Thematische Bibliographien / Atmospheric muon

Inhaltsverzeichnis

  1. Zeitschriftenartikel
  2. Dissertationen
  3. Buchteile
  4. Konferenzberichte
  5. Berichte der Organisationen

Auswahl der wissenschaftlichen Literatur zum Thema „Atmospheric muon“

Autor: Grafiati
Veröffentlicht am 7. Dezember 2024

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Zeitschriftenartikel zum Thema "Atmospheric muon"

1

Yanchukovsky, Valery. „MUON INTENSITY VARIATIONS AND ATMOSPHERIC TEMPERATURE“. Solar-Terrestrial Physics 6, Nr. 1 (01.04.2020): 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, Nr. 1 (30.03.2020): 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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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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Cecchini, S., und M. Spurio. „Atmospheric muons: experimental aspects“. Geoscientific Instrumentation, Methods and Data Systems Discussions 2, Nr. 2 (20.08.2012): 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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Cecchini, S., und M. Spurio. „Atmospheric muons: experimental aspects“. Geoscientific Instrumentation, Methods and Data Systems 1, Nr. 2 (21.11.2012): 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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Янчуковский, Валерий, Valery Yanchukovsky, Василий Кузьменко und Vasiliy Kuzmenko. „Atmospheric effects of the cosmic-ray mu-meson component“. Solar-Terrestrial Physics 4, Nr. 3 (28.09.2018): 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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Янчуковский, Валерий, Valery Yanchukovsky, Василий Кузьменко und Vasiliy Kuzmenko. „Atmospheric effects of the cosmic-ray mu-meson component“. Solnechno-Zemnaya Fizika 4, Nr. 3 (28.09.2018): 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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SANUKI, TOMOYUKI. „REVIEW OF BALLOONS MUON MEASUREMENT IN THE ATMOSPHERE“. International Journal of Modern Physics A 17, Nr. 12n13 (20.05.2002): 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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MITRA, MALA, und 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, Nr. 02 (20.01.1998): 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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Кузьменко, Василий, Vasiliy Kuzmenko, Валерий Янчуковский und Valery Yanchukovsky. „Determination of density of temperature coefficients for the Earth’s atmosphere muons“. Solnechno-Zemnaya Fizika 1, Nr. 2 (17.06.2015): 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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Dissertationen zum Thema "Atmospheric muon"

1

Bazzotti, Marco <1980&gt. „Studies of the atmospheric muon flux with the ANTARES detector“. Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2009. http://amsdottorato.unibo.it/1906/1/bazzotti_marco_tesi.pdf.

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The thesis main topic is the determination of the vertical component of the atmospheric muon flux as a function of the sea depth at the ANTARES site. ANTARES is a Cherenkov neutrino telescope placed at 2500m depth in the Mediterranean Sea at 40 km from the southern cost of France. In order to retrieve back the physical flux from the experimental data a deconvolution algorithm has been perform which takes into consideration the trigger inefficiensies and the reconstruction errors on the zenith angle. The obtained results are in good agreement with other ANTARES indipendent analysis.
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Bazzotti, Marco <1980&gt. „Studies of the atmospheric muon flux with the ANTARES detector“. Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2009. http://amsdottorato.unibo.it/1906/.

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The thesis main topic is the determination of the vertical component of the atmospheric muon flux as a function of the sea depth at the ANTARES site. ANTARES is a Cherenkov neutrino telescope placed at 2500m depth in the Mediterranean Sea at 40 km from the southern cost of France. In order to retrieve back the physical flux from the experimental data a deconvolution algorithm has been perform which takes into consideration the trigger inefficiensies and the reconstruction errors on the zenith angle. The obtained results are in good agreement with other ANTARES indipendent analysis.
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Pretz, John. „Detection of atmospheric muon neutrinos with the IceCube 9-String Detector“. College Park, Md. : University of Maryland, 2006. http://hdl.handle.net/1903/4163.

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Thesis (Ph. D.) -- University of Maryland, College Park, 2006.
Thesis research directed by: Physics. Title from t.p. of PDF. Includes bibliographical references. Published by UMI Dissertation Services, Ann Arbor, Mich. Also available in paper.
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Mauri, Nicoletta <1980&gt. „Measurement of the atmospheric muon charge ratio with the OPERA detector“. Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3932/1/Mauri_Nicoletta_Tesi.pdf.

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The atmospheric muon charge ratio, defined as the number of positive over negative charged muons, is an interesting quantity for the study of high energy hadronic interactions in atmosphere and the nature of the primary cosmic rays. The measurement of the charge ratio in the TeV muon energy range allows to study the hadronic interactions in kinematic regions not yet explored at accelerators. The OPERA experiment is a hybrid electronic detector/emulsion apparatus, located in the underground Gran Sasso Laboratory, at an average depth of 3800 meters water equivalent (m.w.e.). OPERA is the first large magnetized detector that can measure the muon charge ratio at the LNGS depth, with a wide acceptance for cosmic ray muons coming from above. In this thesis, the muon charge ratio is measured using the spectrometers of the OPERA detector in the highest energy region. The charge ratio was computed separately for single and for multiple muon events, in order to select different primary cosmic ray samples in energy and composition. The measurement as a function of the surface muon energy is used to infer parameters characterizing the particle production in atmosphere, that will be used to constrain Monte Carlo predictions. Finally, the experimental results are interpreted in terms of cosmic ray and particle physics models.
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Mauri, Nicoletta <1980&gt. „Measurement of the atmospheric muon charge ratio with the OPERA detector“. Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3932/.

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The atmospheric muon charge ratio, defined as the number of positive over negative charged muons, is an interesting quantity for the study of high energy hadronic interactions in atmosphere and the nature of the primary cosmic rays. The measurement of the charge ratio in the TeV muon energy range allows to study the hadronic interactions in kinematic regions not yet explored at accelerators. The OPERA experiment is a hybrid electronic detector/emulsion apparatus, located in the underground Gran Sasso Laboratory, at an average depth of 3800 meters water equivalent (m.w.e.). OPERA is the first large magnetized detector that can measure the muon charge ratio at the LNGS depth, with a wide acceptance for cosmic ray muons coming from above. In this thesis, the muon charge ratio is measured using the spectrometers of the OPERA detector in the highest energy region. The charge ratio was computed separately for single and for multiple muon events, in order to select different primary cosmic ray samples in energy and composition. The measurement as a function of the surface muon energy is used to infer parameters characterizing the particle production in atmosphere, that will be used to constrain Monte Carlo predictions. Finally, the experimental results are interpreted in terms of cosmic ray and particle physics models.
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Bailly-Salins, Louis. „Atmοspheric muοn studies and light sterile neutrinο search with ΚΜ3ΝeΤ/ΟRCA“. Electronic Thesis or Diss., Normandie, 2024. http://www.theses.fr/2024NORMC228.

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La collaboration KM3NeT construit actuellement deux télescopes Cherenkov à neutrinos au fond de la mer Méditerranée, ORCA (Oscillation Research with Cosmics in the Abyss) pour mesurer les oscillations des neutrinos atmosphériques et ARCA (Astroparticle Research with Cosmics in the Abyss) pour détecter les neutrinos provenant de sources astrophysiques.Dans ce manuscrit, après avoir passé en revue l'état des mesures d'oscillation des neutrinos et des recherches de neutrinos stériles légers dans le premier chapitre, les détecteurs KM3NeT sont présentés dans le deuxième chapitre.Dans le chapitre 3, une méthode d'étalonnage basée sur la qualité des traces de muons atmosphériques reconstruites est utilisée pour valider les procédures d'étalonnage de la position et de l'orientation des détecteurs KM3NeT, et une nouvelle méthode également basée sur les muons est développée pour effectuer l'étalonnage en temps d'une manière beaucoup moins gourmande en ressources CPU que la méthode précédente. Ensuite, dans le chapitre 4, les muons atmosphériques sont étudiés plus en détail pour sélectionner ceux qui s'arrêtent dans le volume instrumenté de KM3NeT/ORCA. Nous montrons qu'avec une configuration très partielle (5%) du détecteur ORCA, plus de 8000 muons d'arrêt peuvent être sélectionnés par jour avec une pureté de plus de 95% et un excellent accord entre données et simulations.Enfin, le chapitre 5 décrit la première analyse d'oscillation réalisée avec les données ORCA pour rechercher un neutrino stérile léger. Aucun signal positif n'est trouvé à un niveau de confiance de 90%, et des limites compétitives sont posées sur l'amplitude du mélange des neutrinos muoniques et tauiques avec un état stérile
The KM3NeT collaboration is currently building two Cherenkov neutrino telescopes at the bottom of the Mediterranean sea, ORCA (Oscillation Research with Cosmics in the Abyss) to measure atmospheric neutrino oscillations and ARCA (Astroparticle Research with Cosmics in the Abyss) to detect neutrinos from astrophysical sources. In this manuscript, after reviewing the status of neutrino oscillation measurements and light sterile neutrino searches in the first chapter, the KM3NeT detectors are presented in the second chapter.In chapter 3, a calibration method based on the quality of the reconstructed atmospheric muon tracks is used to cross-validate the position and orientation calibration procedures of KM3NeT detectors, and a new muon-based method is developed to perform the time calibration in a much less CPU intensive way than the previous method. Then, in chapter 4, atmospheric muons are further studied to select those stopping within the instrumented volume of KM3NeT/ORCA. We show that with a very partial configuration (5%) of the ORCA detector, more than 8000 stopping muons can be selected per day with a purity of more than 95% and an excellent agreement between data and simulations.Finally, chapter 5 describes the first oscillation analysis performed with ORCA data to search for a light sterile neutrino. No positive signal is found at a 90% confidence level, and competitive limits are put on the magnitude of the mixing of muon and tau neutrinos with a sterile state
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Versari, Federico <1992&gt. „Measurement of the atmospheric electron and muon neutrino flux with the ANTARES neutrino telescope“. Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2021. http://amsdottorato.unibo.it/9664/1/PhD_Thesis____.pdf.

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This thesis presents a combined measurement of the energy spectra of atmospheric electron and muon neutrinos in the energy range between around 100 GeV and 50 TeV with the ANTARES neutrino telescope. The analysis uses 3012 days of detector livetime in the period from 2007 to 2017, and selects 1016 neutrino interacting in (or close to) the instrumented volume of the detector, yielding shower-like events and starting track events. The contamination by atmospheric muons is suppressed at the level of a few per mill by different steps in the selection analysis, including a Boosted Decision Tree classifier. The distribution of reconstructed events is unfolded in terms of electron and muon neutrino fluxes and the derived energy spectra are compared with previous measurements.
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Haberland, Marcus. „A search for a prompt atmospheric muon neutrino flux in the northern hemisphere using data releases from IceCube“. Thesis, Uppsala universitet, Högenergifysik, 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-415984.

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The IceCube Neutrino Observatory is a cubic kilometre scale detector for high-energy neutrinos above hundreds of GeV produced in Earth’s atmosphere as well as outside our solar system whenever particles are accelerated to ultra-relativistic energies. The prompt atmospheric contribution is a result of the creation of heavy mesons with charm components in the atmosphere. Past studies from IceCube using a maximum likelihood estimation over the whole neutrino energy spectrum always reported a best-fit zero prompt contribution so far [1–5], contrary to theory [6, 7]. In this analysis we tried to measure this prompt atmospheric flux in muon neutrino event data from different IceCube releases. In contrast to past studies we performed a binned least-squares fit of the conventional atmospheric flux from data at low energies and subtracted this fit and an astrophysical flux reported by IceCube to measure a prompt contribution. Due to a lack of statistics and accessible information from data releases, our results are also compatible with a zero prompt contribution.
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Biron, von Curland Alexander. „Search for atmospheric muon neutrinos and extraterrestric neutrino point sources in the 1997 AMANDA-B10 data“. [S.l.] : [s.n.], 2002. http://deposit.ddb.de/cgi-bin/dokserv?idn=964841223.

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Geyer, Klaus [Verfasser], und Gisela [Akademischer Betreuer] Anton. „Measurements of the atmospheric muon rate with the ANTARES neutrino telescope / Klaus Geyer. Gutachter: Gisela Anton“. Erlangen : Friedrich-Alexander-Universität Erlangen-Nürnberg (FAU), 2015. http://d-nb.info/1076165915/34.

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Buchteile zum Thema "Atmospheric muon"

1

Learned, John G. „The Atmospheric Neutrino Anomaly: Muon Neutrino Disappearance“. In Current Aspects of Neutrino Physics, 89–130. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-662-04597-8_5.

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Chiarusi, Tommaso. „L3+Cosmics: an atmospheric muon experiment at CERN“. In Astrophysical Sources of High Energy Particles and Radiation, 325–30. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0560-9_28.

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3

Spurio, Maurizio. „Atmospheric Muons and Neutrinos“. In Astronomy and Astrophysics Library, 359–95. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-08051-2_11.

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Spurio, Maurizio. „Atmospheric Muons and Neutrinos“. In Astronomy and Astrophysics Library, 401–39. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96854-4_11.

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Paul, Surojit, K. P. Arunbabu, M. Chakraborty, S. K. Gupta, B. Hariharan, Y. Hayashi, P. Jagadeesan et al. „Monitoring the Upper Atmosphere and Interplanetary Magnetic Field Using Atmospheric Muons at GRAPES-3“. In Springer Proceedings in Physics, 1000–1002. Singapore: Springer Nature Singapore, 2024. http://dx.doi.org/10.1007/978-981-97-0289-3_267.

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Lee, T. D., H. Robinson, M. Schwartz und R. Cool. „Intensity of Upward Muon Flux due to Cosmic-Ray Neutrinos Produced in the Atmosphere“. In Selected Papers, 155–58. Boston, MA: Birkhäuser Boston, 1986. http://dx.doi.org/10.1007/978-1-4612-5397-6_21.

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Hoffmann, Michael R. „Possible Chemical Transformations in Snow and Ice Induced by Solar (UV PHOTONS) and Cosmic Irradiation (MUONS)“. In Chemical Exchange Between the Atmosphere and Polar Snow, 353–77. Berlin, Heidelberg: Springer Berlin Heidelberg, 1996. http://dx.doi.org/10.1007/978-3-642-61171-1_16.

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Reines, F., W. R. Kropp, H. W. Sobel, H. S. Gurr, J. Lathrop, M. F. Crouch, J. P. F. Sellschop und B. S. Meyer. „Muons Produced By Atmospheric Neutrinos: Experiment“. In Neutrinos and Other Matters, 208–26. WORLD SCIENTIFIC, 1991. http://dx.doi.org/10.1142/9789814343060_0034.

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Chen, H. H., W. R. Kropp, H. W. Sobel und F. Reines. „Muons Produced by Atmospheric Neutrinos: Analysis“. In Neutrinos and Other Matters, 227–49. WORLD SCIENTIFIC, 1991. http://dx.doi.org/10.1142/9789814343060_0035.

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Perkins, D. H. „Cosmic particles“. In Particle Astrophysics, 229–72. Oxford University PressOxford, 2008. http://dx.doi.org/10.1093/oso/9780199545452.003.0009.

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Abstract The particles circulating in the cosmos include the so-called cosmic rays, which have been intensively studied ever since their discovery by Hess in 1912. Karl K. Darrow, a past chairman of the American Physical Society, caught some of the atmosphere of this early research when he described their study as remarkable ‘for the delicacy of the apparatus, the minuteness of the phenomena, the adventurous excursions of the experimenters and the grandeur of the inferences’. Cosmic rays consist of high-energy particles incident on the Earth from outer space, plus the secondary particles which they generate as they traverse the atmosphere. Their study has a special place in physics, not only in its own right, but because of the pioneering role that cosmic ray research has played—and is still playing—in the study of elementary particles and their interactions. We can recall the discovery in cosmic rays of antimatter, in the form of the positron and e*e– pair production in 1932, and of pions and muons and strange particles in the late 1940s. In those days, before 1950, the cosmic radiation was the only available source of high-energy particles (those above about 1 GeV). These discoveries indeed kick-started the building of large particle accelerators and the development of their associated detecting equipment, developments which were essential in broadening the scope of the subject and putting elementary particle physics on a sound quantitative basis.
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Konferenzberichte zum Thema "Atmospheric muon"

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Kuzmitskiy, A. V., und A. A. Kochanov. „DEPTH INTENSITY RELATION AND ANGULAR DISTRIBUTION OF THE HIGH-ENERGY ATMOSPHERIC MUONS IN WATER MEDIUM: NEW CALCULATION“. In Baikal Young Scientists’ International School on Fundamental Physics, 51–53. Institute of Solar-Terrestrial Physics SB RAS, 2024. http://dx.doi.org/10.62955/0135-3748-2024-51.

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One of the important tasks of high-energy astrophysics is the search for cosmic neutrinos and the determination of their sources. To solve this problem, large-volume detectors are being created – neutrino telescopes that register Cherenkov light from charged particles generated by neutrino interactions in the medium. Cherenkov light can be produced not only by muons from neutrinos or hadron showers, but also by transit atmospheric muons. Therefore, the analysis of events, recorded in neutrino telescopes, requires a thorough study of the background of muons. It is necessary to know the characteristics of muon fluxes generated in the Earth's atmosphere and their zenith-angular distributions near the detector. In this paper, we present the depth intensity relation and zenith-angular distribution of atmospheric muons in the water medium of Lake Baikal for the Baikal-GVD detector. Calculations were performed with new boundary spectra of atmospheric muons at sea level within the hadronic models of Kimel-Mokhov and quark-gluon strings QGSJET-II-03, as well as parameterization of the Hillas-Gaisser spectrum of primary cosmic rays.
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Aamir, Yusuf. „Muon Flux Variance from Severe Atmospheric Conditions“. In Muon Flux Variance from Severe Atmospheric Conditions. US DOE, 2024. http://dx.doi.org/10.2172/2429212.

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3

Garg, Diksha, und Mary Hall Reno. „Atmospheric muon fluxes at sub-orbital neutrino detectors“. In 38th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2023. http://dx.doi.org/10.22323/1.444.0370.

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Bardačová, Zuzana. „Atmospheric muon suppression for Baikal-GVD cascade analysis“. In 38th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2023. http://dx.doi.org/10.22323/1.444.0986.

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5

Savić, Mihailo, Nikola Veselinović, Aleksandar Dragić, Dimitrije Maletić, Dejan Joković, Radomir Banjanac, Vladimir Udovičić, David Knežević und Miloš Travar. „Cosmic Rays and Their Connection to Space Weather and Earth’s Climate“. In Building bridges between climate science and society through a transdisciplinary network, 63–64. Belgrade, Serbia: Scientific Society Isaac Newton, 2024. http://dx.doi.org/10.69646/bbbs2407.

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Annotation:
Cosmic rays have been studied for over a century. In addition to investigating their fundamental properties, such as origin, composition, and acceleration mechanisms, some of the most important studies in the field involve the interaction of cosmic rays within the heliosphere, near-Earth space, and the immediate Earth’s environment. These areas have been of particular interest in recent years.One such type of study focuses on the modulation of cosmic rays by the solar magnetic field and the geomagnetic field in the heliosphere and Earth’s magnetosphere, respectively. Among other things, the study of these modulations allows for the indirect observation of solar events, which produce characteristic signatures in the interplanetary magnetic field.Another interesting aspect of cosmic ray physics involves the interactions of secondary cosmic rays, primarily the muon component, within Earth’s atmosphere. Precise models of these interactions allow for corrections for atmospheric effects to be made to the muon flux, increasing the sensitivity of Earth-based detectors. Additionally, these models can enable inversediagnostics of the atmosphere, potentially providing an additional technique for atmospheric sounding.Thus, precise monitoring of cosmic ray variations can serve as a proxy for measuring solar activity and variations in Earth’s atmosphere. This can be invaluable in situations where direct measurements are not available and can provide significant contributions to the study of space weather and Earth’s climate.
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CIRCELLA, M. „MUON MEASUREMENTS IN THE ATMOSPHERE IN THE CONTEXT OF THE ATMOSPHERIC NEUTRINO ANOMALY“. In Proceedings of the International School of Cosmic Ray Astrophysics 20th Anniversary, 11th Course. WORLD SCIENTIFIC, 2000. http://dx.doi.org/10.1142/9789812793997_0005.

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7

Clark, R. „The atmospheric neutrino muon-like fraction above 1 GeV“. In INTERSECTIONS BETWEEN PARTICLE AND NUCLEAR PHYSICS. ASCE, 1997. http://dx.doi.org/10.1063/1.54393.

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8

Giorgini, Miriam. „Final results on atmospheric muon neutrino oscillations with MACRO“. In International Workshop on Astroparticle and High Energy Physics. Trieste, Italy: Sissa Medialab, 2003. http://dx.doi.org/10.22323/1.010.0036.

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9

Nikolashkin, Semen, Semen V. Titov und Peter Gololobov. „The effect of winter stratospheric warmings on the intensity of the muon component of secondary cosmic rays“. In 26th International Symposium on Atmospheric and Ocean Optics, Atmospheric Physics, herausgegeben von Gennadii G. Matvienko und Oleg A. Romanovskii. SPIE, 2020. http://dx.doi.org/10.1117/12.2575697.

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10

Feng, Qi, und J. Jarvis. „A citizen-science approach to muon events in imaging atmospheric Cherenkov telescope data: the Muon Hunter“. In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0826.

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Berichte der Organisationen zum Thema "Atmospheric muon"

1

Gogos, Jeremy Peter. An atmospheric muon neutrino disappearance measurement with the MINOS far detector. Office of Scientific and Technical Information (OSTI), Dezember 2007. http://dx.doi.org/10.2172/932867.

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2

Molina Bueno, Laura. Measurement of the Muon Atmospheric Production Depth with the Water Cherenkov Detectors of the Pierre Auger Observatory. Office of Scientific and Technical Information (OSTI), September 2015. http://dx.doi.org/10.2172/1248227.

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3

Poirier, J. Calculation of Atmospheric Muons from Cosmic Gamma Rays. Office of Scientific and Technical Information (OSTI), April 2005. http://dx.doi.org/10.2172/839832.

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4

Rahman, Aftabur Dipu. Atmospheric Neutrino Induced Muons in the MINOS Far Detector. Office of Scientific and Technical Information (OSTI), Februar 2007. http://dx.doi.org/10.2172/902865.

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5

Trost, H. J. On the scattering of atmospheric muons in the rock above Soudan 2. Office of Scientific and Technical Information (OSTI), Januar 1992. http://dx.doi.org/10.2172/5613495.

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6

Trost, H. J. On the scattering of atmospheric muons in the rock above Soudan 2. Office of Scientific and Technical Information (OSTI), Januar 1992. http://dx.doi.org/10.2172/10132949.

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