Measurements of the charge ratio of cosmic-ray muons

Aurela, A.M.; MacKeown, P. K.; Wolfendale, A. W.

doi:10.1088/0370-1328/89/2/321

Cited by 15 publications

(5 citation statements)

References 18 publications

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“…The atmospheric muon flux and energy spectrum was also measured using the precise Reference p µ [GeV/c] B H& T PDG [13] 15.1 -82.1 X 0.79 [14] 20-500 X X [15] 11 -810 X X [52] 3-3000 X 0.933 X [19] 10-150 X 0.858 [7] 20-1000…”

Section: Experimental Setupsmentioning

confidence: 99%

Atmospheric muons: experimental aspects

Cecchini

Spurio

2012

Preprint

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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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Section: Experimental Setupsmentioning

confidence: 99%

Atmospheric muons: experimental aspects

Cecchini

Spurio

2012

Preprint

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“…• Absolute ground-based measurements with MARS apparatus in Durham (Aurela et al [7], Ayre et al [12]); Nottingham spectrograph (Baber et al [8], Rastin [14]); spectrometer near College Station, Texas (Bateman et al [9]); Kiel spectrographs (Allkofer et al [10]), MASS apparatus at Prince Albert, Saskatchewan (De Pascale et al [15]); EAS-TOP array at Campo Imperatore, Gran Sasso (Aglietta et al [17]).…”

Section: Parametrization Of the Calculated Pm Fluxmentioning

confidence: 99%

“…Refs. [7][8][9][10][11][12][13][14][15][16][17] for the vertical muon flux, Refs. [18,19] for near-horizontal flux, and Ref.…”

Section: Introductionmentioning

confidence: 99%

“…There is a need to piece together all these data in order to extract some physical inferences thereof. Also, it would be useful to correlate the underground and underwater data with the results of the mentioned direct measurements of the sea-level muon spectrum [7][8][9][10][11][12][13][14][15][16][17] as well as with the data deduced by indirect routes [33,36,37,44,[60][61][62][63][64][65][66].…”

Section: Introductionmentioning

confidence: 99%

“…π,K-muons + PM (QGSM) 3 -π,K-muons + PM (RQPM) 4 -π,K-muons + PM (VFGS) Vertical integral momentum spectrum of muons at sea level. The direct data are taken from Refs [7,8,11,12,14,15,17]. and indirect (underground) data are from Refs.…”

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confidence: 99%

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Atmospheric muon flux at sea level, underground, and underwater

et al. 1998

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The vertical sea-level muon spectrum at energies above 1 GeV and the muon intensities at depths up to 18 km w.e. in different rocks and in water are calculated. The results are particularly collated with a great body of the ground-level, underground, and underwater muon data. In the hadron-cascade calculations, we take into account the logarithmic growth with energy of inelastic cross sections and pion, kaon, and nucleon generation in pion-nucleus collisions. For evaluating the prompt muon contribution to the muon flux, we apply the two phenomenological approaches to the charm production problem: the recombination quark-parton model and the quark-gluon string model. We give simple fitting formulas describing our numerical results. To solve the muon transport equation at large depths of a homogeneous medium, we use a semianalytical method, which allows the inclusion of an arbitrary (decreasing) muon spectrum at the medium boundary and real energy dependence of muon energy losses. Our analysis shows that at the depths up to 6-7 km w.e., essentially all underground data on the muon flux correlate with each other and with the predicted one for conventional (π, K)-muons, to within 10 %. However, the high-energy sea-level muon data as well as the data at high depths are contradictory and cannot be quantitatively described by a single nuclear-cascade model.

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Die Höhen‐ und Zenitwinkelabhängigkeit der Energiespektren von Ultrastrahlungsteilchen

Allkofer

1967

Fortschr. Phys.

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ZusammenfassungDie Energiespektren der kosmischen Strahlung sind von zweifacher Bedeutung. Einmal stellen sie eine wichtige ,,Konstante" der kosmischen Strahlung dar, zum andern lassen sich durch Vergleich der Spektren in verschiedenen Hohenbereichen der Atmosphare Ruckschlusse auf die Wechselwirkungsprozesse ableiten, die beim Weg der Ultrastrahlung durch die Atmosphare statthden. Die gangigen apparativen Methoden reichen zwar im allgemeinen aus, Energiespektren auf Meereshohe zu untersuchen, sie sind jedoch in ihrem Aufbau meistens zu kompliziert und in ihren Dimensionen zu g r d , um damit Messungen auf Hohenlabors oder in Flugzeugen durchfuhren zu konnen. Erst durch neuere Detektortechniken ist es moglich geworden, Ultrastrahlungsspektrometer so zu konstruieren, da13 auch in groBeren Hohenbereichen Messungen von Spektren vorgenommen werden konnen. Dementsprechend ist das Material uber die Hohenabhangigkeiten von Spektren irn Vergleich zu den Spektren auf Meereshohe weit dudtiger. Trotzdem gibt es eine Reihe von Untersuchungen von Spektren in verschiedenen Hohenbereichen, die jedoch in ihren Resultaten nicht immer ubereinstimmen .

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Measurements of the charge ratio of cosmic-ray muons

Cited by 15 publications

References 18 publications

Atmospheric muons: experimental aspects

Atmospheric muons: experimental aspects

Atmospheric muon flux at sea level, underground, and underwater

Die Höhen‐ und Zenitwinkelabhängigkeit der Energiespektren von Ultrastrahlungsteilchen

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