINEGOVSKY, S. I., A. A. KOCHANOV, T. S. SINEGOVSKAYA, A. MISAKI, and N. TAKAHASHI. "ATMOSPHERIC MUON FLUX AT PEV ENERGIES." International Journal of Modern Physics A 25, no. 18n19 (July 30, 2010): 3733–40. http://dx.doi.org/10.1142/s0217751x10049748.

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In the near future, the energy region above few hundreds of TeV may really be accessible for measurements of the atmospheric muon spectrum with IceCube array. Therefore, one expects that muon flux uncertainties above 50 TeV, related to a poor knowledge of charm production cross-sections and insufficiently examined primary spectra and composition, will be diminished. We give predictions for the very high-energy muon spectrum at sea level, obtained with the three hadronic interaction models, taking into account also the muon contribution due to decays of the charmed hadrons.

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21

Pérez Bertolli, C., C. Sarmiento-Cano, and H. Asorey. "MUON FLUX ESTIMATION IN THE ANDES UNDERGROUND LABORATORY." Anales AFA 32, no. 4 (January 15, 2022): 106–11. http://dx.doi.org/10.31527/analesafa.2021.32.4.106.

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The ANDES Underground Laboratory is being planned and designed to be one of the largest and most shielded laboratories in the Southern Hemisphere, which will be located in the Andes Range, in the area of the current Paso AguaNegra that connects the provinces of San Juan (Argentina) and Elqui (Chile). The diversity of experiments that are being planned, including experiments for the direct and indirect search of dark matter and neutrino precision physics, requires a precise knowledge of the flux of high-energy atmospheric muons within the laboratory. These are produced during the interaction of astroparticles with energies between 1012and 1018eV denominated of high and ultra-high energy with the Earth’s atmosphere. In the high-energy component, muons with energies of tens of TeV can be found, capable of passing through thousands of meters of rock. Previous estimates made from reasonable assumptions about the type of rock expected in the area showed that the expected muon flux was compatible with other underground laboratories at an equivalent depth. In this work, extensive atmospheric showers flux simulations were performed at the laboratory site. Afterwards, there was a selection of those muons with sufficient energy to reach the laboratory-based on their angle of incidence and the height at which they enter the mountain. Then a transfer function was modeled using the new geological studies currently available that allow us to have a detailed model of the rock distribution inside the mountain. Finally, the interaction of these muons with the different types of rock was calculated numerically along their way to the laboratory using the continuous slowdown approximation, thus obtaining that the expected muon flux within the laboratory is 1,47±0,02 day−1m−2sr−1

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22

Pyras, L., C. Glaser, S. Hallmann, and A. Nelles. "Atmospheric muons at PeV energies in radio neutrino detectors." Journal of Cosmology and Astroparticle Physics 2023, no. 10 (October 1, 2023): 043. http://dx.doi.org/10.1088/1475-7516/2023/10/043.

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Abstract Experiments seeking to detect radio emission stemming from neutrino interactions will soon reach sensitivities that bring a detection within reach. Since experiments like RNO-G or the future IceCube-Gen2 target more than an order of magnitude more effective volume than existing experiments, the renewed and detailed study of rare backgrounds is needed. In this paper, we study the potential background from energy losses of highly energetic atmospheric muons. Due to both limited experimental measurements and limited modeling in hadronic interaction models, the expected event rate is subject to large uncertainties. Here, we estimate rate predictions and their uncertainties for different models and instrumental parameters. We also study possible routes towards mitigation of the muon background, such as parent air shower detection, and illustrate what is needed to make the first measurement of the prompt muon flux at energies above 10 PeV.

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23

Bhatt, Apoorva, Paweł Malecki, and Dariusz Góra. "Shore Shadow Effect in Baikal." Universe 8, no. 7 (June 24, 2022): 347. http://dx.doi.org/10.3390/universe8070347.

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The measurement of the individual charged particles especially muons in an extended air shower (EAS) resulting from primary cosmic rays provides important distinguishing parameters to identify the chemical composition of the cosmic primary particles. For Neutrino Telescope experiments like Baikal-GVD, the estimation of underwater muon flux is of importance to study atmospheric muons. In this paper, a GEANT4-based simulation is presented to estimate the atmospheric muon flux underwater taking Baikal-GVD as an example. The location of the Baikal-GVD experiment at Lake Baikal provides a unique opportunity to study the passage of muons through its northern shore and the water. The muons arriving from the north direction will lose more energy as compared to those arriving from the south. An approximation for the northern shore is also simulated in the GEANT4 geometry and the results of the simulation are compared with the measurements from the NT-96 detector. The results of the simulations are consistent with the shore shadow observed in the measurements in the NT-96. This approach can also be used to propagate the muons from generators like CORSIKA through long distances in matter like water, ice, earth, etc. for simulations in such experiments.

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Pasquali, L., M. H. Reno, and I. Sarcevic. "Muon and muon neutrino fluxes from atmospheric charm." Nuclear Physics B - Proceedings Supplements 70, no. 1-3 (January 1999): 361–63. http://dx.doi.org/10.1016/s0920-5632(98)00452-6.

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25

Maghrabi, A. H., R. N. Alotaibi, M. M. Almutayri, and M. S. Garawi. "Influence of the Atmospheric Mass on the High Energy Cosmic Ray Muons during a Solar Cycle." Advances in Astronomy 2015 (2015): 1–7. http://dx.doi.org/10.1155/2015/939146.

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The rate of the detected cosmic ray muons depends on the atmospheric mass, height of pion production level, and temperature. Corrections for the changes in these parameters are importance to know the properties of the primary cosmic rays. In this paper, the effect of atmospheric mass, represented here by the atmospheric pressure, on the cosmic ray was studied using data from the KACST muon detector during the 2002–2012 period. The analysis was conducted by calculating the barometric coefficient (α) using regression analysis between the two parameters. The variation ofαover different time scales was investigated. The results revealed a seasonal cycle ofαwith a maximum in September and a minimum in March. Data from Adelaide muon detector were used, and different monthly variation was found. The barometric coefficient displays considerable variability at the interannual scale. Study of the annual variations ofαindicated cyclic variation with maximums between 2008 and 2009 and minimums between 2002 and 2003. This variable tendency is found to be anticorrelated with the solar activity, represented by the sunspot number. This finding was compared with the annual trend ofαfor the Adelaide muon detector for the same period of time, and a similar trend was found.

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26

Honda, Morihiro. "Improving the prediction of the Atmospheric neutrino flux using the atmospheric muon flux." EPJ Web of Conferences 208 (2019): 07001. http://dx.doi.org/10.1051/epjconf/201920807001.

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It is well known that the correlation of atmospheric neutrinos and muons are simply correlated in the energy region of 1–10 GeV, and used for the test bench of the hadronic interaction model used for the calculation of the atmospheric neutrino flux. However, the correlation becomes unclear for neutrinos in the energy range below 1 GeV, which is important for the study of mass ordering of neutrino and CP phase of the neutrino mass. We extend the study of the correlation to the lower neutrino energies and find that the atmospheric muon flux observed at high altitude shows a good correlation to the atmospheric neutrino flux, and could be used to calibrate the hadronic interaction model.

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27

Kedar, S., H. K. M. Tanaka, C. J. Naudet, C. E. Jones, J. P. Plaut, and F. H. Webb. "Muon radiography for exploration of Mars geology." Geoscientific Instrumentation, Methods and Data Systems 2, no. 1 (June 17, 2013): 157–64. http://dx.doi.org/10.5194/gi-2-157-2013.

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Abstract. Muon radiography is a technique that uses naturally occurring showers of muons (penetrating particles generated by cosmic rays) to image the interior of large-scale geological structures in much the same way as standard X-ray radiography is used to image the interior of smaller objects. Recent developments and application of the technique to terrestrial volcanoes have demonstrated that a low-power, passive muon detector can peer deep into geological structures up to several kilometers in size, and provide crisp density profile images of their interior at ten meter scale resolution. Preliminary estimates of muon production on Mars indicate that the near horizontal Martian muon flux, which could be used for muon radiography, is as strong or stronger than that on Earth, making the technique suitable for exploration of numerous high priority geological targets on Mars. The high spatial resolution of muon radiography also makes the technique particularly suited for the discovery and delineation of Martian caverns, the most likely planetary environment for biological activity. As a passive imaging technique, muon radiography uses the perpetually present background cosmic ray radiation as the energy source for probing the interior of structures from the surface of the planet. The passive nature of the measurements provides an opportunity for a low power and low data rate instrument for planetary exploration that could operate as a scientifically valuable primary or secondary instrument in a variety of settings, with minimal impact on the mission's other instruments and operation.

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28

Saraf, Mandar, Pandi Raj Chinnappan, Aditya Deodhar, Mamta Jangra, J. Krishnamoorthi, Gobinda Majumder, Veera Padmavathy, et al. "Design, fabrication and large scale qualification of cosmic muon veto scintillator detectors." Journal of Instrumentation 18, no. 05 (May 1, 2023): P05003. http://dx.doi.org/10.1088/1748-0221/18/05/p05003.

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Abstract The INO collaboration is designing a cosmic muon veto detector (CMVD) to cover the mini-ICAL detector which is operational at the IICHEP transit campus, Madurai in South India. The aim of the CMVD is to study the feasibility of building an experiment to record rare events at a shallow depth of around 100 m, and use plastic scintillators to veto atmospheric muons from those produced by the rare interactions within the target mass of the detector. The efficiency of such a veto detector should be better than 99.99% and false positive rate should be less than 10-5. The CMVD is being built using extruded plastic scintillator (EPS) strips to detect and tag atmospheric muons. More than 700 EPS strips are required to build the CMVD. Two EPS strips are pasted together to make a di-counter (DC) and wavelength shifting fibres are embedded inside the EPS strips to trap the scintillation light generated by a passing cosmic ray muon and transmit it as secondary photons to the Silicon Photo-Multipliers (SiPMs) mounted at the two ends of the DCs. Since the efficiency requirement of the veto detector is rather high, it is imperative to thoroughly test each and every component used for building the CMVD. A cosmic ray muon telescope has been setup using the DCs to qualify all the DCs that will be fabricated. In this paper we will discuss the details of the design and fabrication of the DCs, the cosmic muon setup and the electronics used for their testing and the test results.

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29

Jourde, K., D. Gibert, and J. Marteau. "Improvement of density models of geological structures by fusion of gravity data and cosmic muon radiographies." Geoscientific Instrumentation, Methods and Data Systems 4, no. 2 (August 25, 2015): 177–88. http://dx.doi.org/10.5194/gi-4-177-2015.

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Abstract. This paper examines how the resolution of small-scale geological density models is improved through the fusion of information provided by gravity measurements and density muon radiographies. Muon radiography aims at determining the density of geological bodies by measuring their screening effect on the natural flux of cosmic muons. Muon radiography essentially works like a medical X-ray scan and integrates density information along elongated narrow conical volumes. Gravity measurements are linked to density by a 3-D integration encompassing the whole studied domain. We establish the mathematical expressions of these integration formulas – called acquisition kernels – and derive the resolving kernels that are spatial filters relating the true unknown density structure to the density distribution actually recovered from the available data. The resolving kernel approach allows one to quantitatively describe the improvement of the resolution of the density models achieved by merging gravity data and muon radiographies. The method developed in this paper may be used to optimally design the geometry of the field measurements to be performed in order to obtain a given spatial resolution pattern of the density model to be constructed. The resolving kernels derived in the joined muon–gravimetry case indicate that gravity data are almost useless for constraining the density structure in regions sampled by more than two muon tomography acquisitions. Interestingly, the resolution in deeper regions not sampled by muon tomography is significantly improved by joining the two techniques. The method is illustrated with examples for the La Soufrière volcano of Guadeloupe.

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30

Béné, S. "Air shower simulation for background estimation in muon tomography of volcanoes." Geoscientific Instrumentation, Methods and Data Systems Discussions 2, no. 2 (August 6, 2012): 563–74. http://dx.doi.org/10.5194/gid-2-563-2012.

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Abstract. One of the main sources of background for the radiography of volcanoes with atmospheric muons comes from the accidental coincidences produced in the muon telescopes by the air showers. In order to quantify this background, Monte-Carlo simulations of the showers and of the detector are developed by the Tomuvol collaboration. As a first step, the atmospheric showers were simulated and investigated using two Monte-Carlo packages, CORSIKA and GEANT4. We compared the results provided by the two programs for the muonic component of vertical proton-induced showers at three energies: 1, 10 and 100 TeV. We found that the spatial distribution and energy spectrum of the muons were in good agreement for the two codes, while significant differences were observed for the arrival time of the muons.

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31

Sorokovikov, M. N., A. D. Morozova, T. S. Sinegovskaya, and S. I. Sinegovsky. "Spectra and angle distributions of the atmospheric neutrinos and muons from the charm particle decays." Izvestiâ Akademii nauk SSSR. Seriâ fizičeskaâ 88, no. 3 (March 15, 2024): 507–11. http://dx.doi.org/10.31857/s0367676524030247.

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A new calculation of the prompt component of atmospheric leptons — muon neutrinos and muons from the decays of charmed particles is performed for the same hadron cascade model that was used in calculating the characteristics of atmospheric leptons from the decays of π- and K-mesons. Spectral zenith-angular distributions of prompt and (π, K)-leptons are obtained. The cross-energy intervals are found for which the prompt lepton fluxes contribution comparably to the fluxes of (π, K)-muons and neutrinos. The possibility is shown of the prompt neutrinos detecting at energies much lower of the cross-energy.

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32

Borja, Cristian, Carlos Ávila, Gerardo Roque, and Manuel Sánchez. "Atmospheric Muon Flux Measurement near Earth’s Equatorial Line." Instruments 6, no. 4 (November 22, 2022): 78. http://dx.doi.org/10.3390/instruments6040078.

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We report measurements of muon flux over the sky of the city of Bogotá at 4°35′56′′ north latitude, 74°04′51′′ west longitude, and an altitude of 2657 m above sea level, carried out with a hodoscope composed of four stations of plastic scintillators located equidistant over a distance of 4.8 m. Measurements were taken at different zenith (θ) angles within the range 1.5° ≤ θ ≤90°, the muon flux data is statistically consistent with a cos2θ dependence, with a χ2 per degree of freedom near unity. If instead, we fit to a cosnθ we obtain n = 2.145±0.046 with a lower χ2 per degree of freedom. Integrating the muon flux distribution as a function of the zenith angle over the solid angle of the upper Earth’s hemisphere allows an estimation of the atmospheric vertical muon rate at the altitude and latitude of Bogota obtaining a value of 255.1 ± 5.8m−2s−1. This estimate is consistent with an independent direct measurement of the vertical muon flux with all detectors stacked horizontally. These measurements play a key role in the further development of detectors, aimed to perform muon imaging of Monserrate Hill, located in Bogotá, where the detectors will be placed at similar locations to those used in the present study.

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33

ZHU, SHOU-HUA. "V-PARTICLE AGAIN?" International Journal of Modern Physics D 20, no. 08 (August 15, 2011): 1399–412. http://dx.doi.org/10.1142/s021827181101958x.

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This talk is mainly based on our previous work.1 We will investigate the possibility of detecting light long-lived particle (LLP) produced by high energy cosmic ray colliding with atmosphere. The LLP may penetrate the atmosphere and decay into a pair of muons near/in the neutrino telescope. Such muons can be treated as the detectable signal for neutrino telescope. The particle with such behavior is very similar with that of the first observed strange particle in cosmic ray events, which was coined historically as "V-particle" in some literature. This study is motivated by recent cosmic electron/positron observations which suggest the existence of O(TeV) dark matter and new light O(GeV) particle. It indicates that dark sector may be complicated, and there may exist more than one light particle, for example the dark gauge boson A′ and associated dark Higgs boson h′. In this work, we discuss the scenario with A′ heavier than h′ and h′ is treated as LLP. Based on our numerical estimation, we find that the large volume neutrino telescope IceCube has the capacity to observe several tens of di-muon events per year for favorable parameters if the decay length of LLP can be comparable with the depth of atmosphere. The challenge here is how to suppress the muon background induced by cosmic rays and atmospheric neutrinos.

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34

Shukla, Prashant, and Sundaresh Sankrith. "Energy and angular distributions of atmospheric muons at the Earth." International Journal of Modern Physics A 33, no. 30 (October 30, 2018): 1850175. http://dx.doi.org/10.1142/s0217751x18501750.

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A fair knowledge of the atmospheric muon distributions at Earth is a prerequisite for the simulations of cosmic ray setups and rare event search detectors. A modified power law is proposed for atmospheric muon energy distribution which gives a good description of the cosmic muon data in low as well as high energy regime. Using this distribution, analytical forms for zenith angle [Formula: see text] distribution are obtained. Assuming a flat Earth, it leads to the [Formula: see text] form where it is shown that the parameter [Formula: see text] is nothing but the power of the energy distribution. Exact analytical function is obtained for inclined trajectory of muon. A new closed form for zenith angle distribution is obtained without assuming a flat Earth and which gives an improved description of the data at all angles even above [Formula: see text]. These distributions are tested with the available atmospheric muon data of energy and angular distributions. The parameters of these distributions can be used to characterize the cosmic muon data as a function of energy, angle and altitude.

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35

Yanchukovsky, Valery. "Temperature effect of muons registered under the ground in Yakutsk by telescopes on GAS-discharge counters." Solar-Terrestrial Physics 9, no. 2 (June 29, 2023): 55–65. http://dx.doi.org/10.12737/stp-92202307.

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The Yakutsk spectrograph of cosmic rays includes a complex of muon telescopes based on gas-discharge and scintillation counters located on the surface and under the ground at depths of 7, 20, and 40 m.w.e. Using continuous observations made by muon telescopes on gas-discharge counters and data on the altitude profile of the atmospheric temperature over Yakutsk for the period from January 2016 to December 2018, we have calculated density distributions of temperature coefficients for muons detected on the surface and at various depths under the ground. To do this, we employed multivariate regression methods and principal component methods. The results obtained are compared with the results of earlier theoretical calculations. The results make it possible to correctly take into account the temperature effect in the data from the complex of muon telescopes on gas-discharge counters.

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36

Yanchukovsky, Valery. "Temperature effect of muons registered under the ground in Yakutsk by telescopes on GAS-discharge counters." Solnechno-Zemnaya Fizika 9, no. 2 (June 29, 2023): 60–70. http://dx.doi.org/10.12737/szf-92202307.

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The Yakutsk spectrograph of cosmic rays includes a complex of muon telescopes based on gas-discharge and scintillation counters located on the surface and under the ground at depths of 7, 20, and 40 m.w.e. Using continuous observations made by muon telescopes on gas-discharge counters and data on the altitude profile of the atmospheric temperature over Yakutsk for the period from January 2016 to December 2018, we have calculated density distributions of temperature coefficients for muons detected on the surface and at various depths under the ground. To do this, we employed multivariate regression methods and principal component methods. The results obtained are compared with the results of earlier theoretical calculations. The results make it possible to correctly take into account the temperature effect in the data from the complex of muon telescopes on gas-discharge counters.

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37

Honda, Morihiro. "Atmospheric neutrino and Muon fluxes." Czechoslovak Journal of Physics 56, S1 (September 2006): A281—A290. http://dx.doi.org/10.1007/s10582-006-0162-y.

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38

Maghrabi, Abdullrahman, and Mohammed Almutayri. "Atmospheric Effect on Cosmic Ray Muons at High Cut-Off Rigidity Station." Advances in Astronomy 2016 (2016): 1–9. http://dx.doi.org/10.1155/2016/9620189.

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Cosmic ray data and radiosonde measurements from Riyadh, Saudi Arabia (Rc = 14.4 GV), for the period 2002–2012, were used to study the effect of atmospheric pressure, level of pion production, and temperature at that level, on cosmic ray muons. We found that, even if corrections were made to the detected muons using these three parameters, seasonal variations of the cosmic rays still exist. This suggests that other terrestrial and/or extraterrestrial causes may be considered. The levels of pion production and atmospheric pressure are inversely correlated with the muon rate. On the other hand, the temperature at the pion production level is correlated with muons in spring and winter and inversely correlated in fall and summer. There is no clear explanation for this behavior.

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39

Béné, S., P. Boivin, E. Busato, C. Cârloganu, C. Combaret, P. Dupieux, F. Fehr, et al. "Air shower simulation for background estimation in muon tomography of volcanoes." Geoscientific Instrumentation, Methods and Data Systems 2, no. 1 (January 11, 2013): 11–15. http://dx.doi.org/10.5194/gi-2-11-2013.

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Abstract. One of the main sources of background for the radiography of volcanoes using atmospheric muons comes from the accidental coincidences produced in the muon telescopes by charged particles belonging to the air shower generated by the primary cosmic ray. In order to quantify this background effect, Monte Carlo simulations of the showers and of the detector are developed by the TOMUVOL collaboration. As a first step, the atmospheric showers were simulated and investigated using two Monte Carlo packages, CORSIKA and GEANT4. We compared the results provided by the two programs for the muonic component of vertical proton-induced showers at three energies: 1, 10 and 100 TeV. We found that the spatial distribution and energy spectrum of the muons were in good agreement for the two codes.

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40

Giacomelli, G., and A. Margiotta. "The MACRO Experiment." Modern Physics Letters A 18, no. 29 (September 21, 2003): 2001–18. http://dx.doi.org/10.1142/s0217732303011654.

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In this paper we describe the main results obtained by the MACRO experiment: final stringent upper limits on GUT magnetic monopoles and nuclearites, results on atmospheric neutrino oscillations, high energy muon neutrino astronomy, searches for WIMPs, search for low energy stellar gravitational collapse neutrinos, several studies with high energy downgoing muons and determination of the primary cosmic ray composition at knee energies.

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41

Timakov, S. S., and A. A. Petrukhin. "Azimuthal scanning of the atmosphere in a muon flux." Известия Российской академии наук. Серия физическая 87, no. 8 (August 1, 2023): 1214–16. http://dx.doi.org/10.31857/s0367676523701909.

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A new approach to the analysis of the intensity of the muon flux from different azimuthal directions is considered, which makes it possible to detect waves in the atmosphere from large-scale atmospheric phenomena (fronts, thunderstorm cells).

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42

Dedenko, L. G., A. V. Lukyashin, T. M. Roganova, and G. F. Fedorova. "Testing of almost all the hadronic interaction models by comparing calculated muon energy spectrum with data." EPJ Web of Conferences 208 (2019): 07004. http://dx.doi.org/10.1051/epjconf/201920807004.

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Uncertainties of the model energy spectra of the most energetic secondary charged mesons are discussed. Computer simulations of the partial energy spectra of the atmospheric vertical muons induced by primary cosmic particles with various fixed energies in terms of hadronic interactions models had been carried out with the help of the CORSIKA package. These partial spectra have been convolved with the contemporary spectra of the primary cosmic particles in the energy range 0.1-10 000 TeV. Results of simulations are compared with the contemporary data of the atmospheric vertical muon flux. Comparison shows that all models underestimate the production of secondary charged π±-mesons (and K±-mesons) by a factor of ~ 1.4 ÷ 2 at the highest energies. This underestimation induces a more rapid development of extensive air showers in the atmosphere and results in uncertainties in estimates of energy and composition of the primary cosmic particles.

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43

Dyonisius, Michael N., Vasilii V. Petrenko, Andrew M. Smith, Benjamin Hmiel, Peter D. Neff, Bin Yang, Quan Hua, et al. "Using ice core measurements from Taylor Glacier, Antarctica, to calibrate in situ cosmogenic ¹⁴C production rates by muons." Cryosphere 17, no. 2 (February 20, 2023): 843–63. http://dx.doi.org/10.5194/tc-17-843-2023.

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Abstract. Cosmic rays entering the Earth's atmosphere produce showers of secondary particles such as protons, neutrons, and muons. The interaction of these particles with oxygen-16 (16O) in minerals such as ice and quartz can produce carbon-14 (14C). In glacial ice, 14C is also incorporated through trapping of 14C-containing atmospheric gases (14CO2, 14CO, and 14CH4). Understanding the production rates of in situ cosmogenic 14C is important to deconvolve the in situ cosmogenic and atmospheric 14C signals in ice, both of which contain valuable paleoenvironmental information. Unfortunately, the in situ 14C production rates by muons (which are the dominant production mechanism at depths of >6 m solid ice equivalent) are uncertain. In this study, we use measurements of in situ 14C in ancient ice (>50 ka) from the Taylor Glacier, an ablation site in Antarctica, in combination with a 2D ice flow model to better constrain the compound-specific rates of 14C production by muons and the partitioning of in situ 14C between CO2, CO, and CH4. Our measurements show that 33.7 % (±11.4 %; 95 % confidence interval) of the produced cosmogenic 14C forms 14CO and 66.1 % (±11.5 %; 95 % confidence interval) of the produced cosmogenic 14C forms 14CO2. 14CH4 represents a very small fraction (<0.3 %) of the total. Assuming that the majority of in situ muogenic 14C in ice forms 14CO2, 14CO, and 14CH4, we also calculated muogenic 14C production rates that are lower by factors of 5.7 (3.6–13.9; 95 % confidence interval) and 3.7 (2.0–11.9; 95 % confidence interval) for negative muon capture and fast muon interactions, respectively, when compared to values determined in quartz from laboratory studies (Heisinger et al., 2002a, b) and in a natural setting (Lupker et al., 2015). This apparent discrepancy in muogenic 14C production rates in ice and quartz currently lacks a good explanation and requires further investigation.

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44

Oyama, Yuichi. "Evidence of High-energy Neutrinos from SN1987A by Kamiokande-II and IMB." Astrophysical Journal 925, no. 2 (February 1, 2022): 166. http://dx.doi.org/10.3847/1538-4357/ac4269.

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Abstract High-energy neutrinos from SN1987A were searched for using upward-going muons recorded by the Kamiokande-II experiment and the IMB experiment. Between 1987 August 11 and October 20, and from an angular window of 10° radius, two upward-going muon events were recorded by Kamiokande-II, and also two events were recorded by IMB. The probability that these upward-going muons were explained by a chance coincidence of atmospheric neutrinos was calculated to be 0.27%. This shows possible evidence of high-energy neutrinos from SN1987A.

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45

Nagahara, Shogo, and Seigo Miyamoto. "Feasibility of three-dimensional density tomography using dozens of muon radiographies and filtered back projection for volcanos." Geoscientific Instrumentation, Methods and Data Systems 7, no. 4 (November 7, 2018): 307–16. http://dx.doi.org/10.5194/gi-7-307-2018.

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Abstract. This study is the first trial to apply the method of filtered back projection (FBP) to reconstruct three-dimensional (3-D) bulk density images via cosmic-ray muons. We also simulated three-dimensional reconstruction image with dozens of muon radiographies for a volcano using the FBP method and evaluated its practicality. The FBP method is widely used in X-ray and CT image reconstruction but has not been used in the field of muon radiography. One of the merits of using the FBP method instead of the ordinary inversion method is that it does not require an initial model, while ordinary inversion analysis needs an initial model. We also added new approximation factors by using data on mountain topography in existing formulas to successfully reduce systematic reconstruction errors. From a volcanic perspective, lidar is commonly used to measure and analyze mountain topography. We tested the performance and applicability to a model of Omuroyama, a monogenetic scoria cone located in Shizuoka, Japan. As a result, it was revealed that the density difference between the original and reconstructed images depended on the number of observation points and the accidental error caused by muon statistics depended on the multiplication of total effective area and exposure period. Combining all of the above, we established how to evaluate an observation plan for volcanos using dozens of muon radiographies.

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46

Kato, Chihiro, Wataru Kihara, Yukino Ko, Akira Kadokura, Ryuho Kataoka, Paul Evenson, Satoru Uchida, et al. "New cosmic ray observations at Syowa Station in the Antarctic for space weather study." Journal of Space Weather and Space Climate 11 (2021): 31. http://dx.doi.org/10.1051/swsc/2021005.

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Muon detectors and neutron monitors were recently installed at Syowa Station, in the Antarctic, to observe different types of secondary particles resulting from cosmic ray interactions simultaneously from the same location. Continuing observations will give new insight into the response of muon detectors to atmospheric and geomagnetic effects. Operation began in February, 2018 and the system has been stable with a duty-cycle exceeding 94%. Muon data shows a clear seasonal variation, which is expected from the atmospheric temperature effect. We verified successful operation by showing that the muon and neutron data are consistent with those from other locations by comparing intensity variations during a space weather event. We have established a web page to make real time data available with interactive graphics (http://polaris.nipr.ac.jp/cosmicrays/).

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47

BARBASHINA, N. S., R. P. KOKOULIN, K. G. KOMPANIETS, A. A. PETRUKHIN, D. A. TIMASHKOV, I. I. YASHIN, G. MANNOCCHI, G. TRINCHERO, and O. SAAVEDRA. "WAVELET ANALYSIS OF ATMOSPHERIC MUON DATA." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 6944–46. http://dx.doi.org/10.1142/s0217751x05030545.

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Experimental data on atmospheric muons obtained with Russian-Italian coordinate detector DECOR have been processed by means of method of wavelet transformation. Results of analysis exhibit time perturbations caused by effects like Forbush decreases and allow to determine not only their periods but also moments of their appearance.

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48

Cârloganu, C., V. Niess, S. Béné, E. Busato, P. Dupieux, F. Fehr, P. Gay, et al. "Towards a muon radiography of the Puy de Dôme." Geoscientific Instrumentation, Methods and Data Systems 2, no. 1 (February 6, 2013): 55–60. http://dx.doi.org/10.5194/gi-2-55-2013.

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Abstract. High-energy (above a few hundred GeV) atmospheric muons are a natural probe for geophysical studies. They can travel through kilometres of rock allowing for a radiography of the density distribution within large structures, like mountains or volcanoes. A collaboration between volcanologists, astroparticle and particle physicists, Tomuvol was formed in 2009 to study tomographic muon imaging of volcanoes with high-resolution, large-scale tracking detectors. We report on two campaigns of measurements at the flank of the Puy de Dôme using glass resistive plate chambers (GRPCs) developed for particle physics, within the CALICE collaboration.

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49

Fedynitch, A., W. Woodley, and M. C. Piro. "On the Accuracy of Underground Muon Intensity Calculations." Astrophysical Journal 928, no. 1 (March 1, 2022): 27. http://dx.doi.org/10.3847/1538-4357/ac5027.

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Abstract Cosmic-ray muons detected by deep underground and underwater detectors have served as an information source on the high-energy cosmic-ray spectrum and hadronic interactions in air showers for almost a century. The theoretical interest in underground muons has nearly faded away because space-borne experiments probe the cosmic-ray spectrum more directly, and accelerators provide precise measurements of hadron yields. However, underground muons probe unique hadron interaction energies and phase space, which are still inaccessible to present accelerator experiments. The cosmic-ray nucleon energies reach the hundred-TeV and PeV ranges, which are barely accessible with space-borne experiments. Our new calculation combines two modern computational tools: mceq for surface muon fluxes and proposal for underground transport. We demonstrate excellent agreement with measurements of cosmic-ray muon intensities underground within estimated errors. Beyond that, the precision of historical data turns out to be significantly smaller than our error estimates. This result shows that the sources of high-energy atmospheric lepton flux uncertainties at the surface or underground can be significantly constrained without taking more data or building new detectors. The reduction of uncertainties can be expected to impact data analyses at large-volume neutrino telescopes and be used for the design of future ton-scale direct dark matter detectors.

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50

Tuneu, Jordi, Peter Filip, and Eva Santos. "On the mystery of the multi-muon flux at the TeV cosmic-ray energy range." EPJ Web of Conferences 283 (2023): 05008. http://dx.doi.org/10.1051/epjconf/202328305008.

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Current Monte Carlo simulations do not provide a good description of the muon component of extensive air showers. Many air shower experiments report discrepancies between their data and Monte Carlo predictions, ranging from the TeV scale up to the highest energies. In these proceedings, we address the seasonal variation of the multi-muon events observed by the NOvA Near Detector (ND). For our studies, we use the general-purpose Monte Carlo code FLUKA to treat the transport and interaction of the air-shower particles in the atmosphere and other media. Our design considers a multilayered atmosphere and a layered underground approximated to match the NOvA ND location and detector geometry. Our atmospheric model uses air densities for winter and summer calculated from the temperature and geopotential information for the pressure levels given by the European Center for Medium-Range Weather Forecasts (ECMWF) datasets in situ. Understanding the multi-muon flux at the cosmic ray high-energy range may lead to a better description of the muon production mechanisms in ultra-high-energy extensive air showers. In addition, it can help to improve future Monte Carlo codes or hint at new physics processes or interactions.

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