Cosmic Rays in the Atmosphere

Grieder, P. K. F.

doi:10.1016/b978-044450710-5/50004-x

Cited by 34 publications

(50 citation statements)

References 185 publications

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“…As their names imply, they observe neutrons and muons generated in the process called cosmic ray cascade. When a cosmic ray particle moves toward the Earth, most of the time it interacts with atmospheric atoms/molecules, generating secondary particles such as those mentioned above, whose intensity variation with time can be influenced by atmospheric phenomena (Grieder 2001;Dorman 2004). The atmospheric pressure changes are the main atmospheric effect on the cosmic ray intensity observed by these instruments.…”

Section: Introductionmentioning

confidence: 99%

The Temperature Effect in Secondary Cosmic Rays (Muons) Observed at the Ground: Analysis of the Global Muon Detector Network Data

Mendonça

Braga

Echer

et al. 2016

ApJ

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The analysis of cosmic ray intensity variation seen by muon detectors at Earthʼs surface can help us to understand astrophysical, solar, interplanetary and geomagnetic phenomena. However, before comparing cosmic ray intensity variations with extraterrestrial phenomena, it is necessary to take into account atmospheric effects such as the temperature effect. In this work, we analyzed this effect on the Global Muon Detector Network (GMDN), which is composed of four ground-based detectors, two in the northern hemisphere and two in the southern hemisphere. In general, we found a higher temperature influence on detectors located in the northern hemisphere. Besides that, we noticed that the seasonal temperature variation observed at the ground and at the altitude of maximum muon production are in antiphase for all GMDN locations (low-latitude regions). In this way, contrary to what is expected in high-latitude regions, the ground muon intensity decrease occurring during summertime would be related to both parts of the temperature effect (the negative and the positive). We analyzed several methods to describe the temperature effect on cosmic ray intensity. We found that the mass weighted method is the one that best reproduces the seasonal cosmic ray variation observed by the GMDN detectors and allows the highest correlation with long-term variation of the cosmic ray intensity seen by neutron monitors.

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Section: Introductionmentioning

confidence: 99%

The Temperature Effect in Secondary Cosmic Rays (Muons) Observed at the Ground: Analysis of the Global Muon Detector Network Data

Mendonça

Braga

Echer

et al. 2016

ApJ

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“…The dominant noisy "single" muons at hundred-GeV energies will loose memory of the primary low energy and hidden mini-shower, (a hundreds GeV or TeVs hadrons ); a single muon will blaze just alone. The muon "single" rings or arcs frequency is larger (than muon bundles ones) and it is based on solid observational data ( [13] ; [12],as shown in fig.2 and references on MUTRON experiment therein); these "noise" event number is:…”

Section: Blazing Cerenkov Flashes By Showers and Decaying Muonsmentioning

confidence: 99%

“…depending on the exact zenith angle and seeing: assuming on average a suppression 5 · 10 −3 and the nominal Magic energy threshold at 30 GeV , it does corresponds to a hadronic shower at far horizons (diluted by nearly three order of magnitude by larger distances) at energy above E CR ≃ 6 PeV. Their primary flux may be estimated considering the known cosmic ray on the top of the atmosphere (both protons or helium) (see DICE Experiment referred in [12] 2km + 360km = 527km; the consequent shower area widen by more than an order of magnitude (and more than three order respect to vertical showers) and the consequent foreseen event number, now for a much harder penetrating C.R. shower at E CR ≥ 3 · 10 17 eV , becomes:…”

Section: Blazing Cerenkov Flashes By Showers and Decaying Muonsmentioning

confidence: 99%

“…See [5], [6], [2], [10], [7], [8], Figure 5: Schematic Picture of an Horizontal Cosmic Ray Air-Shower (superior track) (HAS), induced by EeVν τ ,ν τ HORTAU born inside the east side of the Ande at west side of Auger array detector. Our prediction is that within the first year of record AUGER detectors must reveal the Ande shadows to UHECR, from West-North side by their statistical absence respect flat opposite directions, while within three-five years it should probably observe a few of HORTAUs induced by GZK neutrinos interacting inside the same shadows of the Ande mountain chain (see [6], [7], [8]); [16]) ; Figure 6: Observed Flux of Muons as a function of the zenith angle above (see also [12] and [13]) the horizons; for the muons below the horizons their flux at 91 o zenith angle is two order of magnitude below ≃ 10 −7 cm −2 s −1 sr −1 , as observed by NEVOD and Decor detectors in recent years. As the zenith angle increases the upward muons flux reduces further ; at 94 o and ten GeV energy it is just four order below: ≃ 10 −9 cm −2 s −1 sr −1 , see recent results by NEVOD and DECOR experiments (2003) ; at higher energies (hundred GeVs) and larger zenith angle only muons induced by atmospheric neutrinos arises at ≃ 2 − 3 · 10 −13 cm −2 s −1 sr −1 as well as Neutrino Tau induced Air-Shower (muon secondaries) .…”

Section: Blazing Cerenkov Flashes By Showers and Decaying Muonsmentioning

confidence: 99%

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Air-shower spectroscopy at horizons

Fargion¹

2006

Progress in Particle and Nuclear Physics

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Downward cosmic rays are mostly revealed on the ground by their air-showers diluted and filtered secondary µ + µ − traces and-or by their (Cerenkov -Fluorescent) lights because of the high altitude numerous and luminous electromagnetic e + e − ,γ shower component. Horizontal and Upward air-showers are even more suppressed by deeper atmosphere opacity and by the Earth shadows. In such noise-free horizontal and upward directions rare Ultra High Cosmic rays and rarer neutrino induced air-showers may shine, mostly mediated by resonant PeVsν e + e − → W − interactions in air or by higher energy Tau Air-showers originated by ν τ skimming the Earth. At high altitude (mountains, planes, balloons) the air density is so rarefied that nearly all common air-showers might be observed at their maximal growth at a tuned altitude and directions. The arrival angle samples different distances and the corresponding most probable primary cosmic ray energy. The larger and larger distances (between observer and C.R. interaction) make wider and wider the shower area and it enlarge the probability to be observed (up to three order of magnitude more than vertical showers); the observation of a maximal electromagnetic shower development may amplify the signal by two-three order of magnitude (respect suppressed shower at sea level); the peculiar altitude-angle range (ten-twenty km. height and ≃ 80 o − 90 o zenith angle) may disentangle at best the primary cosmic ray energy and composition. Even from existing mountain observatory the up-going air-showers may trace , above the horizons, PeV-EeV high energy cosmic rays and , below the horizons, PeV-EeV neutrino astronomy: their early signals may be captured in already existing gamma telescopes as Magic at Canarie, while facing the Earth edges during (useless) cloudy nights.

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“…The geometrical factor was deduced from the simulation. The differential and integral spectra of cosmic rays were taken from [14] and [15]. A minimum momentum cut of 0.2 GeV/c was used to allow for the two lead shields.…”

Section: Geometric Factor and Intrinsic Efficiencymentioning

confidence: 99%

Development of a compact scintillator hodoscope with wavelength-shifting fibre read-out

Achenbach

Cobb

Wahl

2005

Nuclear Instruments and Methods in Physics Research Section A:

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We report on the prototyping of a plastic scintillator hodoscope with wavelengthshifting fibre read-out by a multi-anode photomultiplier as part of the development of a detector for cosmic ray muons to be carried aboard an aircraft. Light yield and light attenuation measurements on single-and double-clad wavelength-shifting fibres were performed. Low power, low-threshold, discriminators were designed. A prototype 16-channel hodoscope with two planes was built and tested with cosmic rays. After correcting for geometrical factors a global intrinsic efficiency of ǫ > 98 % was obtained in both planes. The overall performance of the hodoscope proved it to be well suited for the Adler experiment to measure the high altitude muon flux.

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Cosmic Rays in the Atmosphere

Cited by 34 publications

References 185 publications

The Temperature Effect in Secondary Cosmic Rays (Muons) Observed at the Ground: Analysis of the Global Muon Detector Network Data

The Temperature Effect in Secondary Cosmic Rays (Muons) Observed at the Ground: Analysis of the Global Muon Detector Network Data

Air-shower spectroscopy at horizons

Development of a compact scintillator hodoscope with wavelength-shifting fibre read-out

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