Cosmic-Ray Spectra and Composition in the Energy Range of 10-1000 TeV per Particle Obtained by the RUNJOB Experiment

Derbina, V. A.; Галкин, В. И.; Hareyama, M.; Hirakawa, Yuichi; Horiuchi, Y.; Ichimura, M.; Inoue, N.; Kamioka, Eiji; Kobayashi, Tadashi; Kopenkin, V.; Kuramata, S.; Managadze, A. K.; Matsutani, H.; Misnikova, N. P.; Mukhamedshin, R. A.; Nagasawa, S.; Nakano, R.; Namiki, M.; Nakazawa, Makoto; Nanjo, H.; Nazarov, S. N.; Ohata, Sho; Ohtomo, Hiromi; Оседло, В. И.; Oshuev, D. S.; Publichenko, P. A.; Rakobolskaya, I.V.; Роганова, Т. М.; Saito, Carlos Hiroo; Sazhina, G. P.; Semba, H.; Shibata, T.; Shuto, D.; Sugimoto, H.; Suzuki, Ryo; Свешникова, Л.; Таран, Віталій Михайлович; Yajima, N.; Yamagami, T.; Yashin, I. V.; Zamchalova, E. A.; Зацепин, Г. Т.; Zayarnaya, I. S.

doi:10.1086/432715

Cited by 139 publications

(99 citation statements)

References 16 publications

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“…This is the standard lore in the field, although it is expected to give a biased with φ = 600 MV; CAPRICE94 (Boezio et al 1999) and CAPRICE98 (Boezio et al 2003) with φ = 650 MV and 600 MV respectively; IMAX (Menn et al 2000) with φ = 750 MV; and the series of BESS balloon flights BESS93 (Wang et al 2002) BESS97 (Shikaze et al 2007), BESS98 (Sanuki et al 2000;Shikaze et al 2007), BESS99 (Shikaze et al 2007), BESS00 (Shikaze et al 2007), and BESS02 (BESS-TeV, Haino et al 2004;Shikaze et al 2007), for which φ = 700 MV, 491 MV, 591 MV, 658 MV, 1300 MV, 1109 MV respectively. The intermediate and high-energy data are: ATIC-2 (Panov et al 2009), CREAM-I (Ahn et al 2010a), JACEE (Asakimori et al 1998), MUBEE (Zatsepin et al 1993), RICH-II (Diehl et al 2003), RUNJOB (Derbina et al 2005), SOKOL (Ivanenko et al 1993), and Ichimura et al (1993). modulation level (for example, we do not know the true interstellar proton spectrum, there is the problem of polarity in the solar magnetic field, etc.).…”

Section: Datamentioning

confidence: 99%

p, He, and C to Fe cosmic-ray primary fluxes in diffusion models

Putze

Maurin

Donato

2011

A&A

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Context. The source spectrum of cosmic rays is not well determined by diffusive shock acceleration models. The propagated fluxes of proton, helium, and heavier primary cosmic-ray species (up to Fe) are a means to indirectly access it. But how robust are the constraints, and how degenerate are the source and transport parameters? Aims. We check the compatibility of the primary fluxes with the transport parameters derived from the B/C analysis, but also ask whether they add further constraints. We study whether the spectral shapes of these fluxes and their ratios are mostly driven by source or propagation effects. We then derive the source parameters (slope, abundance, and low-energy shape). Methods. Simple analytical formulae are used to address the issue of degeneracies between source/transport parameters, and to understand the shape of the p/He and C/O to Fe/O data. The full analysis relies on the USINE propagation package, the MINUIT minimisation routines (χ 2 analysis) and a Markov Chain Monte Carlo (MCMC) technique. Results. Proton data are well described in the simplest model defined by a power-law source spectrum and plain diffusion. They can also be accommodated by models with, e.g., convection and/or reacceleration. There is no need for breaks in the source spectral indices below ∼1 TeV/n. Fits to the primary fluxes alone do not provide physical constraints on the transport parameters. If we leave the source spectrum free, parametrised by the form dQ/dE = qβ η S R −α , and fix the diffusion coefficient K(R) = K 0 β η T R δ so as to reproduce the B/C ratio, the MCMC analysis constrains the source spectral index α to be in the range 2.2−2.5 for all primary species up to Fe, regardless of the value of the diffusion slope δ. The values of the parameter η S describing the low-energy shape of the source spectrum are degenerate with the parameter η T describing the low-energy shape of the diffusion coefficient: we find η S − η T ≈ 0 for p and He data, but η S − η T ≈ 1 for C to Fe primary species. This is consistent with the toy-model calculation in which the shape of the p/He and C/O to Fe/O data is reproduced if η S − η T ≈ 0−1 (no need for different slopes α). When plotted as a function of the kinetic energy per nucleon, the low-energy p/He ratio is determined mostly by the modulation effect, whereas primary/O ratios are mostly determined by their destruction rate. Conclusions. Models based on fitting B/C are compatible with primary fluxes. The different spectral indices for the propagated primary fluxes up to a few TeV/n can be naturally ascribed to transport effects only, implying universality of elemental source spectra.

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Section: Datamentioning

confidence: 99%

p, He, and C to Fe cosmic-ray primary fluxes in diffusion models

Putze

Maurin

Donato

2011

A&A

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“…The charge ratio is expected to increase as a consequence of the increasing kaon contribution to the muon flux because in high energy interactions, single K + 's can be produced in associated production with strange baryons while single K − 's cannot. The muon charge ratio is expected to decrease at even higher energies due to heavy flavor production [3,4] and changes in composition of the cosmic-ray primaries [5][6][7]. However, as these latter two processes are expected to only affect the charge ratio at energies greater than those studied here they are not considered further.…”

Section: Introductionmentioning

confidence: 99%

Measurement of the underground atmospheric muon charge ratio using the MINOS Near Detector

Adamson¹,

Andreopoulos²,

Auty³

et al. 2011

Phys. Rev. D

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The magnetized MINOS Near Detector, at a depth of 225 meters of water equivalent (mwe), is used to measure the atmospheric muon charge ratio. The ratio of observed positive to negative 2 atmospheric muon rates, using 301 days of data, is measured to be 1.266 ± 0.001(stat.) +0.015 −0.014 (syst.). This measurement is consistent with previous results from other shallow underground detectors, and is 0.108 ± 0.019(stat. + syst.) lower than the measurement at the functionally identical MINOS Far Detector at a depth of 2070 mwe. This increase in charge ratio as a function of depth is consistent with an increase in the fraction of muons arising from kaon decay for increasing muon surface energies.PACS numbers: 13.85. Tp. 95.55.Vj, 95.85.Ry

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“…A comparison of the GRAPES-3 all-particle energy spectrum with the direct observations [94][95][96][98][99][100] as seen in Fig. 26 also display good agreement, except for the RUNJOB results [99].…”

Section: High Energy Astroparticle Physics At Ooty and The Grapes-3 Ementioning

confidence: 73%

“…25. The H and He data are taken from [94,95,[98][99][100] and the N, Al and Fe data from [5,95,99,100]. …”

Section: S K Guptamentioning

confidence: 99%

High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

Gupta¹

2014

Proceedings of the Indian National Science Academy

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The astroparticle studies at Ooty have their roots going way back into the fifties, when studies using cosmic rays were initiated with cloud chambers of progressively larger sizes as the primary detector and measuring device to obtain properties of hadrons at high energies. This study was subsequently strengthened with the installation of a total absorption calorimeter and a modest extensive air shower array to probe the composition of the primary cosmic rays to very high energies. The discovery of pulsars provided a thrust for the exploration of these compact objects as the sources of γ-rays at TeV energies with the aid of atmospheric Cerenkov detectors in the seventies. With the rapid technological advances occurring during the subsequent years in detectors, electronics and computers, physicists world-wide were able to set up very large and remarkably sensitive experiments that were hard to imagine a decade earlier. With the increasing sophistication and complexity the modern experiments require participation of very large teams of scientists. This development has made the formation of collaboration of large number of physicists both experimental and theoretical, engineers, technicians etc., from a number of institutions and universities, a prerequisite for setting up any major experimental facility. The GRAPES-3 experiment is a collaboration of 34 scientists from 13 institutions, including 8 from India and 5 from Japan. The GRAPES-3 experiment contains a dense extensive air shower array operating with ~ 400 scintillator detectors and a 560 m 2 tracking muon detector (Em > 1 GeV), at Ooty in India. 25 % of scintillator detectors are instrumented with two fast photomultiplier tubes (PMTs) for extending the dynamic range to ~ 5x10 3 particles m -2. The scintillators, signal processing electronics and data recording systems were fabricated in-house to cut costs and optimize performance. The muon multiplicity distribution of the EAS is used to probe the composition of primary cosmic rays below the 'knee', with an overlap with direct measurements. Search for multi-TeV γ-rays from point sources is done with the aid of the muon detector. A good angular resolution of 0.7 o at 30 TeV, is measured from shadow of the Moon on the isotropic flux of cosmic rays. Sensitive limit on the diffuse flux of 100 TeV γ-rays is placed by using muon detector to filter out the charged cosmic ray background. The tracking muon detector allows sensitive measurements on the coronal mass ejections and solar flares through Forbush decrease events. We have major expansion plans to enhance the sensitivity of the GRAPES-3 experiment in the areas listed above. PACS

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Cosmic-Ray Spectra and Composition in the Energy Range of 10-1000 TeV per Particle Obtained by the RUNJOB Experiment

Cited by 139 publications

References 16 publications

p, He, and C to Fe cosmic-ray primary fluxes in diffusion models

p, He, and C to Fe cosmic-ray primary fluxes in diffusion models

Measurement of the underground atmospheric muon charge ratio using the MINOS Near Detector

High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

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