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Artículos de revistas sobre el tema "Atmospheric muon"

Autor: Grafiati
Publicado: 7 de diciembre de 2024
Última modificación: 31 de julio de 2025

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1

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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2

Yanchukovsky, Valery. "MUON INTENSITY VARIATIONS AND ATMOSPHERIC TEMPERATURE." Solar-Terrestrial Physics 6, no. 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 i
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3

Yanchukovsky, Valery. "MUON INTENSITY VARIATIONS AND ATMOSPHERIC TEMPERATURE." Solnechno-Zemnaya Fizika 6, no. 1 (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 i
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4

Cecchini, S., and M. Spurio. "Atmospheric muons: experimental aspects." Geoscientific Instrumentation, Methods and Data Systems Discussions 2, no. 2 (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 (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 (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 obtain
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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 (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 obta
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8

SANUKI, TOMOYUKI. "REVIEW OF BALLOONS MUON MEASUREMENT IN THE ATMOSPHERE." International Journal of Modern Physics A 17, no. 12n13 (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
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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 (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, g
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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 (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
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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 (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 expe
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12

WANG DeXin, ZHANG Rui, YU DeKang, et al. "Observation and Research on Cosmic Ray Muons and Solar Modulation Effect Based on Plastic Scintillator Detector." Acta Physica Sinica 74, no. 5 (2025): 0. https://doi.org/10.7498/aps.74.20241704.

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Cosmic rays, originating from celestial phenomena such as stars, supernovae, and other astrophysical sources, are composed of high-energy particles that enter Earth’ s atmosphere. Upon interaction with atmospheric nuclei, these primary cosmic rays generate an array of secondary particles, with muons constituting the dominant component at ground level. Muons, due to their relative abundance, stability, and well-characterized energy loss mechanisms, serve as critical probes for investigating the fundamental properties of cosmic rays. Studies of muon energy distribution, diurnal anisotropy, and t
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13

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 (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 pres
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14

Scapparone, E. "Energy Estimate of Neutrino Induced Upgoing Muons." International Journal of Modern Physics A 18, supp01 (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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15

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 (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,
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16

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 (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 adva
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17

CURRAT, CHARLES A. "Measuring Cosmic Ray and Atmospheric Neutrinos in the Sudbury Neutrino Observatory." International Journal of Modern Physics A 20, no. 14 (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 atmosphe
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18

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 (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, mac
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19

TIMASHKOV, D. A., M. B. AMELCHAKOV, D. V. CHERNOV, et al. "ALBEDO MUONS: NEW DATA AND CALCULATIONS." International Journal of Modern Physics A 20, no. 29 (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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20

Dorman, L. I., and I. V. Dorman. "Cosmic-ray atmospheric electric field effects." Canadian Journal of Physics 73, no. 7-8 (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
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21

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 (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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22

Pérez Bertolli, C., C. Sarmiento-Cano, and H. Asorey. "MUON FLUX ESTIMATION IN THE ANDES UNDERGROUND LABORATORY." Anales AFA 32, no. 4 (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
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23

Bhatt, Apoorva, Paweł Malecki, and Dariusz Góra. "Shore Shadow Effect in Baikal." Universe 8, no. 7 (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 op
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24

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 scale
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25

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 (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 subj
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26

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 (1999): 361–63. http://dx.doi.org/10.1016/s0920-5632(98)00452-6.

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27

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 t
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28

An, Xuanzhu, Haoran Yao, and Haotian Yao. "Exploring the Relationship Between Muon Detection Rates and Atmospheric Pressure Using Cosmic Watch Detectors." Theoretical and Natural Science 107, no. 1 (2025): 157–63. https://doi.org/10.54254/2753-8818/2025.22629.

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This study explores how atmospheric pressure affects muon detection rates. By analyzing data from six Cosmic Watch detectors, we organized the collected information, examined the correlation between atmospheric pressure and muon detection rates, and addressed the timing discrepancies across detectors. Our findings show that muon detection rates decrease as atmospheric pressure rises. The study also improves time difference correction methods, providing new strategies and tools for detecting rare coincidence events recorded by multiple detectors.
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29

Saraf, Mandar, Pandi Raj Chinnappan, Aditya Deodhar, et al. "Design, fabrication and large scale qualification of cosmic muon veto scintillator detectors." Journal of Instrumentation 18, no. 05 (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
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30

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 (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. P
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31

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 (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
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32

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 (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
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33

Béné, S. "Air shower simulation for background estimation in muon tomography of volcanoes." Geoscientific Instrumentation, Methods and Data Systems Discussions 2, no. 2 (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 a
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34

Borja, Cristian, Carlos Ávila, Gerardo Roque, and Manuel Sánchez. "Atmospheric Muon Flux Measurement near Earth’s Equatorial Line." Instruments 6, no. 4 (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. Integr
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35

Shukla, Prashant, and Sundaresh Sankrith. "Energy and angular distributions of atmospheric muons at the Earth." International Journal of Modern Physics A 33, no. 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 distributio
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36

ZHU, SHOU-HUA. "V-PARTICLE AGAIN?" International Journal of Modern Physics D 20, no. 08 (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 electro
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37

Tanaka, Hiroyuki K. M. "Distance of flight of cosmic-ray muons to study dynamics of the upper muosphere." Geoscientific Instrumentation, Methods and Data Systems 14, no. 1 (2025): 1–11. https://doi.org/10.5194/gi-14-1-2025.

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Abstract. The Earth can be divided by main layers, including the atmosphere, geosphere (solid Earth), and biosphere, depending on its predominant component. In this work, the layer of the Earth which constantly contains a high concentration of muons (∼8×1012 muons) and its upper border are respectively defined as the muosphere and muopause. The altitude of the muosphere spans from the lower stratosphere to the upper crust of the Earth. In order to study its dynamics, the muopause height was spatiotemporally studied with a new kind of technique called the distance of flight (DOF), which utilize
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38

Yanchukovsky, Valery. "Temperature effect of muons registered under the ground in Yakutsk by telescopes on GAS-discharge counters." Solar-Terrestrial Physics 9, no. 2 (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 regres
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39

Yanchukovsky, Valery. "Temperature effect of muons registered under the ground in Yakutsk by telescopes on GAS-discharge counters." Solnechno-Zemnaya Fizika 9, no. 2 (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 regres
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40

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

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41

Giacomelli, G., and A. Margiotta. "The MACRO Experiment." Modern Physics Letters A 18, no. 29 (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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42

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,
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43

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 (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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44

Béné, S., P. Boivin, E. Busato, et al. "Air shower simulation for background estimation in muon tomography of volcanoes." Geoscientific Instrumentation, Methods and Data Systems 2, no. 1 (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 muon
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45

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. Compa
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46

Vancea, Cătălin, Alexandru Bălăceanu, Mădălina Dobre та ін. "μ 36: a SiPM-read scintillator detector designed for muography applications". Journal of Instrumentation 20, № 05 (2025): P05019. https://doi.org/10.1088/1748-0221/20/05/p05019.

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Abstract We report on the development of a muography detector composed of scintillator bars, wavelength-shifting optical fibers, and silicon photomultipliers (SiPMs), aiming to measure the directional muon flux, necessary in muography applications such as archaeology, or mining safety. Components have been tested using atmospheric muons, light collection has been optimized, and uniformity has been improved. The assembled detector has been validated in laboratory conditions.
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47

Oyama, Yuichi. "Evidence of High-energy Neutrinos from SN1987A by Kamiokande-II and IMB." Astrophysical Journal 925, no. 2 (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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48

Kato, Chihiro, Wataru Kihara, Yukino Ko, 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
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49

Dyonisius, Michael N., Vasilii V. Petrenko, Andrew M. Smith, et al. "Using ice core measurements from Taylor Glacier, Antarctica, to calibrate in situ cosmogenic 14C production rates by muons." Cryosphere 17, no. 2 (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
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50

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 (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
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