Browsing by Autor "N. Inoue"
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Item type: Item , A halo event observed by hybrid detectors at Mt. Chacaltaya(Elsevier BV, 2003) Hiroshi Aoki; K. Hashimoto; K. Honda; N. Inoue; N. Kawasumi; N. Martinić; C. E. Navia; N. Ohmori; A. Ohsawa; L. C. S. OliveiraItem type: Item , A Halo Event observed by the Hybrid Experiment at Mt. Chacaltaya(Elsevier BV, 2005) Hiroshi Aoki; K. Hashimoto; K. Honda; N. Inoue; N. Kawasumi; N. Martinić; Christopher O'; Nobuaki Ochi; N. Ohmori; A. OhsawaItem type: Item , A halo event observed with an emulsion chamber and air shower array at Mt Chacaltaya(IOP Publishing, 2004) Hiroshi Aoki; K. Hashimoto; K. Honda; N. Inoue; N. Kawasumi; N. Martinić; Christopher O'; Nobuaki Ochi; N. Ohmori; A. OhsawaA hybrid experiment to operate simultaneously an air shower array, a hadron calorimeter and an emulsion chamber is under way at Mt Chacaltaya (5200 m, Bolivia). An event with a halo, a blackened area of ~1 cm on x-ray film of the emulsion chamber, was observed with the experiment. Information about the halo (Ehalo = 850 TeV) and on high energy particles of electromagnetic and hadronic components outside the halo (?E? = 632.5 TeV and ?E(?)h = 278.8 TeV with a detection threshold of 2 TeV) was obtained from emulsion chamber data. Details about low energy hadrons were determined from the hadron calorimeter data, and characteristics of the accompanying air shower (Ne = 7.0 ? 107, s = 0.59) were determined by the air shower array. We reconstruct the event, based on the observed data. The event is compared with simulated events, which supports the conclusion that nuclear interactions change their characteristics in the high energy region so as to result in stronger energy subdivision.Item type: Item , A systematic study of the hybrid experiment at Mt.Chacaltaya(EDP Sciences, 2013) M. Tamada; Hiroshi Aoki; K. Honda; N. Inoue; N. Kawasumi; N. Martinić; Nobuaki Ochi; N. Ohmori; A. Ohsawa; H. SembaIn the hybrid experiment on Mt.Chacaltaya, we can observe three different components of airshowers, that is, air-shower size, burst-density and high energy families (a bundle of high energy particles). Burst-density in each block of hadron calorimeters are newly recalculated in simulations in oder to compare directly to the experimental data. Energy deposits in the scintillators of the hadron calorimeters are calculated using GEANT4 for every particle, incident upon the hadron calorimeter, in the air-showers simulated using CORSIKA, and are converted into burst-density, taking into consideration the exact structure of experimental hadron calorimeter. We study correlations among three observable components in the air-showers. Correlations between air-shower size and burst-density and those between air-shower size and accompanied family energy can be explained by model calculations by adjusting primary particle composition, the former correlation is in favor of proton-primaries but the latter iron-primaries. No model can describe well observed correlations between burst-density and family energy. That is, the observed family energy accompanied by the air-showers with larger burst-density is systematically smaller than that expected in the simulated events. Effects of a fluctuation in the cross-section of hadronic interactions are studied to settle the disagreement between experimental data and simulations.Item type: Item , A systematic study of the hybrid experiment at Mt.Chacaltaya(EDP Sciences, 2013) M. Tamada; Hiroshi Aoki; K. Honda; N. Inoue; N. Kawasumi; N. Martinić; Nobuaki Ochi; N. Ohmori; A. Ohsawa; H. SembaIn the hybrid experiment on Mt.Chacaltaya, we can observe three different components of airshowers, that is, air-shower size, burst-density and high energy families (a bundle of high energy particles). Burst-density in each block of hadron calorimeters are newly recalculated in simulations in oder to compare directly to the experimental data. Energy deposits in the scintillators of the hadron calorimeters are calculated using GEANT4 for every particle, incident upon the hadron calorimeter, in the air-showers simulated using CORSIKA, and are converted into burst-density, taking into consideration the exact structure of experimental hadron calorimeter. We study correlations among three observable components in the air-showers. Correlations between air-shower size and burst-density and those between air-shower size and accompanied family energy can be explained by model calculations by adjusting primary particle composition, the former correlation is in favor of proton-primaries but the latter iron-primaries. No model can describe well observed correlations between burst-density and family energy. That is, the observed family energy accompanied by the air-showers with larger burst-density is systematically smaller than that expected in the simulated events. Effects of a fluctuation in the cross-section of hadronic interactions are studied to settle the disagreement between experimental data and simulations.Item type: Item , Arrival directions of large air showers, low-mu showers and old-age low-mu air showers observed at St. Chacaltaya(NASA Headquarters, 1985) T. Kaneko; K. Hagiwara; H. Yoshii; N. Martinić; L. Siles; P. Miranda; F. Kakimoto; Toru Obara; N. Inoue; K. SugaArrival directions of air showers with primary energies in the range 10 to the 16.5 power eV to 10 to the 18th power eV show the first harmonic in right ascension (RA) with amplitude of 2.7 + or - 1.0% and phase of 13-16h. However, the second harmonic in RA slightly seen for showers in the range 10 to the 18th power eV to 10 to the 19th power eV disappeared by accumulation of observed showers. The distribution of arrival directions of low-mu air showers with primary energies around 10 to the 15th power eV observed at Chacaltaya from 1962 to 1967 is referred to, relating to the above-mentioned first harmonic. Also presented in this paper are arrival directions of old-age low-mu air showers observed at Chacaltaya from 1962 to 1967, for recent interest in gamma-ray air showers.Item type: Item , Arrival-time distribution of muons and electrons in large air showers observed at 5200m above sea level(American Institute of Physics, 1979) C. Aguirre; R. Anda; A. Trepp; F. Kakimoto; Y. Mizumoto; K. Suga; N. Izu; Y. Kamouchi; N. Inoue; Shinsuke KawaiAn experiment is going on at Mt. Chacaltaya in Bolivia (550 gcm−2 atmospheric depth) to observe arrival‐time distributions of muons and electrons in air showers above 1017 eV to study the early stage of longitudinal development related directly with the character of nuclear interactions and the composition of primary cosmic rays at these high energies. The preliminary results are presented at the Seminar.Item type: Item , Cosmic ray nuclear interactions and EAS-triggered families observed by the Chacaltaya hybrid experiment(Elsevier BV, 2008) Hiroshi Aoki; K. Honda; N. Inoue; Takaaki Ishii; N. Kawasumi; N. Martinić; Nobuaki Ochi; N. Ohmori; A. Ohsawa; M. TamadaItem type: Item , Energetic delayed hadrons in large air showers observed at 5200m above sea level(1985) T. Kaneko; K. Hagiwara; H. Yoshii; N. Martinić; L. Siles; P. Miranda; F. Kakimoto; I. Tsuchimoto; N. Inoue; K. SugaEnergetic delayed hadrons in air showers with electron sizes in the range 10 to the 6th power to 10 to the 9th power were studied by observing the delayed bursts produced in the shield of nine square meter scintillation detectors in the Chacaltaya air-shower array. The frequency of such delayed burst is presented as a function of electron size, core distance and sec theta.Item type: Item , Simultaneous observation of families and accompanied air showers at Mt. Chacaltaya(American Physical Society, 1996) N. Kawasumi; I. Tsushima; K. Honda; K. Hashimoto; T. Matano; N. Inoue; K. Mori; A. Ohsawa; M. Tamada; N. OhmoriSimultaneous observations of families and accompanied air showers with emulsion chambers and the air shower array of electronic equipment at Mt. Chacaltaya (5200 m, 540 g/${\mathrm{cm}}^{2}$) reveal that families bear the data of nuclear interactions generated deep in the atmosphere. 47 outstanding families with \ensuremath{\Sigma}${\mathit{E}}_{\ensuremath{\gamma}}$\ensuremath{\ge}10 TeV are correlated with the accompanied air showers of the size ${10}^{5}$--${10}^{8}$. A scatter plot of the average family energy versus the size of the relative air shower requires further energy fractionizing process(es) in the propagation of high energy cosmic rays in the atmosphere, such as a larger dissipative mechanism in nuclear interaction, heavier chemical composition of the primary cosmic rays, etc. We reach the conclusion that nuclear interaction changes its features in the energy region ${\mathit{E}}_{0}$\ensuremath{\gtrsim}${10}^{16}$ eV, because the heavier composition, proposed so far, is not sufficient for the required dissipative process. A comparison with the data from the HADRON experiment at a similar altitude with a similar technique shows that no larger deviations are present between both experiments. \textcopyright{} 1996 The American Physical Society.Item type: Item , Simultaneous observation of families and accompanied air showers at Mt. Chacaltaya I(Elsevier BV, 1997) K. Honda; N. Kawasumi; I. Tsushima; K. Hashimoto; T. Nishida; T. Matano; N. Inoue; A. Ohsawa; M. Tamada; N. OhmoriItem type: Item , Simultaneous observation of families and accompanied air showers at Mt. Chacaltaya II(Elsevier BV, 1997) C. Aguirre; K. Hashimoto; K. Honda; N. Inoue; N. Kawasumi; N. Martinic; T. Matano; N. Ohmori; A. Ohsawa; F. OscoItem type: Item , Simultaneous observation of families and accompanied air showers at Mt. Chacaltaya. II. Study of the hadronic component in air showers(American Physical Society, 2000) C. Aguirre; Hiroshi Aoki; K. Hashimoto; K. Honda; N. Inoue; N. Kawasumi; Yoshikazu Maeda; N. Martinić; T. Matano; N. OhmoriAn experimental setup of an air shower array, hadron calorimeter, and emulsion chamber is being carried out at Mt. Chacaltaya (5200 m, Bolivia), in order to study the hadron interaction and the primary cosmic rays in the energy region exceeding ${10}^{15}$ eV. The number of hadrons in the air shower, detected by the hadron calorimeter, is discussed mainly in this paper. A comparison with the simulation shows that the number of hadrons in the air shower is not compatible with that of the simulation, indicating that the Feynman scaling law is violated more strongly than the one assumed in the simulation at ${10}^{16}$ eV. The average mass number of the primary cosmic rays, estimated from the distribution of the number of hadrons, is $〈\mathrm{ln}A〉=2.8\ifmmode\pm\else\textpm\fi{}0.5$ at ${10}^{16}$ eV.Item type: Item , Simultaneous observation of families and associated air showers at Mt. Chacaltaya(Springer Nature, 1996) N. Kawasumi; I. Tsushima; K. Honda; K. Hashimoto; T. Matano; N. Inoue; K. Mori; K. Yokoi; A. Ohsawa; M. TamadaItem type: Item , Study of hadronic component in air showers at Mt. Chacaltaya(Elsevier BV, 2001) C. Aguirre; Hiroshi Aoki; K. Hashimoto; K. Honda; N. Inoue; N. Kawasumi; Yoshikazu Maeda; N. Martinić; N. Ohmori; A. OhsawaItem type: Item , Study of primary cosmic ray composition from gamma ray families in air shower cores(Elsevier BV, 1997) K. Honda; N. Kawasumi; I. Tsushima; K. Hashimoto; T. Nishida; T. Matano; N. Inoue; A. Ohsawa; M. Tamada; N. OhmoriItem type: Item , Un evento de tipo halo detectado con cámara de emulsiones y arreglo para chubascos en el Monte Chacaltaya(2004) Hiroshi Aoki; K. Hashimoto; N. Kawasumi; K. Honda; N. Inoue; N. Martinić; C. E. Navia; Nobuaki OchiItem type: Item , VHE gamma-rays with energies above 1014 eV observed at Mt.Chacaltaya(Elsevier BV, 1990) N. Inoue; T. Matano; K. Mori; K. Hashimoto; K. Honda; N. Kawasumi; I. Tsushima; Z. Aliaga; N. Martinić; A. ReguerínItem type: Item , What can we study through families and accompanied air showers?(Elsevier BV, 1999) T. Matano; T. Nishida; N. Kawasumi; I. Tsushima; K. Hashimoto; K. Honda; N. Inoue; K. Mori; A. Ohsawa; K. Yokoi