Composition and energy spectra of cosmic-ray primaries in the energy range 1013–1015 eV/particle observed by Japanese–Russian joint balloon experiment

Apanasenko, A.V.; Sukhadolskaya, V. A.; Derbina, V. A.; Fujii, Masami; Galkine, V. I.; Getsov, G. G.; Hareyama, M.; Ichimura, M.; Ito, S.; Kamioka, Eiji; Kitami, T.; Kobayashi, Tadashi; Kolesnikov, V. D.; Kopenkin, V.; Kotunova, N.M.; Kuramata, S.; Kuriyama, Y.; Lapshin, V. I.; Managadze, A. K.; Matsutani, H.; Mikami, Hideki; Misnikova, N. P.; Mukhamedshin, R. A.; Namiki, M.; Nanjo, H.; Nazarov, S. N.; Nikolsky, S. I.; Ohe, Toshihito; Ohta, Shigeo; Оседло, В. И.; Oshuev, D. S.; Podorozhny, D.; Publichenko, P. A.; Rakobolskaya, I.V.; Роганова, Т. М.; Saito, Miho; Sazhina, G. P.; Semba, H.; Shabanova, Yu N.; Shibata, T.; Sugimoto, H.; Свешникова, Л.; Takahashi, K.; Tsuchiya, Takeshi; Таран, Віталій Михайлович; Yajima, N.; Yamagami, T.; Yamamoto, Kazuhiro; Yashin, I. V.; Zamchalova, E. A.; Зацепин, Г. Т.; Zayarnaya, I. S.

doi:10.1016/s0927-6505(00)00163-8

Cited by 151 publications

(39 citation statements)

References 29 publications

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“…All particle spectrum. Points -data of direct and EAS experiments [18,[26][27][28][29][30][31]. Solid line -spectrum of used primary model, dotted line -spectrum of background cosmic ray flux.…”

Section: Resultsmentioning

confidence: 99%

“…Energy spectrum of helium nuclei. Points -data of direct experiments [17,18,25,27,[32][33][34]. Dotted line -background spectrum, dashed line -spectrum from individual supernova remnant.…”

Section: Resultsmentioning

confidence: 99%

“…Energy spectrum of Fe-group. Points -data of direct experiments [16,18,26,27,35,36]. Solid line -model spectrum.…”

Section: Resultsmentioning

confidence: 99%

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Multiplicity spectrum of muon bundles and primary CR composition in the range 1 – 10000 TeV

Petkov

Szabelski

Gaponenko

et al. 2013

EPJ Web of Conferences

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Abstract. Multiplicity spectrum of muon bundles underground, with E µ ≥ f ew × 100 GeV, is an effective tool for study of primary Cosmic Ray spectrum and composition in wide range of the primary energies. In this paper we study integral muon number distribution measured at the Baksan Underground Scintillation Telescope (BUST). The analyzed range of the number of muon tracks crossing BUST (1 -170) approximately corresponds to the primary energy range 1 − 10 4 TeV. The analysis shows that non-power law primary spectra are preferable below the knee. Such a spectrum can be obtained as superposition of the basic power law primary spectrum and an additional component from nearby supernova remnant in the Galaxy.

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Section: Resultsmentioning

confidence: 99%

“…Energy spectrum of helium nuclei. Points -data of direct experiments [17,18,25,27,[32][33][34]. Dotted line -background spectrum, dashed line -spectrum from individual supernova remnant.…”

Section: Resultsmentioning

confidence: 99%

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Multiplicity spectrum of muon bundles and primary CR composition in the range 1 – 10000 TeV

Petkov

Szabelski

Gaponenko

et al. 2013

EPJ Web of Conferences

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“…Since there is significant overlap between the MMDs for the Al and the Fe groups, thus these two species have been combined by assuming an abundance ratio (Al/Fe) of 0.8 based on one of the direct measurements [99]. Since the abundance ratio Al/Fe was fixed, therefore, effectively the number of independent mass species were reduced to four resulting in a relatively rapid convergence during the minimization procedure.…”

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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“…1. As a result of the experimental data processing it was noted that the primary protons are identified in about half of the events related to the nucleon-nucleus interactions [1]. The single charged particle tracks are detected by nuclear emulsion with close to 100% efficiency (it is based on tracing the secondary π ± mesons as well as primary protons through the emulsion layers).…”

Section: Introductionmentioning

confidence: 99%

The search for primary particle tracks in nucleon-nucleus interactions with gamma ray energy ΣE_γ ≥ 3 TeV registered in stratospheric X-ray emulsion chambers using data of the RUNJOB experiment

Zayarnaya

Irkhina

2017

EPJ Web Conf.

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Abstract. We present here the result of a retreatment of data from the RUNJOB (RUssia-Nippon JOint Balloon) experiment of nucleon-nucleus interactions registered in stratospheric X-ray emulsion chambers (REC) using a new method for searching and tracing of galactic particles in nuclear emulsions. In about halfcof these interactions (∼ 50) recorded in REC RUNJOB'96-3B, RUNJOB'97-6A and RUNJOB'99-11A,B with energy released in the electromagnetic component E γ ≥ 3 TeV and E γ ≥ 5 TeV respectively, single charged particle tracks are not found within the search area defined individually by the particle track location accuracy. The absence of primary proton tracks is consistent with the original treatment of the RUNJOB experimental data.There is a difference in the zenith angular distribution for two groups of events in which a single charged particle track is observed or absent. The average penetration depth of the primary particles in REC to the interaction vertex in the zenith angle range from 60 • to 79 • differs by a factor two for these groups.

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Composition and energy spectra of cosmic-ray primaries in the energy range 1013–1015 eV/particle observed by Japanese–Russian joint balloon experiment

Cited by 151 publications

References 29 publications

Multiplicity spectrum of muon bundles and primary CR composition in the range 1 – 10000 TeV

Multiplicity spectrum of muon bundles and primary CR composition in the range 1 – 10000 TeV

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

The search for primary particle tracks in nucleon-nucleus interactions with gamma ray energy ΣE_γ ≥ 3 TeV registered in stratospheric X-ray emulsion chambers using data of the RUNJOB experiment

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Composition and energy spectra of cosmic-ray primaries in the energy range 1013–1015 eV/particle observed by Japanese–Russian joint balloon experiment

Cited by 151 publications

References 29 publications

Multiplicity spectrum of muon bundles and primary CR composition in the range 1 – 10000 TeV

Multiplicity spectrum of muon bundles and primary CR composition in the range 1 – 10000 TeV

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

The search for primary particle tracks in nucleon-nucleus interactions with gamma ray energy ΣEγ ≥ 3 TeV registered in stratospheric X-ray emulsion chambers using data of the RUNJOB experiment

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The search for primary particle tracks in nucleon-nucleus interactions with gamma ray energy ΣE_γ ≥ 3 TeV registered in stratospheric X-ray emulsion chambers using data of the RUNJOB experiment