Cosmic-ray muons in the deep ocean

Babson, J.; Barish, B.; Becker‐Szendy, R.; Bradner, H.; Cady, R.; Clem, J.; Dye, S. T.; Gaidos, J. A.; Gorham, P. W.; Grieder, P. K. F.; Jaworski, M.; Kitamura, Takashi; Kropp, W. R.; Learned, J. G.; Matsuno, S.; March, R.; Mitsui, K.; O’Connor, Daniel; Ōhashi, Y.; Okada, Atsushi; Peterson, V. Z.; Price, L. R.; Reines, F.; Roberts, A.; Roos, C. E.; Sobel, H. W.; Stenger, V. J.; Webster, Michael S.; Wilson, C.

doi:10.1103/physrevd.42.3613

Cited by 106 publications

(64 citation statements)

References 18 publications

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“…When comparing results on atmospheric muons at large depths obtained for pure and sea water the data are recalculated to each other using value ρ = 1.027 g cm − 3 as a sea water density (Ref. [38,39]). The difference between pure and sea water is negligible small for the muon propagation if one works in water equivalent units which was tested by us up to slant depth D = 10 km w.e.…”

Section: Selected Results and Comparison With Other Algorithmsmentioning

confidence: 99%

MUM: Flexible precise Monte Carlo algorithm for muon propagation through thick layers of matter

2001

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We present a new Monte Carlo muon propagation algorithm MUM (MUons+Medium) which possesses some advantages over analogous algorithms presently in use. The most important features of algorithm are described. Results on the test for accuracy of treatment the muon energy loss with MUM are presented and analyzed. It is evaluated to be of 2×10 −3 or better, depending upon simulation parameters. Contributions of different simplifications which are applied at Monte Carlo muon transportation to the resulting error are considered and ranked. It is shown that when simulating muon propagation through medium it is quite enough to account only for fluctuations in radiative energy loss with fraction of energy lost being as large as 0.05÷0.1. Selected results obtained with MUM are given and compared with ones from other algorithms. PACS number(s): 13.85Tp, 96.40.Tv, 02.70Lq

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Section: Selected Results and Comparison With Other Algorithmsmentioning

confidence: 99%

MUM: Flexible precise Monte Carlo algorithm for muon propagation through thick layers of matter

2001

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“…Even though angular distributions of atmospheric muons have been published by practically all largevolume neutrino detectors and prototypes [75,76,77,78,79,80,81,82], none of the measurements is accurate enough to provide a strict external constraint. For the time being, there is no other choice than to note the effect and continue to investigate possible explanations.…”

Section: Discussionmentioning

confidence: 99%

Characterization of the atmospheric muon flux in IceCube

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Astroparticle Physics

101

117

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Muons produced in atmospheric cosmic ray showers account for the by far dominant part of the event yield in large-volume underground particle detectors. The IceCube detector, with an instrumented volume of about a cubic kilometer, has the potential to conduct unique investigations on atmospheric muons by exploiting the large collection area and the possibility to track particles over a long distance. Through detailed reconstruction of energy deposition along the tracks, the characteristics of muon bundles can be quantified, and individual particles of exceptionally high energy identified. The data can then be used to constrain the cosmic ray primary flux and the contribution to atmospheric lepton fluxes from prompt decays of short-lived hadrons.In this paper, techniques for the extraction of physical measurements from atmospheric muon events are described and first results are presented. The multiplicity spectrum of TeV muons in cosmic ray air showers for primaries in the energy range from the knee to the ankle is derived and found to be consistent with recent results from surface detectors. The single muon energy spectrum is determined up to PeV energies and shows a clear indication for the 2 emergence of a distinct spectral component from prompt decays of short-lived hadrons. The magnitude of the prompt flux, which should include a substantial contribution from light vector meson di-muon decays, is consistent with current theoretical predictions.The variety of measurements and high event statistics can also be exploited for the evaluation of systematic effects. In the course of this study, internal inconsistencies in the zenith angle distribution of events were found which indicate the presence of an unexplained effect outside the currently applied range of detector systematics. The underlying cause could be related to the hadronic interaction models used to describe muon production in air showers.

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“…This is a reach equivalent to that of a hypothetical astronomical telescope sensitive to wavelengths from radio to X-rays. Above 10 5 TeV the observations are free of muon and neutrino backgrounds produced in cosmic ray interactions with the Earth's atmosphere. Each neutrino is a discovery.…”

Section: Introductionmentioning

confidence: 96%

“…Adding to the technological challenge is the requirement that the detector be shielded from the abundant flux of cosmic ray muons by deployment at a depth of typically several kilometers. After the cancellation of a pioneering attempt [5] to build a neutrino telescope off the coast of Hawaii, successful operation of a smaller instrument in Lake Baikal [6] bodes well for several efforts to commission neutrino telescopes in the Mediterranean [5,7]. We will here mostly concentrate on the construction and first four years of operation of the AMANDA telescope [4,8] which has transformed a large volume of natural deep Antarctic ice into a Cherenkov detector.…”

Section: Introductionmentioning

confidence: 99%

Cosmic neutrinos from the sources of galactic and extragalactic cosmic rays

Halzen

2007

Astrophys Space Sci

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Although kilometer-scale neutrino detectors such as IceCube are discovery instruments, their conceptual design is very much anchored to the observational fact that Nature produces protons and photons with energies in excess of 10 20 eV and 10 13 eV, respectively. The puzzle of where and how Nature accelerates the highest energy cosmic particles is unresolved almost a century after their discovery. From energetics considerations we anticipate order 10 ∼ 100 neutrino events per kilometer squared per year pointing back at the source(s) of both galactic and extragalactic cosmic rays. In this context, we discuss the results of the AMANDA and IceCube neutrino telescopes which will deliver a kilometersquare-year of data over the next 3 years.

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Cosmic-ray muons in the deep ocean

Cited by 106 publications

References 18 publications

MUM: Flexible precise Monte Carlo algorithm for muon propagation through thick layers of matter

MUM: Flexible precise Monte Carlo algorithm for muon propagation through thick layers of matter

Characterization of the atmospheric muon flux in IceCube

Cosmic neutrinos from the sources of galactic and extragalactic cosmic rays

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