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Sample records for air-shower array combined

  1. Combination of emulsion chamber and air shower array at Mt. Chacaltaya

    International Nuclear Information System (INIS)

    Data of 34 familes with the accompanying air showers, observed by the combination of emulsion chamber and air shower array at Mt. Chacaltaya, are presented. Comparison with the simulation calculation concludes that a change is necessary in the characteristics of hadron interactions in E0≥1015 eV

  2. L3+C air shower array

    CERN Multimedia

    Laurent Guiraud

    2000-01-01

    Photo 01: a view of the L3+C air shower array; 50 scintillators on the roof of the SX-hall above L3. Photo 02: view of one of the detectors of the array.Photo 04: detectors seen against the background of the LEP Point 2 facilities.

  3. A small air-shower array at Mount Chacaltaya

    International Nuclear Information System (INIS)

    We have operated a small air-shower array at Mount Chacaltaya in Bolivia since September 1987 and have observed air showers with primary energies above 2.0.1013 eV. This array consists of thirty-three unshielded scintillation detectors and a shielded scintillation detector. The unshielded detectors are installed over an almost flat field of approximately 8.103m2 area, while the shielded detector is located at the array center. In the present paper, we report both the details and the operation of this array and the analysis method for the observed data. Furthermore, we have simulated air showers with a Monte Carlo technique. Then, analyzing these air showers, we examine the performance of our array, that is, the accuracy in determination of the electron sizes and the arrival directions of observed air showers. (orig.)

  4. The sensitive area of cosmic ray air shower arrays

    International Nuclear Information System (INIS)

    Some closed expressions are derived for the collecting area of cosmic ray air shower arrays, taking into account the varying geometry such arrays present to showers arriving from different directions. (orig.)

  5. A mini-array for large air showers

    Science.gov (United States)

    Ng, L. K.; Chan, S. K.; Hazen, W. E.; Hazen, E. S.

    1985-01-01

    A mini-array that utilizes the Linsley effect is proposed for the measurement of large air showers. An estimate of the detectable shower rates for various shower sizes is made. Details of the detection and data collection systems are also described.

  6. A critical analysis of air shower structure functions and size spectrum measurements with the NBU air shower array

    Science.gov (United States)

    Chaudhuri, N.; Basak, D. K.

    1985-01-01

    A total of 11,000 showers in the size range 10 to the 4 to 10 to the 6 particles so far detected by the NBU air shower array has been analyzed using five different structure functions. A comparison of structure functions in terms: (1) of shower size; and (2) electron density at various core distances has been discussed to indicate the present status of structure functions in air shower analysis.

  7. A Radio Air-Shower Test Array (RASTA) for IceCube

    International Nuclear Information System (INIS)

    In this paper we explore the possibility to complement the cosmic ray physics program of the ICECUBE observatory with an extended surface array of radio antennas. The combination of air shower sampling on the surface and muon calorimetry underground offers significant scientific potential: the neutrino sensitivity above the horizon can be enhanced by vetoing air showers on the ground, photon-induced air showers can be identified by their small muon component and the coincident measurement of the particle density on the surface and the muon component gives useful information on the composition of the primary flux. All of these analyses are pursued with the existing ICETOP array. However, the ICETOP footprint is small compared to the acceptance of the INICE sensor array, which severely limits the solid angle for coincident measurements, calling for an extended surface air shower detector. As demonstrated by the LOPES experiment, measuring air showers through their geosynchrotron emission has become a viable and cost-efficient method. The science case for the RASTA project - a dedicated radio array seeking to exploit this method at the South Pole - is presented.

  8. A new study of muons in air showers by NBU air shower array

    Science.gov (United States)

    Chaudhuri, N.; Mukherjee, N.; Sarkar, S.; Basak, D. K.; Ghosh, B.

    1985-01-01

    The North Bengal University (NBU) air shower array has been in operation in conjunction with two muon magnetic spectrographs. The array incorporates 21 particle density sampling detectors around the magnetic spectrographs covering an area of 900 sq m. The layout of the array is based on the arrangement of detectors in a square symmetry. The array set up on the ground level is around a 10 m high magnetic spectrograph housing. This magnetic spectrograph housing limits the zenith angular acceptance of the incident showers to a few degrees. Three hundred muons in the fitted showers of size range 10 to the 4th power to 10 to the 5th power particles have so far been scanned and the momenta determined in the momentum range 2 - 440 GeV/c. More than 1500 recorded showers are now in the process of scanning and fitting. A lateral distribution of muons of energy greater than 300 MeV in the shower size range 10 to the 5th power to 7 x 10 to the 5th power has been obtained.

  9. Angular resolution of air-shower array-telescopes

    Science.gov (United States)

    Linsley, J.

    1985-01-01

    A fundamental limit on the angular resolution of air shower array-telescopes is set by the finite number of shower particles coupled with the finite thickness of the particle swarm. Consequently the angular resolution which can be achieved in practice depends in a determinant manner on the size and number of detectors in an array-telescope, as well as on the detector separation and the timing resolution. It is also necessary to examine the meaning of particle density in whatever type of detector is used. Results are given which can be used to predict the angular resolution of a given instrument for showers of various sizes, and to compare different instruments.

  10. Design and operation of the Chicago air shower array

    International Nuclear Information System (INIS)

    The Chicago Air Shower Array (CASA) is a large-area surface scintillator array designed to study PeV sources of cosmic rays. The complete detector will consist of 1089 detector stations, distributed on a square 15 m grid. We have operated an array of 49 stations for much of the 1989 calendar year, an array of 529 stations for much of 1990, and the balance of the 1089 stations will be operating in early 1991. This surface array, together with the University of Michigan underground muon detectors (MIA), and the University of Utah atmospheric Cerenkov telescopes and Fly's Eye air fluorescence detector, constitute a uniquely powerful instrument, dubbed the Utah Michigan Chicago (UMC) experiment, for the study of PeV sources. We report here the performance and current status of these detectors

  11. Akeno 20 km (2) air shower array (Akeno Branch)

    Science.gov (United States)

    Teshima, M.; Ohoka, H.; Matsubara, Y.; Hara, T.; Hatano, Y.; Hayashida, N.; He, C. X.; Honda, M.; Ishikawa, F.; Kamata, K.

    1985-01-01

    As the first stage of the future huge array, the Akeno air shower array was expanded to about 20 sq. km. by adding 19 scintillation detectors of 2.25 sq m area outside the present 1 sq. km. Akeno array with a new data collection system. These detectors are spaced about 1km from each other and connected by two optical fiber cables. This array has been in partial operation from 8th, Sep. 1984 and full operation from 20th, Dec. 1984. 20 sq m muon stations are planned to be set with 2km separation and one of them is now under construction. The origin of the highest energy cosmic rays is studied.

  12. Expected rates with mini-arrays for air showers

    Science.gov (United States)

    Hazen, W. E.

    1985-01-01

    As a guide in the design of mini-arrays used to exploit the Linsley effect in the study of air showers, it is useful to calculate the expected rates. The results can aid in the choice of detectors and their placement or in predicting the utility of existing detector systems. Furthermore, the potential of the method can be appraised for the study of large showers. Specifically, we treat the case of a mini-array of dimensions small enough compared to the distance of axes of showers of interest so that it can be considered a point detector. The input information is taken from the many previous studies of air showers by other groups. The calculations will give: (1) the expected integral rate, F(sigma, rho), for disk thickness, sigma, or rise time, t sub 1/2, with local particle density, rho, as a parameter; (2) the effective detection area A(N) with sigma (min) and rho (min) and rho (min) as parameters; (3) the expected rate of collection of data F sub L (N) versus shower size, N.

  13. LORA: A scintillator array for LOFAR to measure extensive air showers

    International Nuclear Information System (INIS)

    The measurement of the radio emission from extensive air showers, induced by high-energy cosmic rays, is one of the key science projects of the LOFAR radio telescope. The LOfar Radboud air shower Array (LORA) has been installed in the core of LOFAR in the Netherlands. The main purpose of LORA is to measure the properties of air showers and to trigger the read-out of the LOFAR radio antennas to register extensive air showers. The experimental set-up of the array of scintillation detectors and its performance are described

  14. Thunderstorm Observations by Air-Shower Radio Antenna Arrays

    CERN Document Server

    Apel, W D; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Buchholz, P; Buitink, S; Cantoni, E; Chiavassa, A; Daumiller, K; de Souza, V; Doll, P; Ender, M; Engel, R; Falcke, H; Finger, M; Fuhrmann, D; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Nehls, S; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmidt, A; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Wommer, M; Zabierowski, J; Zensus, J A; 10.1016/j.asr.2011.06.003

    2013-01-01

    Relativistic, charged particles present in extensive air showers lead to a coherent emission of radio pulses which are measured to identify the shower initiating high-energy cosmic rays. Especially during thunderstorms, there are additional strong electric fields in the atmosphere, which can lead to further multiplication and acceleration of the charged particles and thus have influence on the form and strength of the radio emission. For a reliable energy reconstruction of the primary cosmic ray by means of the measured radio signal it is very important to understand how electric fields affect the radio emission. In addition, lightning strikes are a prominent source of broadband radio emissions that are visible over very long distances. This, on the one hand, causes difficulties in the detection of the much lower signal of the air shower. On the other hand the recorded signals can be used to study features of the lightning development. The detection of cosmic rays via the radio emission and the influence of s...

  15. A new study of shower age distribution in near vertical showers by EAS air shower array

    Science.gov (United States)

    Chaudhuri, N.; Basak, D. K.; Goswami, G. C.; Ghosh, B.

    1984-01-01

    The air shower array has been developed since it started operation in 1931. The array covering an area of 900 sq m now incorporates 21 particle density sampling detectors around two muon magnetic spectrographs. The air showers are detected in the size range 10 to the 4th power to 10 to the 6th power particles. A total of 11000 showers has so far been detected. Average values of shower age have been obtained in various shower size ranges to study the dependence of shower age on shower size. The core distance dependence of shower age parameter has also been analyzed for presentation.

  16. Study of single and combined mass-sensitive observables of cosmic ray induced extensive air showers

    Science.gov (United States)

    Rastegarzadeh, G.; Nemati, M.

    2016-03-01

    In this study, combinations of the global arrival time, (Δτ_{global}), pseudorapidity, and lateral density distribution (ρ_{μ}) of muons, which are three mass-sensitive observables of cosmic ray induced extensive air showers, have been used as new parameters to study the primary mass discrimination around the knee energies (100 TeV-10 PeV). This is a simulation-based study and the simulations have been performed for the KASCADE array at Karlsruhe and the Alborz-I array at Tehran to study the effect of the altitude on the quality of the primary mass discrimination. The merit factors of the single and combined three mass-sensitive observables have been calculated to compare the discrimination power of combined and single observables. We have used the CORSIKA 7.4 code to simulate the extensive air showers (EASs) sample sets. Considering all aspects of our study, it is found that the ratio of the global time to the lateral density distribution of the muons gives better results than other ratios; also in the case of single observables, the muon density gives better results compared with the other observables. Also it is shown that below 1 PeV primary energies, the ratio of the muon global time to the muon density (Δτ_{global}/ρ_{μ}) results in a better mass discrimination relative to the muon density only.

  17. Hybrid experiments with air-shower array and emulsion chamber at high mountains

    International Nuclear Information System (INIS)

    Characteristics of air-shower-triggered atmospheric families detected in the hybrid experiments together with emulsion chamber and AS-array at high mountains are compared with those of simulations. The analysis of families accompanied by air-showers with Ne≥107 shows that the experimental family-energy distribution favors a proton-dominant chemical composition of primary cosmic-rays but the lateral distribution favors a heavy-dominant composition. Thus no simulations can describe the overall characteristics of the data of hybrid experiments.

  18. Hybrid experiments with air-shower array and emulsion chamber at high mountains

    Energy Technology Data Exchange (ETDEWEB)

    Besshapov, S.P.; Cherdintseva, K.V.; Chubenko, A.P.; Nesterova, N.M.; Nikolskaya, N.M.; Pavluchenko, V.P.; Shaulov, S.B. [P.N.Lebedev Physical Institute, Leninsky prospect 53, 119991 Moscow (Russian Federation); Nam, R.A.; Piskal, V.V.; Vildanov, N.G.; Vildanova, L.I. [Tien-Shan highmountain CR station, Mitina 3, 480021 Almaty (Kazakhstan); Janseitova, J.K. [Jezkazgan University, Jezkazgan, Republic Kazakhstan (Kazakhstan); Aoki, H. [Faculty of Science, Soka University, Hachijoji, Tokyo, 192-8577 (Japan); Honda, K. [Faculty of Engineering, University of Yamanashi, Kofu, 400-8511 (Japan); Inoue, N. [Faculty of Science, Saitama University, Saitama, 388-8570 (Japan); Kawasumi, N. [Faculty of Education, University of Yamanashi, Kofu, 400-8510 (Japan); Martinic, N. [Insitute de Investigaciones Fisicas, Universidad Mayor de San Andres, La Paz (Bolivia, Plurinational State of); Ochi, N. [General Education, Yonago National College of Technology, Yonago, 683-8502 (Japan); Ohmori, N. [Faculty of Science, Kochi University, Kochi, 780-8520 (Japan); Ohsawa, A. [Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, 277-8582 (Japan)

    2009-12-15

    Characteristics of air-shower-triggered atmospheric families detected in the hybrid experiments together with emulsion chamber and AS-array at high mountains are compared with those of simulations. The analysis of families accompanied by air-showers with N{sub e}>=10{sup 7} shows that the experimental family-energy distribution favors a proton-dominant chemical composition of primary cosmic-rays but the lateral distribution favors a heavy-dominant composition. Thus no simulations can describe the overall characteristics of the data of hybrid experiments.

  19. Future Extensive Air Shower arrays: From Gamma-Ray Astronomy to Cosmic Rays

    Science.gov (United States)

    Di Sciascio, Giuseppe

    2016-07-01

    Despite large progresses in building new detectors and in the analysis techniques, the key questions concerning the origin, acceleration and propagation of Galactic Cosmic Rays are still open. A number of new EAS arrays is in progress. The most ambitious and sensitive project between them is LHAASO, a new generation multi-component experiment to be installed at very high altitude in China (Daocheng, Sichuan province, 4400 m a.s.l.). The experiment will face the open problems through a combined study of photon- and charged particle-induced extensive air showers in the wide energy range 1011 - 1018 eV. In this paper the status of the experiment will be summarized, the science program presented and the outlook discussed in comparison with leading new projects.

  20. Future Extensive Air Shower arrays: from Gamma-Ray Astronomy to Cosmic Rays

    CERN Document Server

    Di Sciascio, Giuseppe

    2015-01-01

    Despite large progresses in building new detectors and in the analysis techniques, the key questions concerning the origin, acceleration and propagation of Galactic Cosmic Rays are still open. A number of new EAS arrays is in progress. The most ambitious and sensitive project between them is LHAASO, a new generation multi-component experiment to be installed at very high altitude in China (Daocheng, Sichuan province, 4400 m a.s.l.). The experiment will face the open problems through a combined study of photon- and charged particle-induced extensive air showers in the wide energy range 10$^{11}$ - 10$^{18}$ eV. In this paper the status of the experiment will be summarized, the science program presented and the outlook discussed in comparison with leading new projects.

  1. Development of Yangbajing Air shower Core detector array for a new EAS hybrid Experiment

    CERN Document Server

    Liu, Jinsheng; Chen, Ding; Zhang, Ying; Zhai, Liuming; Chen, Xu; Hu, Xiaobin; Lin, Yuhui; Zhang, Xueyao; Feng, Cunfeng; Jia, Huanyu; Zhou, Xunxiu; DanZengLuoBu,; Chen, Tianlu; Li, Haijin; Liu, Maoyuan; Yuan, Aifang

    2015-01-01

    Aiming at the observation of cosmic-ray chemical composition at the "knee" energy region, we have been developinga new type air-shower core detector (YAC, Yangbajing Air shower Core detector array) to be set up at Yangbajing (90.522$^\\circ$ E, 30.102$^\\circ$ N, 4300 m above sea level, atmospheric depth: 606 g/m$^2$) in Tibet, China. YAC works together with the Tibet air-shower array (Tibet-III) and an underground water cherenkov muon detector array (MD) as a hybrid experiment. Each YAC detector unit consists of lead plates of 3.5 cm thick and a scintillation counter which detects the burst size induced by high energy particles in the air-shower cores. The burst size can be measured from 1 MIP (Minimum Ionization Particle) to $10^{6}$ MIPs. The first phase of this experiment, named "YAC-I", consists of 16 YAC detectors each having the size 40 cm $\\times$ 50 cm and distributing in a grid with an effective area of 10 m$^{2}$. YAC-I is used to check hadronic interaction models. The second phase of the experiment,...

  2. Observation of Multi-Tev Gamma Rays from the Crab Nebula Using the Tibet Air Shower Array

    CERN Document Server

    Amenomori, M; Cao, P Y; Danzengluobu; Ding, L K; Feng, Z Y; Fu, Y; Guo, H W; He, M; Hibino, K; Hotta, N; Huang, Q; Huo, A X; Izu, K; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Labaciren; Li Jing Yi; Lü, H; Lu, S L; Luo, G X; Meng, X R; Mizutani, K; Mu, J; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Ouchi, T; Ren, J R; Saitô, T; Sakata, M; Sasaki, T; Shi, Z Z; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Taira, K; Tan, Y H; Tateyama, N; Torii, S; Utsugi, T; Wang, C R; Wang, H; Xu, X W; Yamamoto, Y; Yu, G C; Yuan, A F; Yuda, T; Zhang, C S; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhaxi Sang Zhu; Zha Xi Ciren; Zhou, W D

    1999-01-01

    The Tibet experiment, operating at Yangbajing (4,300 m above sea level), is the lowest energy air shower array and the new high density array constructed in 1996 has sensitivity to $\\gamma$-ray air showers at energies as low as 3 TeV. With this new array, the Crab Nebula was observed in multi-TeV obtained the energy spectrum of $\\gamma$-rays in the energy region above 3 TeV which partially overlaps those observed with imaging atmospheric Cherenkov telescopes. This is the first observation of $\\gamma$-ray signals from point sources with a conventional air shower array using scintillation detectors.

  3. Measurement of shower electrons and muons using a small air shower array

    Science.gov (United States)

    Chan, S. K.; Ng, L. K.

    1985-01-01

    A small air shower array has been used to measure the size spectrum of air showers at sea level in the size range 6.10 to the 3rd power to 10 to the 6th power. The result fitted with the power law gives an index 2.79 + or - 0.11 for the differential spectrum. Lateral distribution of electrons fitted with the well known NKG function results in an age parameter s = 1.35 for core distances less than 30m and s = 0.8 for longer core distances. Lateral distribution of muons follows the general shape of Greisen's relation but is much higher in intensity. Muon and electron densities at the same observation point are also compared.

  4. A halo event observed with an emulsion chamber and air shower array at Mt Chacaltaya

    International Nuclear Information System (INIS)

    A 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 (ΣEγ = 632.5 TeV and ΣE(γ)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 x 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

  5. Search for cosmic gamma rays with the Carpet-2 extensive air shower array

    CERN Document Server

    Dzhappuev, D D; Kudzhaev, A U; Klimenko, N F; Lidvansky, A S; Troitsky, S V

    2015-01-01

    The present-day status of the problem of searching for primary cosmic gamma rays at energies above 100 TeV is discussed, as well as a proposal for a new experiment in this field. It is shown that an increase of the area of the muon detector of the Carpet-2 air shower array up to 410 square meters, to be realized in 2016, will make this array quite competitive with past and existing experiments, especially at modest energies. Some preliminary results of measurements made with smaller area of the muon detector are presented together with estimates of expected results to be obtained with the coming large-area muon detector.

  6. Air Shower Radio Emission with Energy E$_0$$\\geq$10$^{19}$ eV by Yakutsk Array Data

    CERN Document Server

    Knurenko, S P

    2016-01-01

    The paper presents short technical description of Yakutsk Radio Array and some preliminary results obtained from measurements of radio emission at 32 MHz frequency induced by air shower particles with energy {\\epsilon}$\\geq$1$\\cdot$10$^{19}$ eV. The data obtained at Yakutsk array in 1987-1989 (first set of measurements) and 2009-2014 (new set of measurements). For the first time, at Yakutsk array radio emission from air shower with energy > 10$^{19}$ eV was registered including the shower with highest energy ever registered at Yakutsk array with energy $\\sim$2$\\cdot$10$^{20}$ eV.

  7. Towards improving the reconstruction quality for air showers detected with the AERA array

    International Nuclear Information System (INIS)

    We present a study on simulated air showers with relevance for the AERA experiment at the Pierre Auger Observatory. Investigating the radio component of air showers requires good knowledge of the geometrical properties of the shower, like for example the position of the shower core and the arrival direction of the shower. At the Pierre Auger Observatory the geometrical observables of the detected events are reconstructed with the help of the FD and SD components (the Infill array playing the major role in the shower core reconstruction for AERA). We investigate the possibility to increase the quality of the shower core reconstruction by increasing the density of surface detectors in an area close the the position of the radio antennas. From the technical point of view, extending the surface array by adding new SD stations to the Infill is not a straight forward job so simulation studies can be used to test various configurations for the additional stations. We present the effects induced on the reconstruction quality, for several geometrical configurations.

  8. On the extension of the sensitive area of an extensive air shower surface array

    CERN Document Server

    Kh, H Hedayati

    2016-01-01

    A large distance between true and reconstructed core locations of an extensive air shower (EAS) may results in great systematic mis-estimation of EAS parameters. The reconstruction of those EASs whose core locations are outside the boundary of a surface array (outside EAS (OEAS)) results in a large distance of the reconstructed core location from the true one, especially when the true core is far outside the array. Although it may not be mentioned, the identification of OEASs is a necessary and important step in the reconstruction procedure of an EAS. In this paper, an existing technique is optimized for the identification of OEASs. The simultaneous use of this technique and a recently developed approach for reconstructing the core location of an EAS can significantly increase the sensitive area of a surface array.

  9. Temporal signatures of the Cherenkov light induced by extensive air showers of cosmic rays detected with the Yakutsk array

    CERN Document Server

    Ivanov, A A

    2016-01-01

    We analyze temporal characteristics of signals from the wide field-of-view (WFOV) Cherenkov telescope (CT) detecting extensive air showers (EAS) of cosmic rays (CR) in coincidence with surface detectors of the Yakutsk array. Our aim is to reveal causal relationships between measured characteristics and physical properties of EAS.

  10. Measurement of the cosmic-ray energy spectrum above 1016 eV with the LOFAR Radboud Air Shower Array

    Science.gov (United States)

    Thoudam, S.; Buitink, S.; Corstanje, A.; Enriquez, J. E.; Falcke, H.; Hörandel, J. R.; Nelles, A.; Rachen, J. P.; Rossetto, L.; Schellart, P.; Scholten, O.; ter Veen, S.; Trinh, T. N. G.; van Kessel, L.

    2016-01-01

    The energy reconstruction of extensive air showers measured with the LOFAR Radboud Air Shower Array (LORA) is presented in detail. LORA is a particle detector array located in the center of the LOFAR radio telescope in the Netherlands. The aim of this work is to provide an accurate and independent energy measurement for the air showers measured through their radio signal with the LOFAR antennas. The energy reconstruction is performed using a parameterized relation between the measured shower size and the cosmic-ray energy obtained from air shower simulations. In order to illustrate the capabilities of LORA, the all-particle cosmic-ray energy spectrum has been reconstructed, assuming that cosmic rays are composed only of protons or iron nuclei in the energy range between ˜2 × 1016 and 2 × 1018 eV. The results are compatible with literature values and a changing mass composition in the transition region from a Galactic to an extragalactic origin of cosmic rays.

  11. An optimized method for the reconstruction of the direction of air showers for scintillator arrays

    International Nuclear Information System (INIS)

    An optimized method is presented for the reconstruction of air shower directions for scintillator arrays. The method takes into account that both the expectation value and the spread of the measured arrival times not only depend on the distance of a counter from the shower axis, but also on the number of particles registered in that counter. It also takes into account that the distributions of the measured arrival times are not Gaussian. For showers recorded with the HEGRA scintillator array above the threshold energy of Ethres= 20 TeV the mean angular resolution obtained with this method is left angle σθ63% right angle =1.0 circle, and above a threshold Ethres= 50 TeV it is left angle σθ63% right angle =0.6 circle. Comparing the new procedure with the HEGRA standard procedure the angular resolution has improved on average by a factor of 1.33. The mis-pointing has been determined with an accuracy of 0.15 circle. The method is developed using experimental data. (orig.)

  12. OBSERVATION OF COSMIC-RAY ANISOTROPY WITH THE ICETOP AIR SHOWER ARRAY

    International Nuclear Information System (INIS)

    We report on the observation of anisotropy in the arrival direction distribution of cosmic rays at PeV energies. The analysis is based on data taken between 2009 and 2012 with the IceTop air shower array at the south pole. IceTop, an integral part of the IceCube detector, is sensitive to cosmic rays between 100 TeV and 1 EeV. With the current size of the IceTop data set, searches for anisotropy at the 10–3 level can, for the first time, be extended to PeV energies. We divide the data set into two parts with median energies of 400 TeV and 2 PeV, respectively. In the low energy band, we observe a strong deficit with an angular size of about 30° and an amplitude of (– 1.58 ± 0.46stat ± 0.52sys) × 10–3 at a location consistent with previous observations of cosmic rays with the IceCube neutrino detector. The study of the high energy band shows that the anisotropy persists to PeV energies and increases in amplitude to (– 3.11 ± 0.38stat ± 0.96sys) × 10–3.

  13. A method of observing cherenkov light from extensive air shower at Yakutsk EAS array

    Science.gov (United States)

    Timofeev, Lev; Anatoly, Ivanov

    2016-07-01

    Proposed a new method for measuring the cherenkov light from the extensive air shower (EAS) of cosmic rays (CR), which allows to determine not only the primary particle energy and angle of arrival, but also the parameters of the shower in the atmosphere - the maximum depth and "age". For measurements Cherenkov light produced by EAS is proposed to use a ground network of wide-angle telescopes which are separated from each other by a distance 100-300 m depending on the total number of telescopes operating in the coincidence signals, acting autonomously, or includes a detector of the charged components, radio waves, etc. as part of EAS. In a results such array could developed, energy measurement and CR angle of arrival data on the depth of the maximum and the associated mass of the primary particle generating by EAS. This is particularly important in the study of galactic cosmic ray in E> 10^14 eV, where currently there are no direct measurements of the maximum depth of the EAS.

  14. Observation of Cosmic Ray Anisotropy with the IceTop Air Shower Array

    CERN Document Server

    Aartsen, M G; Abdou, Y; Ackermann, M; Adams, J; Aguilar, J A; Ahlers, M; Altmann, D; Andeen, K; Auffenberg, J; Bai, X; Baker, M; Barwick, S W; Baum, V; Bay, R; Beattie, K; Beatty, J J; Bechet, S; Tjus, J Becker; Becker, K -H; Bell, M; Benabderrahmane, M L; BenZvi, S; Berdermann, J; Berghaus, P; Berley, D; Bernardini, E; Bertrand, D; Besson, D Z; Bindig, D; Bissok, M; Blaufuss, E; Blumenthal, J; Boersma, D J; Bohaichuk, S; Bohm, C; Bose, D; Böser, S; Botner, O; Brayeur, L; Brown, A M; Bruijn, R; Brunner, J; Carson, M; Casey, J; Casier, M; Chirkin, D; Christy, B; Clark, K; Clevermann, F; Cohen, S; Cowen, D F; Silva, A H Cru; Danninger, M; Daughhetee, J; Davis, J C; Clercq, C D; Ridder, S D; Descamps, F; Desiati, P; Vries-Uiterweerd, G d; DeYoung, T; Díaz-Vélez, J C; Dreyer, J; Dumm, J P; Dunkman, M; Eagan, R; Eisch, J; Ellsworth, R W; Engdegård, O; Euler, S; Evenson, P A; Fadiran, O; Fazely, A R; Fedynitch, A; Feintzeig, J; Feusels, T; Filimonov, K; Finley, C; Fischer-Wasels, T; Flis, S; Franckowiak, A; Franke, R; Frantzen, K; Fuchs, T; Gaisser, T K; Gallagher, J; Gerhardt, L; Gladstone, L; Glüsenkamp, T; Goldschmidt, A; Golup, G; Goodman, J A; Góra, D; Grant, D; Groß, A; Grullon, S; Gurtner, M; Ha, C; Ismail, A Ha; Hallgren, A; Halzen, F; Hanson, K; Heereman, D; Heimann, P; Heinen, D; Helbing, K; Hellauer, R; Hickford, S; Hill, G C; Hoffman, K D; Hoffmann, R; Homeier, A; Hoshina, K; Huelsnitz, W; Hulth, P O; Hultqvist, K; Hussain, S; Ishihara, A; Jacobi, E; Jacobsen, J; Japaridze, G S; Jlelati, O; Kappes, A; Karg, T; Karle, A; Kiryluk, J; Kislat, F; Kläs, J; Klein, S R; Köhne, J -H; Kohnen, G; Kolanoski, H; Köpke, L; Kopper, C; Kopper, S; Koskinen, D J; Kowalski, M; Krasberg, M; Kroll, G; Kunnen, J; Kurahashi, N; Kuwabara, T; Labare, M; Landsman, H; Larson, M J; Lauer, R; Lesiak-Bzdak, M; Lünemann, J; Madsen, J; Maruyama, R; Mase, K; Matis, H S; McNally, F; Meagher, K; Merck, M; Mészáros, P; Meures, T; Miarecki, S; Middell, E; Milke, N; Miller, J; Mohrmann, L; Montaruli, T; Morse, R; Nahnhauer, R; Naumann, U; Nowicki, S C; Nygren, D R; Obertacke, A; Odrowski, S; Olivas, A; Olivo, M; O'Murchadha, A; Panknin, S; Paul, L; Pepper, J A; Heros, C Pérez de los; Pieloth, D; Pirk, N; Posselt, J; Price, P B; Przybylski, G T; Rädel, L; Rawlins, K; Redl, P; Resconi, E; Rhode, W; Ribordy, M; Richman, M; Riedel, B; Rodrigues, J P; Rothmaier, F; Rott, C; Ruhe, T; Ruzybayev, B; Ryckbosch, D; Saba, S M; Salameh, T; Sander, H -G; Santander, M; Sarkar, S; Schatto, K; Scheel, M; Scheriau, F; Schmidt, T; Schmitz, M; Schoenen, S; Schöneberg, S; Schönherr, L; Schönwald, A; Schukraft, A; Schulte, L; Schulz, O; Seckel, D; Seo, S H; Sestayo, Y; Seunarine, S; Sheremata, C; Smith, M W E; Soiron, M; Soldin, D; Spiczak, G M; Spiering, C; Stamatikos, M; Stanev, T; Stasik, A; Stezelberger, T; Stokstad, R G; Stößl, A; Strahler, E A; Ström, R; Sullivan, G W; Taavola, H; Taboada, I; Tamburro, A; Ter-Antonyan, S; Tilav, S; Toale, P A; Toscano, S; Usner, M; Drift, D va de; Eijndhoven, N va; Overloop, A Va; Santen, J va; Vehring, M; Voge, M; Vraeghe, M; Walck, C; Waldenmaier, T; Wallraff, M; Walter, M; Wasserman, R; Weaver, Ch; Wendt, C; Westerhoff, S; Whitehorn, N; Wiebe, K; Wiebusch, C H; Williams, D R; Wissing, H; Wolf, M; Wood, T R; Woschnagg, K; Xu, C; Xu, D L; Xu, X W; Yanez, J P; Yodh, G; Yoshida, S; Zarzhitsky, P; Ziemann, J; Zierke, S; Zilles, A; Zoll, M

    2012-01-01

    We report on the observation of anisotropy in the arrival direction distribution of cosmic rays at PeV energies. The analysis is based on data taken between 2009 and 2012 with the IceTop air shower array at the South Pole. IceTop, an integral part of the IceCube detector, is sensitive to cosmic rays between 100 TeV and 1 EeV. With the current size of the IceTop data set, searches for anisotropy at the 10^-3 level can, for the first time, be extended to PeV energies. We divide the data set into two parts with median energies of 400 TeV and 2 PeV, respectively. In the low energy band, we observe a strong deficit with an angular size of about 30 degrees and an amplitude of (-1.58 +/- 0.46 (stat) +/- 0.52 (sys)) x 10^(-3) at a location consistent with previous observations of cosmic rays with the IceCube neutrino detector. The study of the high energy band shows that the anisotropy persists to PeV energies and increases in amplitude to (-3.11 +/- 0.38 (stat) +/- 0.96 (sys)) x 10^(-3).

  15. Anisotropy of successive air showers

    Science.gov (United States)

    Ochi, N.; Wada, T.; Yamashita, Y.; Ohashi, A.; Yamamoto, I.; Nakatsuka, T.; Large Area Air Shower (LAAS) Group

    2001-04-01

    We have investigated the anisotropy of successive air shower (SAS) events, which we define as the detection of many air showers within a short time window, using data from six stations of the Large Area Air Shower (LAAS) group. On the criterion of 22 air showers within 20 minutes, five SAS events are found against 1.4 expected from the Poisson distribution in Okayama University station's data. From six stations' data, we find 24 SAS events in total. By plotting them in equatorial coordinates, it is revealed that SAS events are observed more frequently when the Galactic plane is around the zenith. This can be attributed to a hypothetical small flux of ultra-high-energy γ-rays from the direction of the Galactic plane superposed on conventional cosmic rays. If this hypothesis is true, the analytical procedure used here has potential to measure ultra-high-energy γ-ray sources by even small air shower arrays like ours.

  16. Anisotropy of successive air showers

    International Nuclear Information System (INIS)

    We have investigated the anisotropy of successive air shower (SAS) events, which we define as the detection of many air showers within a short time window, using data from six stations of the Large Area Air Shower (LAAS) group. On the criterion of 22 air showers within 20 minutes, five SAS events are found against 1.4 expected from the Poisson distribution in Okayama University station's data. From six stations' data, we find 24 SAS events in total. By plotting them in equatorial coordinates, it is revealed that SAS events are observed more frequently when the Galactic plane is around the zenith. This can be attributed to a hypothetical small flux of ultra-high-energy γ-rays from the direction of the Galactic plane superposed on conventional cosmic rays. If this hypothesis is true, the analytical procedure used here has potential to measure ultra-high-energy γ-ray sources by even small air shower arrays like ours

  17. The effect of the atmospheric condition on the extensive air shower analysis at the Telescope Array experiment

    International Nuclear Information System (INIS)

    The accuracies in determination of air shower parameters such as longitudinal profiles or primary energies with the fluorescence detection technique are strongly dependent on atmospheric conditions of the molecular and aerosol components. Moreover, air fluorescence photon yield depends on the atmospheric density, and the transparency of the air for fluorescence photons depends on the atmospheric conditions from EAS to FDs. In this paper, we describe the atmospheric monitoring system in the Telescope Array (TA experiment), and the impact of the atmospheric conditions in air shower reconstructions. The systematic uncertainties of the determination of the primary cosmic ray energies and of the measurement of depth of maximum development (Xmax) of EASs due to atmospheric variance are evaluated by Monte Carlo simulation.

  18. The Telescope Array RADAR (TARA) Project and the Search for the Radar Signature of Cosmic Ray Induced Extensive Air Showers

    Science.gov (United States)

    Prohira, Steven; TARA Collaboration; Telescope Array Collaboration

    2016-03-01

    The TARA (Telescope Array Radar) cosmic ray detector has been in operation since May 2013. It is the most ambitious effort to date to test an idea that originated in the 1940's: that ionization produced by cosmic ray extensive air showers should reflect electromagnetic radiation. The observation of this effect would open the possibility that remote-sensing radar technology could be used to detect and reconstruct extensive air showers, thus increasing the aperture available for the study of the highest-energy cosmic rays. TARA employs a bi-static radar configuration, consisting of a 25 kW, 5 MW ERP transmitter at 54.1 MHz broadcasting across the Telescope Array surface detector. 40 km distant, a set of log-periodic receiver antennas are read out by two independent data acquisition systems employing different techniques to select signals of the form expected for radar targets moving at close to the speed of light. In this talk, we describe the TARA detector and present the first quantitative limits on the radar cross-section of extensive air showers.

  19. A search for sources of ultra high energy gamma rays at air shower energies with Ooty EAS array

    Science.gov (United States)

    Tonwar, S. C.; Gopalakrishnan, N. V.; Sreekantan, B. V.

    1985-01-01

    A 24 detector extensive air shower array is being operated at Ootacamund (2200 m altitude, 11.4 deg N latitude) in southern India to search for sources of Cosmic gamma rays of energies greater then 5 x 10 to the 13th power eV. The angular resolution of the array has been experimentally estimated to be better than about 2 deg. Since June '84, nearly 2.5 million showers have been collected and their arrival directions determined. These showers are being studied to search for very high energy gamma ray emission from interesting astrophysical objects such as Cygnus X-3, Crab pulsar and Geminga.

  20. LOPES-3D, an antenna array for full signal detection of air-shower radio emission

    CERN Document Server

    Apel, W D; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Buchholz, P; Cantoni, E; Chiavassa, A; Daumiller, K; de Souza, V; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Finger, M; Fuchs, B; Fuhrmann, D; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmidt, A; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Wommer, M; Zabierowski, J; Zensus, J A; 10.1016/j.nima.2012.08.082

    2013-01-01

    To better understand the radio signal emitted by extensive air-showers and to further develop the radio detection technique of high-energy cosmic rays, the LOPES experiment was reconfigured to LOPES-3D. LOPES-3D is able to measure all three vectorial components of the electric field of radio emission from cosmic ray air showers. The additional measurement of the vertical component ought to increase the reconstruction accuracy of primary cosmic ray parameters like direction and energy, provides an improved sensitivity to inclined showers, and will help to validate simulation of the emission mechanisms in the atmosphere. LOPES-3D will evaluate the feasibility of vectorial measurements for large scale applications. In order to measure all three electric field components directly, a tailor-made antenna type (tripoles) was deployed. The change of the antenna type necessitated new pre-amplifiers and an overall recalibration. The reconfiguration and the recalibration procedure are presented and the operationality of...

  1. On Temporal Variations of the Multi-TeV Cosmic Ray Anisotropy using the Tibet III Air Shower Array

    CERN Document Server

    Amenomori, M; Chen, D; Cui, S W; Danzengluobu,; Ding, L K; Ding, X H; Fan, C; Feng, C F; Feng, Zhaoyang; Feng, Z Y; Gao, X Y; Geng, Q X; Gou, Q B; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Hu, Haibing; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Jiang, L; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren,; Le, G M; Li, A F; Li, H C; Li, J Y; Liu, C; Lou, Y -Q; Lu, H; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Ozawa, S; Saito, T; Saito, T Y; Sakata, M; Sako, T K; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Wang, B; Wang, H; Wang, Y; Wang, Y G; Wu, H R; Xue, L; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhang, Y; Zhang, Yi; Zhang, Ying; Zhaxisangzhu,; Zhou, X X

    2010-01-01

    We analyze the large-scale two-dimensional sidereal anisotropy of multi-TeV cosmic rays by Tibet Air Shower Array, with the data taken from 1999 November to 2008 December. To explore temporal variations of the anisotropy, the data set is divided into nine intervals, each in a time span of about one year. The sidereal anisotropy of magnitude about 0.1% appears fairly stable from year to year over the entire observation period of nine years. This indicates that the anisotropy of TeV Galactic cosmic rays remains insensitive to solar activities since the observation period covers more than a half of the 23rd solar cycle.

  2. Future plan for observation of cosmic gamma rays in the 100 TeV energy region with the Tibet air shower array : simulation and sensitivity

    CERN Document Server

    Amenomori, M; Chen, D; Cui, S W; Danzengluobu,; Ding, L K; Ding, X H; Fan, C; Feng, C F; Feng, Zhaoyang; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Hu, Haibing; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren,; Le, G M; Li, A F; Li, J Y; Lou, Y -Q; Lü, H; Lu, S L; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saitô, T; Saito, T Y; Sakata, M; Sako, T K; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Wang, B; Wang, H; Wang, X; Wang, Y; Wang, Y G; Wu, H R; Xue, L; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhang, Y; Zhang, Yi; Zhaxisangzhu,; Zhou, X X

    2007-01-01

    The Tibet air shower array, which has an effective area of 37,000 square meters and is located at 4300 m in altitude, has been observing air showers induced by cosmic rays with energies above a few TeV. We have a plan to add a large muon detector array to it for the purpose of increasing its sensitivity to cosmic gamma rays in the 100 TeV energy region by discriminating them from cosmic-ray hadrons. We have deduced the attainable sensitivity of the muon detector array using our Monte Carlo simulation. We report here on the detailed procedure of our Monte Carlo simulation.

  3. Future plan for observation of cosmic gamma rays in the 100 TeV energy region with the Tibet air shower array : physics goal and overview

    CERN Document Server

    Amenomori, M; Chen, D; Cui, S W; Danzengluobu,; Ding, L K; Ding, X H; Fan, C; Feng, C F; Feng, Zhaoyang; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Hu, Haibing; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren,; Le, G M; Li, A F; Li, J Y; Lou, Y -Q; Lü, H; Lu, S L; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saitô, T; Saito, T Y; Sakata, M; Sako, T K; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Wang, B; Wang, H; Wang, X; Wang, Y; Wang, Y G; Wu, H R; Xue, L; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhang, Y; Zhang, Yi; Zhaxisangzhu,; Zhou, X X

    2007-01-01

    The Tibet air shower array, which has an effective area of 37,000 square meters and is located at 4300 m in altitude, has been observing air showers induced by cosmic rays with energies above a few TeV. We are planning to add a large muon detector array to it for the purpose of increasing its sensitivity to cosmic gamma rays in the 100 TeV (10 - 1000 TeV) energy region by discriminating them from cosmic-ray hadrons. We report on the possibility of detection of gamma rays in the 100 TeV energy region in our field of view, based on the improved sensitivity of our air shower array deduced from the full Monte Carlo simulation.

  4. LOPES-3D: An antenna array for full signal detection of air-shower radio emission

    International Nuclear Information System (INIS)

    To better understand the radio signal emitted by extensive air-showers and to further develop the radio detection technique of high-energy cosmic rays, the LOPES experiment was reconfigured to LOPES-3D. LOPES-3D is able to measure all three vectorial components of the electric field of radio emission from cosmic ray air showers. The additional measurement of the vertical component ought to increase the reconstruction accuracy of primary cosmic ray parameters like direction and energy, provides an improved sensitivity to inclined showers, and will help to validate simulation of the emission mechanisms in the atmosphere. LOPES-3D will evaluate the feasibility of vectorial measurements for large scale applications. In order to measure all three electric field components directly, a tailor-made antenna type (tripoles) was deployed. The change of the antenna type necessitated new pre-amplifiers and an overall recalibration. The reconfiguration and the recalibration procedure are presented and the operationality of LOPES-3D is demonstrated.

  5. Cherenkov counter of extensive air showers for combined operation with the neutrino telescope NT-200

    International Nuclear Information System (INIS)

    The Baikal NT-200 neutrino telescope consists of 192 optical modules based on the Quasar-370 hybrid photodetectors. To study the angular resolution of NT-200 neutrino telescope one has developed the Cherenkov counter of extensive air showers with 1 deg angular resolution. Paper describes the electron structure of the facility made in terms of the CAMAC standard. One evaluates the measurement error for time intervals depending on the amplitude of output signals of photodetector. The counting rate of coinciding events of the Cherenkov counter for extensive air showers and of NT-200 deep-sea neutrino telescope constitutes about 0.5 min-1.Measuring of time interval between the trigger signals of the neutrino telescope and of the Cherenkov counter enables to suppress efficiently random coincidences and to obtain additional information on the muon trajectory

  6. Observation of PeV Gamma Rays from the Monogem Ring with the Tibet Air Shower Array

    CERN Document Server

    Amenomori, M; Chen, D; Cui, S W; Danzengluobu; Ding, L K; Ding, X H; Feng Cun Feng; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Hu, H; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren; Le, G M; Li, J Y; Lü, H; Lu, S L; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saitô, T; Saito, T Y; Sakata, M; Sasaki, T; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Wang, H; Wang, X; Wang, Y G; Wu, H R; Xue Liang; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhang, Y; Zhang, Yi; Zhaxi Sang Zhu; Zhou, X X

    2005-01-01

    We searched for steady PeV gamma-ray emission from the Monogem ring region with the Tibet air shower array from 1997 February to 2004 October. No evidence for statistically significant gamma-ray signals was found in a region 111$\\degr$ $\\leq$ R.A. $<$ 114$\\degr$, 12$\\fdg$5 $\\leq$ decl. $<$ 15$\\fdg$5 in the Monogem ring where the MAKET-ANI experiment recently claimed a positive detection of PeV high-energy cosmic radiation, although our flux sensitivity is approximately 10 times better than MAKET-ANI's. We set the most stringent integral flux upper limit at a 99% confidence level of 4.0 $\\times$ 10$^{-12}$ cm$^{-2}$ s$^{-1}$ sr$^{-1}$ above 1 PeV on diffuse gamma rays extended in the 3$^{\\circ}$ $\\times$ 3$^{\\circ}$ region.

  7. Search for the Multi-TeV Gamma Rays from the Shell-Like SNR G40.5-0.5 Using the Tibet Air Shower Array

    Institute of Scientific and Technical Information of China (English)

    ZHANG Ji-Long; TAN You-Hen; LU Hong; WANG Hui

    2005-01-01

    @@ Using observation data of the Tibet air shower array in different periods, a region with the highest excess of 4.4 σ in the multi-TeV was detected from the SNR G40.5-0.5 direction, although statistically insignificant yet. The position of the highest excess is located around the EGRET unidentified source 3EG J1903+0550.

  8. Underground Water Cherenkov Muon Detector Array with the Tibet Air Shower Array for Gamma-Ray Astronomy in the 100 TeV Region

    CERN Document Server

    Amenomori, M; Bi, X J; Chen, D; Cui, S W; Feng Zhao Yang; Danzengluobu; Ding, L K; Feng Cun Feng; Feng, Z; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Haibing, H; Hu, H B; Huang, J; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren; Le, G M; Li, A F; Li, J Y; Lü, H; Lu, S L; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanj, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saitô, T; Saito, T Y; Sakata, M; Sako, T K; Sasaki, T; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Tori, S; Wang, B; Tsuchiya, H; Udo, S; Wang, X; Wang, Y G; Wu, H R; Xue Liang; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhamg, N J; Zhamg, X, Y; Zhamg, Y; Zhamg, Yi; Zha Xisang Zhu; Zhou, X X; al, et

    2006-01-01

    We propose to build a large water-Cherenkov-type muon-detector array (Tibet MD array) around the 37,000 m$^{2}$ Tibet air shower array (Tibet AS array) already constructed at 4,300 m above sea level in Tibet, China. Each muon detector is a waterproof concrete pool, 6 m wide $\\times$ 6 m long $\\times$ 1.5 m deep in size, equipped with a 20 inch-in-diameter PMT. The Tibet MD array consists of 240 muon detectors set up 2.5 m underground. Its total effective area will be 8,640 m$^{2}$ for muon detection. The Tibet MD array will significantly improve gamma-ray sensitivity of the Tibet AS array in the 100 TeV region (10-1000 TeV) by means of gamma/hadron separation based on counting the number of muons accompanying an air shower. The Tibet AS+MD array will have the sensitivity to gamma rays in the 100 TeV region by an order of magnitude better than any other previous existing detectors in the world.

  9. Electronics and data acquisition system of the extensive air shower detector array at the University of Puebla

    Science.gov (United States)

    Perez, E.; Salazar, H.; Villasenor, L.; Martinez, O.; Conde, R.; Murrieta, T.

    Field programmable gate arrays (FPGAs) are playing an increasing role in DAQ systems in cosmic ray experiments due to their high speed and integration and their low cost and low power comsumption. In this paper we describe in detail the new electronics and data acquisition system based on FPGA boards of the extensive air shower detector array built in the Campus of the University of Puebla. The purpose of this detector array is to measure the energy and arrival direction of primary cosmic rays with energies around 1015 eV. The array consists of 10 liquid scintillator detectors and 6 water Cherenkov detectors (of 1.86 m2 cross section), distributed in a square grid with a detector spacing of 20 m over an area of 4000 m2. The electronics described also makes use of analog to digital converters with a resolution of 10 bits and sampling speeds of 100 MS/s to digitize the PMT signals. We also discuss the advantages of discriminating the PMT signals inside the FPGAs with respect to the conventional use of dedicated discrimination circuits.

  10. World's largest air shower array now on track of super-high-energy cosmic-rays Pierre Auger Observatory seeks source of highest-energy extraterrestrial particles

    CERN Multimedia

    2003-01-01

    "With the completion of its hundredth surface detector, the Pierre Auger Observatory, under construction in Argentina, this week became the largest cosmic-ray air shower array in the world. Managed by scientists at the Department of Energy's Fermi National Accelerator Laboratory, the Pierre Auger project so far encompasses a 70-square-mile array of detectors that are tracking the most violent-and perhaps most puzzling- processes in the entire universe" (1 page).

  11. Observation of TeV Gamma Rays from the Fermi Bright Galactic Sources with the Tibet Air Shower Array

    CERN Document Server

    Amenomori, M; Chen, D; Cui, S W; Danzengluobu,; Ding, L K; Ding, X H; Fan, C; Feng, C F; Feng, Zhaoyang; Feng, Z Y; Gao, X Y; Geng, Q X; Gou, Q B; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Hu, Haibing; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Jiang, L; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren,; Le, G M; Li, A F; Li, H C; Li, J Y; Liu, C; Lou, Y -Q; Lu, H; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Ozawa, S; Saito, T; Saito, T Y; Sakata, M; Sako, T K; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Wang, B; Wang, H; Wang, Y; Wang, Y G; Wu, H R; Xue, L; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhang, Y; Zhang, Yi; Zhang, Ying; Zhaxisangzhu,; Zhou, X X

    2009-01-01

    Using the Tibet-III air shower array, we search for TeV gamma-rays from 27 potential Galactic sources in the early list of bright sources obtained by the Fermi Large Area Telescope at energies above 100 MeV. Among them, we observe 7 sources instead of the expected 0.61 sources at a significance of 2 sigma or more excess. The chance probability from Poisson statistics would be estimated to be 3.8 x 10^-6. If the excess distribution observed by the Tibet-III array has a density gradient toward the Galactic plane, the expected number of sources may be enhanced in chance association. Then, the chance probability rises slightly, to 1.2 x 10^-5, based on a simple Monte Carlo simulation. These low chance probabilities clearly show that the Fermi bright Galactic sources have statistically significant correlations with TeV gamma-ray excesses. We also find that all 7 sources are associated with pulsars, and 6 of them are coincident with sources detected by the Milagro experiment at a significance of 3 sigma or more at ...

  12. Search for TeV gamma rays emission from the shell-like SNR G40.5-0.5 using the Yangbajing extensive air shower array

    International Nuclear Information System (INIS)

    Using observation data of the Yangbajing extensive air shower array from October 2000 to September 2001, the TeV gamma rays from the shell-like SNR G40.5-0.5 direction were detected. A region with the highest excess of 4.4σ was found using two dimensional analysis method. The position of EGRET unidentified source GeV J1907+0557 is near the centrer of the region. (authors)

  13. Detection of thermal neutrons with the PRISMA-YBJ array in Extensive Air Showers selected by the ARGO-YBJ experiment

    CERN Document Server

    Bartoli, B; Bi, X J; Cao, Z; Catalanotti, S; Chen, S Z; Chen, T L; Cui, S W; Dai, B Z; D'Amone, A; Danzengluobu,; De Mitri, I; Piazzoli, B D'Ettorre; Di Girolamo, T; Di Sciascio, G; Feng, C F; Feng, Zhaoyang; Feng, Zhenyong; Gou, Q B; Guo, Y Q; He, H H; Hu, Haibing; Hu, Hongbo; Iacovacci, M; Iuppa, R; Jia, H Y; Labaciren,; Li, H J; Liu, C; Liu, J; Liu, M Y; Lu, H; Ma, L L; Ma, X H; Mancarella, G; Mari, S M; Marsella, G; Mastroianni, S; Montini, P; Ning, C C; Perrone, L; Pistilli, P; Salvini, P; Santonico, R; Shen, P R; Sheng, X D; Shi, F; Surdo, A; Tan, Y H; Vallania, P; Vernetto, S; Vigorito, C; Wang, H; Wu, C Y; Wu, H R; Xue, L; Yang, Q Y; Yang, X C; Yao, Z G; Yuan, A F; Zha, M; Zhang, H M; Zhang, L; Zhang, X Y; Zhang, Y; Zhao, J; Zhaxiciren,; Zhaxisangzhu,; Zhou, X X; Zhu, F R; Zhu, Q Q; Stenkin, Yu V; Alekseenko, V V; Aynutdinov, V; Cai, Z Y; Guo, X W; Liu, Y; Rulev, V; Shchegolev, O B; Stepanov, V; Volchenko, V; Zhang, H

    2015-01-01

    We report on a measurement of thermal neutrons, generated by the hadronic component of extensive air showers (EAS), by means of a small array of EN-detectors developed for the PRISMA project (PRImary Spectrum Measurement Array), novel devices based on a compound alloy of ZnS(Ag) and 6LiF. This array has been operated within the ARGO-YBJ experiment at the high altitude Cosmic Ray Observatory in Yangbajing (Tibet, 4300 m a.s.l.). Due to the tight correlation between the air shower hadrons and thermal neutrons, this technique can be envisaged as a simple way to get information on the EAS hadronic component, avoiding the use of huge calorimeters. Coincident events generated by primary cosmic rays of energies greater than 100 TeV have been selected and analyzed. The EN-detectors have been used to record simultaneously thermal neutrons and the air shower electromagnetic component. The density distribution of both components and the total number of thermal neutrons have been measured. The correlation of these data w...

  14. LAAS network observation of air showers

    International Nuclear Information System (INIS)

    A network observation of air showers is in progress in Japan. Researchers from 10 institutions are taking part in the network, forming the Large Area Air Shower (LAAS) group. As of June 2000, eight air shower arrays (stations) are in operation, while five more stations are under construction. The stations are scattered over an enormous area of 130,000 km2, however the Global Positioning System (GPS) provides comparable time stamps among them with an accuracy of one microsecond. The aim of the network is to find out correlations in primary cosmic rays just below the knee. The data from the planned Norikura array (2,770 m a.s.l.) is expected to reveal new aspects of correlated cosmic rays. The current status of the network and performance of arrays calculated by the air shower simulation code CORSIKA are described here

  15. Revised Upper Limits of the Diffuse Tev Gamma Rays from the Galactic Planes with the Tibet II and III Air Shower Arrays

    CERN Document Server

    Amenomori, M; Bi, X J; Chen, D; Cui, S W; Danzengluobu; Ding, L K; Ding, X H; Feng Cun Feng; Zhaoyang Feng; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Haibing, H; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren; Le, G M; Li, A F; Li, J Y; Lou, Y Q; Lü, H; Lu, S L; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saitô, T; Saito, T Y; Sakata, M; Sako, T K; Sasaki, T; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Wang, B; Wang, H; Wang, X; Wang, Y G; Wu, H R; Xue Liang; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhang, Y; Yi Zhang Zhaxisangzhu; Zhou, X X; al, et

    2006-01-01

    The flux upper limits of the diffuse gamma rays, from the inner and outer Galactic planes, are revised by factors of 4.0$\\sim$3.7 for mode energies 3$\\sim$10 TeV, respectively, by using the simulation results of the effective area ratios for gamma-ray induced showers and cosmic-ray induced ones in the Tibet air shower array. In our previous work, (Amenomori et al., ApJ, 580, 887, 2002) the flux upper limits were deduced only from the flux ratio of air showers generated by gamma rays versus cosmic rays. The details of the simulation are given in the paper (Amenomori et al., Advances in Space Research, 37, 1932, 2006). The present result using the same data as in ApJ suggests that the spectral index of source electrons is steeper than 2.2 and 2.1 for the inner and outer Galactic planes, respectively.

  16. Experimental study of high energy muons from Extensive Air Showers in the energy range 100 TeV to 10 PeV

    OpenAIRE

    Wilkens, Henric George Sacha

    2003-01-01

    The L3+C experiment at CERN combines a small Air Shower array with a high resolution muon spectrometer, located under 30 m of overburden. The measurement of the shower particle density combined with the measurement of cosmic ray induced muons in the L3 spectrometer allows for a detailed check of theoretical models of air shower creation and development

  17. Wide field-of-view Cherenkov telescope for the detection of cosmic rays in coincidence with the Yakutsk extensive air shower array

    International Nuclear Information System (INIS)

    The Yakutsk array group is developing a wide field-of-view Cherenkov telescope to be operated in coincidence with the surface detectors of the extensive air shower array. Currently, the engineering prototype of the reflecting telescope with the front-end electronics is designed, assembled, and tested to demonstrate the feasibility of the conceived instrument. The status and specifications of the prototype telescope are presented, as well as the modernization program of the already existing Cherenkov light detectors subset of the array measuring ultra-high energy cosmic rays

  18. Multi-TeV Gamma-Ray Flares from Markarian 421 in 2000 and 2001 Observed with the Tibet Air Shower Array

    OpenAIRE

    Amenomori, M.

    2003-01-01

    Several strong TeV gamma-ray flares were detected from Markarian 421 in the years 2000 and 2001 by the Tibet III air shower array at a level of statistical significance of 5.1 sigma. Markarian 421 was unprecedentedly active at X-ray and TeV gamma-ray energies during this period, and a positive correlation was found between the change of the ASM/RXTE X-ray flux and the Tibet TeV gamma-ray flux. When a power-law energy spectrum for gamma-rays from this source is assumed, the spectral index is c...

  19. Radio Detection of Horizontal Extensive Air Showers with AERA

    CERN Document Server

    ,

    2015-01-01

    AERA, the Auger Engineering Radio Array, located at the Pierre Auger Observatory in Malarg\\"ue, Argentina measures the radio emission of extensive air showers in the 30-80 MHz frequency range and is optimized for the detection of air showers up to 60$^{\\circ}$ zenith angle. In this contribution the motivation, the status, and first results of the analysis of horizontal air showers with AERA will be presented.

  20. The angular resolution of air shower gamma ray telescopes

    Science.gov (United States)

    Morello, C.; Navarra, G.; Periale, L.; Vallania, P.

    1985-01-01

    A crucial charactristic of air shower arrays in the field of high energy gamma-ray astronomy is their angular resolving power, the arrival directions being obtained by the time of flight measurements. A small air shower array-telescope is used to study the resolution in the definition of the shower front as a function of the shower size.

  1. Radio Measurements of Air Showers with LOPES

    International Nuclear Information System (INIS)

    LOPES is a digital antenna array for the radio measurement of cosmic-ray air showers at energies around 1017 eV. It is triggered by the KASCADE-Grande air-shower array at the Karlsruhe Institute of Technology (KIT), Germany. Because of an absolute amplitude calibration and a sophisticated data analysis, LOPES can test models for the radio emission to an up-to-now unachieved level, thus improving our understanding of the radio emission mechanisms. Recent REAS simulations of the air-shower radio emission come closer to the measurements than any previously tested simulations. We have determined the radio-reconstruction precision of interesting air-shower parameters by comparing LOPES reconstructions to both REAS simulations and KASCADE-Grande measurements, and present our latest results for the angular resolution, the energy and the Xmax reconstruction based on the radio measurement of about 500 air showers. Although the precision of LOPES is limited by the high level of anthropogenic noise at KIT, it opens a promising perspective for next-generation radio arrays in regions with a lower ambient noise level.

  2. A primary result to search for 3 TeV γ-ray bursts by using data of Tibet HD air shower array

    International Nuclear Information System (INIS)

    A search for γ-ray bursts at 3 TeV energy region was done by using the data of Tibet HD air shower array, which was obtained in the period of February 1997-June 1998. About 2.5 x 109 EAS events were analysed to search for the shower clusters appearing in a fixed time interval and small sky bin. An equal-zenith angle method is used to estimate the background and three different time intervals (Δt = 1, 10, 100 s) were adopted in the research. A part of clusters show excess over the background and some significances are greater than 3σ obviously. Although a few clusters reach 4σ significance, the result of this work can not be considered to show the evidence of γ-ray bursts; instead it just indicated that the air shower array of Tibet HD now has higher sensitivity for γ-ray bursts compared to that of Tibet I and II. Much higher sensitivity in near future is expected to give clear evidence of 1-100 TeV γ-ray bursts

  3. Detection of Multi-TeV $\\gamma$ Rays from Markarian 501 during an Unforeseen Flaring State in 1997 with the Tibet Air Shower Array

    CERN Document Server

    Amenomori, M; Cao, P Y; Danzengluobu; Ding, L K; Feng, Z Y; Fu, Y; Guo, H W; He, M; Hibino, K; Hotta, N; Huang, Q; Huo, A X; Izu, K; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Labaciren; Li Jing Yi; Lü, H; Lu, S L; Luo, G X; Meng, X R; Mizutani, K; Mu, J; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Ouchi, T; Ren, J R; Saitô, T; Sakata, M; Sasaki, T; Shi, Z Z; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Taira, K; Tan, Y H; Tateyama, N; Torii, S; Utsugi, T; Wang, C R; Wang, H; Xu, X W; Yamamoto, Y; Yu, G C; Yuan, A F; Yuda, T; Zhang, C S; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zha Xi Ciren; Zhaxi Sang Zhu; Zhou, W D

    2000-01-01

    In 1997, the BL Lac Object Mrk 501 entered a very active phase and was thebrightest source in the sky at TeV energies, showing strong and frequentflaring. Using the data obtained with a high density air shower array that hasbeen operating successfully at Yangbajing in Tibet since 1996, we searched forgamma-ray signals from this source during the period from February throughAugust in 1997. Our observation detected multi-TeV $\\gamma$-ray signals at the3.7-Sigma level during this period. The most rapid increase of the excesscounts was observed between April 7 and June 16 and the statisticalsignificance of the excess counts in this period was 4.7-Sigma. Among severalobservations of flaring TeV gamma-rays from Mrk 501 in 1997, this is the onlyobservation using a conventional air shower array. We present the energyspectrum of gamma-rays which will be worthy to compare with those obtained byimaging atmospheric Cerenkov telescopes.

  4. Structure of air shower disc near the core

    Science.gov (United States)

    Inoue, N.; Kawamoto, M.; Misaki, Y.; Maeda, T.; Takeuchi, T.; Toyoda, Y.

    1985-01-01

    The longitudinal structure of the air shower disk is studied by measuring the arrival time distributions of air shower particles for showers with electron size in the range 3.2 x 10 to the 5.5. power to 3.2 x 10 to the 7.5 power in the Akeno air-shower array (930 gcm squared atmospheric depth). The average FWHM as a parameter of thickness of air shower disk increases with core distances at less than 50m. AT the present stage, dependence on electron size, zenith angle and air shower age is not apparent. The average thickness of the air shower disk within a core distance of 50m could be determined by an electromagnetic cascade starting from the lower altitude.

  5. Search for Gamma Rays above 100 TeV from the Crab Nebula with the Tibet Air Shower Array and the 100 m2 muon Detector

    Science.gov (United States)

    Amenomori, M.; Bi, X. J.; Chen, D.; Chen, T. L.; Chen, W. Y.; Cui, S. W.; Danzengluobu; Ding, L. K.; Feng, C. F.; Feng, Zhaoyang; Feng, Z. Y.; Gou, Q. B.; Guo, Y. Q.; He, H. H.; He, Z. T.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, H. B.; Huang, J.; Jia, H. Y.; Jiang, L.; Kajino, F.; Kasahara, K.; Katayose, Y.; Kato, C.; Kawata, K.; Kozai, M.; Labaciren; Le, G. M.; Li, A. F.; Li, H. J.; Li, W. J.; Liu, C.; Liu, J. S.; Liu, M. Y.; Lu, H.; Meng, X. R.; Miyazaki, T.; Mizutani, K.; Munakata, K.; Nakajima, T.; Nakamura, Y.; Nanjo, H.; Nishizawa, M.; Niwa, T.; Ohnishi, M.; Ohta, I.; Ozawa, S.; Qian, X. L.; Qu, X. B.; Saito, T.; Saito, T. Y.; Sakata, M.; Sako, T. K.; Shao, J.; Shibata, M.; Shiomi, A.; Shirai, T.; Sugimoto, H.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, S.; Tsuchiya, H.; Udo, S.; Wang, H.; Wu, H. R.; Xue, L.; Yamamoto, Y.; Yamauchi, K.; Yang, Z.; Yasue, S.; Yuan, A. F.; Yuda, T.; Zhai, L. M.; Zhang, H. M.; Zhang, J. L.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhang, Ying; Zhaxisangzhu; Zhou, X. X.; Tibet ASγ Collaboration

    2015-11-01

    A 100 m2 muon detector (MD) was successfully constructed under the existing Tibet air shower (AS) array in the late fall of 2007. The sensitivity of the Tibet AS array to cosmic gamma rays can be improved by selecting muon-poor events with the MD. Our MC simulation of the MD response reasonably agrees with the experimental data in terms of the charge distribution for one-muon events and the background rejection power. Using the data collected by the Tibet AS array and the 100 m2 MD taken from 2008 March to 2010 February, we search for continuous gamma-ray emission from the Crab Nebula above ∼100 TeV. No significant excess is found, and the most stringent upper limit is obtained above 140 TeV.

  6. GRAPES-3-A high-density air shower array for studies on the structure in the cosmic-ray energy spectrum near the knee

    International Nuclear Information System (INIS)

    The change in the spectral index from about -2.7 to -3.1 at ∼3x1015eV in the all-particle energy spectrum of primary cosmic rays is very significant for learning about the nature of cosmic sources of ultra-high energy particles and their acceleration and propagation in the galactic disk. Any observation of a fine structure in the spectrum would be important for improving our understanding of these physical processes. The GRAPES-3 air shower array has been designed to achieve higher precision in determination of various shower parameters to enable observation of any fine structure in the energy spectrum, if it exists. The details of the shower detectors, shower trigger and the data acquisition system are presented here along with estimates of trigger efficiencies from Monte Carlo simulations for primary photons (γ-rays) and several nuclei

  7. Observation by an air-shower array in Tibet of the multi-TeV cosmic-ray anisotropy due to terrestrial orbital motion around the Sun.

    Science.gov (United States)

    Amenomori, M; Ayabe, S; Cui, S W; Danzengluobu; Ding, L K; Ding, X H; Feng, C F; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Hu, Haibing; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren; Le, G M; Li, J Y; Lu, H; Lu, S L; Meng, X R; Mizutani, K; Mori, S; Mu, J; Munakata, K; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saito, T; Sakata, M; Sasaki, T; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Utsugi, T; Wang, B S; Wang, H; Wang, X; Wang, Y G; Wu, H R; Xue, L; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Zhang, Y; Zhaxisangzhu; Zhou, X X

    2004-08-01

    We report on the solar diurnal variation of the galactic cosmic-ray intensity observed by the Tibet III air shower array during the period from 1999 to 2003. In the higher-energy event samples (12 and 6.2 TeV), the variations are fairly consistent with the Compton-Getting anisotropy due to the terrestrial orbital motion around the Sun, while the variation in the lower-energy event sample (4.0 TeV) is inconsistent with this anisotropy. This suggests an additional anisotropy superposed at the multi-TeV energies, e.g., the solar modulation effect. This is the highest-precision measurement of the Compton-Getting anisotropy ever made. PMID:15323615

  8. Radio detection of cosmic ray induced air showers at the Pierre Auger Observatory

    International Nuclear Information System (INIS)

    AERA - the Auger Engineering Radio Array - is currently being set up at the southern site of the Pierre Auger Observatory. AERA will explore the potential of the radio-detection technique to cosmic ray induced air showers with respect to the next generation of large-scale surface detectors. As AERA is co-located with the low-energy enhancements of the Pierre Auger Observatory, the observation of air showers in coincidence with the Auger surface and fluorescence detector will allow to study the radio emission processes in detail and to calibrate the radio signal. Finally, the combined reconstruction of shower parameters with three independent techniques promises new insights into the nature of cosmic rays in the transition region from 1017 to 1019 eV. Besides the detection of coherent radiation in the MHz frequency range, the setups AMBER - Air-shower Microwave Bremsstrahlung Experimental Radiometer - and MIDAS - MIcrowave Detection of Air Showers - prepare to check the possibility to detect air showers due the emission of molecular bremsstrahlung in the GHz range at the Auger site. This article presents the status of the radio-detection setups and discusses their physics potential as well as experimental challenges. Special focus is laid on the first stage of AERA which is the startup to the construction of a 20 km2 radio array.

  9. Observation of microwave emission from extensive air showers with CROME

    Directory of Open Access Journals (Sweden)

    Wilczyński H.

    2013-06-01

    Full Text Available We report on the measurement of microwave radio signals from air showers with the CROME (Cosmic Ray Observation via Microwave Emission experiment. CROME is located in the center of the KASCADE-Grande air shower array. The radio signals of the CROME antennas are stored for each high-energy trigger from the KASCADE-Grande array and matched offine with the KASCADE-Grande data. After almost one year of data taking microwave signals have been observed for more than ten air showers.

  10. Acoustic detection of air shower cores

    Science.gov (United States)

    Gao, X.; Liu, Y.; Du, S.

    1985-01-01

    At an altitude of 1890m, a pre-test with an Air shower (AS) core selector and a small acoustic array set up in an anechoic pool with a volume of 20x7x7 cu m was performed, beginning in Aug. 1984. In analyzing the waveforms recorded during the effective working time of 186 hrs, three acoustic signals which cannot be explained as from any source other than AS cores were obtained, and an estimation of related parameters was made.

  11. A study of the shadowing of galactic cosmic rays by the sun in a quiet phase of solar activity with the Tibet air shower array

    CERN Document Server

    Amenomori, M

    2000-01-01

    We have shown that the Sun's shadow by high energy cosmic rays moves year by year and its behavior is correlated with a time variation of the large-scale structure of the solar and interplanetary magnetic fields. The solar activity was near minimum in the period from 1996 through 1997. Using the data obtained with the Tibet air shower array, we examined the shadowing of cosmic rays by the Sun in this quiet phase of solar cycle, and found that the Sun's shadow was just in the apparent direction of the Sun, though it was observed at the position considerably away from the Sun to the south-west in the period between 1990 and 1993. It is known that the magnetic pole of equivalent solar dipole was reversed during the previous active phase, and near solar minimum the dipole was aligned with the rotating axis, preserving its N-pole on the north pole side of the Sun. This causes the solar magnetic field to shift the Sun's shadow to the east. Thus, the observed results suggest that the shift of the Sun's shadow due to...

  12. Study of hadronic component in air showers at Mt. Chacaltaya

    International Nuclear Information System (INIS)

    An experiment to operate an air shower array, a burst detector (or a hadron calorimeter) and an emulsion chamber is under way at Mt. Chacaltaya (5,200 m, Bolivia), in order to study the hadron interactions and the primary cosmic rays in the energy region exceeding 1015 eV. The number of hadrons in the air shower, detected by the burst detector, indicates that the proton fraction among the primary cosmic rays exceeds 50 %

  13. Radio detection of air showers with LOFAR and AERA

    CERN Document Server

    Hörandel, Jörg R

    2015-01-01

    High-energy cosmic rays impinging onto the atmosphere of the Earth initiate extensive air showers. With the LOFAR radio telescope and the Auger Engineering Radio Array (AERA) at the Pierre Auger Observatory radio emission from air showers is detected. Recent results are presented from both experiments. The measured properties of the radio emission are described. The measurements are used to derive the properties of high-energy cosmic rays: their arrival direction, energy, and particle type (mass).

  14. Dependence of the Energy Spectrum of UHE Cosmic Rays on the Latitude of an Extensive Air Shower Array

    CERN Document Server

    Glushkov, A V

    2012-01-01

    Several energy spectra of cosmic rays with energies E_0 \\geq 10^17 eV measured at the Yakutsk EAS, AGASA, Haverah Park, HiRes, Auger, and SUGAR arrays are considered. It is shown that the fairly good mutual agreement of the spectrum shapes can be achieved if the energy of each spectrum is multiplied by a factor K specific for each spectrum. These factors exhibit a pronounced dependence on the latitude of the above-mentioned arrays.

  15. Observation of Polarised Microwave Emission from Cosmic Ray Air Showers

    CERN Document Server

    Smida, R; Engel, R; Arteaga-Velazquez, J C; Bekk, K; Bertaina, M; Bluemer, J; Bozdog, H; Brancus, I M; Chiavassa, A; Cossavella, F; Di Pierro, F; Doll, P; Fuchs, B; Fuhrmann, D; Grupen, C; Haungs, A; Heck, D; Hoerandel, J R; Huber, D; Huege, T; Kampert, K -H; Kang, D; Klages, H; Kleifges, M; Kroemer, O; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Mayer, H J; Mathys, S; Melissas, M; Morello, C; Neunteufel, P; Oehlschlaeger, J; Palmieri, N; Pekala, J; Pierog, T; Rautenberg, J; Rebel, H; Riegel, M; Roth, M; Salamida, F; Schieler, H; Schoo, S; Schroeder, F G; Sima, O; Stasielak, J; Toma, G; Trinchero, G C; Unger, M; Weber, M; Weindl, A; Wilczynski, H; Will, M; Wochele, J; Zabierowski, J

    2013-01-01

    We report on the first direct measurement of the basic features of microwave radio emission from extensive air showers. Using a trigger provided by the KASCADE-Grande air shower array, the signals of the microwave antennas of the CROME (Cosmic-Ray Observation via Microwave Emission) experiment have been read out and searched for signatures of radio emission by high-energy air showers. Microwave signals have been detected for more than 30 showers with energies above $3\\times10^{16}$\\,eV. The observations presented in this Letter are consistent with a mainly forward-beamed, coherent and polarised emission process in the GHz frequency range. An isotropic, unpolarised radiation is disfavoured as the dominant emission model. The measurements show that microwave radiation offers a new means of studying air showers at very high energy.

  16. Phenomenology of extensive air showers

    International Nuclear Information System (INIS)

    High energy primary cosmic rays, when penetrating from the outer space into the Earth's atmosphere initiate the development of so called Extensive Air Showers (EAS) by the multiparticle production of the cascading interactions of the primary particle with nuclei of atmospheric molecules and nuclei. A careful study of the EAS development, distributing the large energy of the primary particle (p, He, C, N, O, . . .Fe) among billions of secondary particles, which move like a wide particle pancake through the atmosphere and can be experimentally studied with largely extended ground based detector arrays, provide an indirect access to information about the energy and nature of the primary radiation. The lecture introduces in a tutorial way the phenomenological features of the EAS development, the formation of the different shower components (electrons, photons, muons, hadrons and air-Cherenkov radiation) and considers various EAS parameters (total intensities (sizes), lateral and arrival time distributions, etc.) as observables of experimental studies. The most important interaction ingredients which drive the EAS development and lead to the appearance at ground are discussed, in particular in view of a basic understanding and conducting realistic Monte Carlo simulations of the EAS features. The presentation will be illustrated with various recent results of the KASCADE experiment, for which a short account is given. (author)

  17. A Northern Sky Survey for Steady TeV Gamma-Ray Point Sources Using the Tibet Air Shower Array

    CERN Document Server

    Amenomori, M; Cui, S W; Danzengluobu; Ding, L K; Ding, X H; Feng Cun Feng; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Haibing, H; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren; Le, G M; Li, J Y; Lü, H; Lu, S L; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saitô, T; Sakata, M; Sasaki, T; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takashima, M; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Utsugi, T; Wang, H; Wang, X; Wang, Y G; Wu, H R; Xue Liang; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S I; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Yi Zhang; Zhang, Y; Zhaxi Sang Zhu; Zhou, X X

    2005-01-01

    Results on TeV gamma-ray point source search using data taken from the Tibet HD (Feb. 1997 -- Sep. 1999) and Tibet III (Nov. 1999 -- Oct. 2001) arrays are presented. From 0 degree to 60 degree in declination (Dec), significan t excesses from the well-known steady source Crab Nebula and the high state of the flare type source Markarian 421 ar e observed. Because the levels of significance from other positions are not sufficiently high, a 90% confidence leve l (CL) upper limit on the flux is set assuming a Crab like energy spectrum. To allow cross-checking, two independentl y developed analyses are used in this work.

  18. Muonic footprint of simulated extensive air showers

    International Nuclear Information System (INIS)

    The number of muons at ground is one of the major parameters in extensive air showers to discriminate hadronic showers from photon ones. There are already numerous studies focusing on this matter and on using the muon content in combination with other parameters. In our study, we use CORSIKA showers for photon and proton primaries at E=1018 eV without thinning of shower muons to analyze the structure of the muonic footprint at different core distances.

  19. Large-Scale Sidereal Anisotropy of Galactic Cosmic-Ray Intensity Observed by the Tibet Air Shower Array

    CERN Document Server

    Amenomori, M; Cui, S W; Danzengluobu; Ding, L K; Ding, X H; Feng Cun Feng; Feng, Z Y; Gao, X Y; Geng, Q X; Guo, H W; He, H H; He, M; Hibino, K; Hotta, N; Haibing, H; Hu, H B; Huang, J; Huang, Q; Jia, H Y; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kawata, K; Labaciren; Le, G M; Li, J Y; Lü, H; Lu, S L; Meng, X R; Mizutani, K; Mu, J; Munakata, K; Nagai, A; Nanjo, H; Nishizawa, M; Ohnishi, M; Ohta, I; Onuma, H; Ouchi, T; Ozawa, S; Ren, J R; Saitô, T; Sakata, M; Sasaki, T; Shibata, M; Shiomi, A; Shirai, T; Sugimoto, H; Takashima, M; Takita, M; Tan, Y H; Tateyama, N; Torii, S; Tsuchiya, H; Udo, S; Utsugi, T; Wang, H; Wang, X; Wang, Y G; Wu, H R; Xue Liang; Yamamoto, Y; Yan, C T; Yang, X C; Yasue, S I; Ye, Z H; Yu, G C; Yuan, A F; Yuda, T; Zhang, H M; Zhang, J L; Zhang, N J; Zhang, X Y; Yi Zhang; Zhang, Y; Zhaxi Sang Zhu; Zhou, X X

    2005-01-01

    We present the large-scale sidereal anisotropy ofgalactic cosmic-ray intensity in the multi-TeV region observed with the Tibet-IIIair shower array during the period from 1999 through 2003. The sidereal daily variation of cosmic rays observed in this experiment shows an excess of relative intensity around $4\\sim7 $ hours local sidereal time, as well as a deficit around 12 hours local sidereal time. While the amplitude of the excess is not significant when averaged over all declinations, the excess in individual declinaton bands becomes larger and clearer as the viewing direction moves toward the south. The maximum phase of the excess intensity changes from $\\sim$7 at the northern hemisphere to $\\sim$4 hours at the equatorial region. We also show that both the amplitude and the phase of the first harmonic vector of the daily variation are remarkably independent of primary energy in the multi-TeV region. This is the first result determining the energy and declination dependences of the full 24-hour profiles of t...

  20. Radio signal correlation at 32 MHz with extensive air showers parameters

    Science.gov (United States)

    Knurenko, Stanislav; Petrov, Igor

    2015-08-01

    The paper presents correlations of radio signals measured at the Yakutsk array with air shower parameters: the shower energy E0 and the depth of maximum Xmax. It is shown that from radio emission measurements of air showers one can obtain individual shower parameters and hence, the mass composition of cosmic rays. In addition, we also derived a generalized formula for calculating the primary energy of the air showers.

  1. CONEX and CORSIKA: a new 3D hybrid model for air shower simulation

    International Nuclear Information System (INIS)

    The hybrid air shower simulation code CONEX has been implemented as an option in the air shower Monte-Carlo model CORSIKA. In CONEX, Monte-Carlo simulation of high energy interactions is combined with a fast numerical solution of cascade equations. Low energy secondary particles can then be tracked within CORSIKA to obtain the lateral extension of the air shower. This allows the fast and realistic simulation of 3D showers at ultra-high energies.

  2. Search for coincident air showers in the network observation

    International Nuclear Information System (INIS)

    Here we report results of the coincident event analysis, using air shower data taken at six stations of the Large Area Air Shower (LAAS) group in Japan. In this analysis we search for pairs of coincident air showers between stations, which are hypothetically induced by bursts of ultra-high-energy γ-ray sources or by secondary particles from interactions of extremely-high-energy cosmic rays with interstellar matter. From four years data (2.3 x 106 air showers) we find a pair of air showers with a very small time difference of 195 microseconds and an angular distance of 5.3 degrees, which is within the angular accuracy of our arrays, between two stations separated by 152 km. The chance probability of this event is 0.16. The Crab Nebula, a well-known ultra-high-energy γ-ray source, is within the angular accuracy from the arrival direction of this event. We expect that this event was induced by the ultra-high-energy γ-rays emitted in a burst of the Crab Nebula

  3. Air showers and geomagnetic field

    International Nuclear Information System (INIS)

    The influence of the geomagnetic field on the development of air showers is studied. The well known International Geomagnetic Reference Field was included in the AIRES air shower simulation program as an auxiliary tool to allow the calculation of very accurate estimations of the geomagnetic field given the geographic coordinates, altitude above sea level and date of a given event. Our simulations indicate that the geomagnetic deflections significantly alter some shower observables such as, for example, the lateral distribution of muons in the case of events with large zenith angles (larger than 75 deg.). On the other hand, such alterations seem to be unimportant for smaller zenith angles. Global observables such as the total number of particles or longitudinal development parameters do not present appreciable dependences on the geomagnetic deflections for all the cases that were studied. (author)

  4. Study of hadronic component in air showers at Mt. Chacaltaya

    International Nuclear Information System (INIS)

    An experiment of an air shower array, a hadron calorimeter (8 m2) and an emulsion chamber (8 m2, 15 cm Pb) is under way at Mt. Chacaltaya (5200 m above sea level, Bolivia), in order to study the hadron interactions and the primary cosmic rays in the energy region exceeding 1015 eV. The number of particles in the hadronic component in the air shower, which is detected by the hadron calorimeter, is not compatible with that obtained by simulations, indicating that violation of the Feynman scaling law is stronger at 1016 eV than the one assumed in the simulations. The average mass number of the primary cosmic rays, estimated from the distribution of the number of hadrons in the air shower, is = 2.8 ± 0.5 at 1016 eV

  5. Air shower detectors in gamma-ray astronomy

    Energy Technology Data Exchange (ETDEWEB)

    Sinnis, Gus [Los Alamos National Laboratory

    2008-01-01

    Extensive air shower (EAS) arrays directly detect the particles in an EAS that reach the observation altitude. This detection technique effectively makes air shower arrays synoptic telescopes -- they are capable of simultaneously and continuously viewing the entire overhead sky. Typical air shower detectors have an effective field-of-view of 2 sr and operate nearly 100% of the time. These two characteristics make them ideal instruments for studying the highest energy gamma rays, extended sources and transient phenomena. Until recently air shower arrays have had insufficient sensitivity to detect gamma-ray sources. Over the past decade, the situation has changed markedly. Milagro, in the US, and the Tibet AS{gamma} array in Tibet, have detected very-high-energy gamma-ray emission from the Crab Nebula and the active galaxy Markarian 421 (both previously known sources). Milagro has discovered TeV diffuse emission from the Milky Way, three unidentified sources of TeV gamma rays, and several candidate sources of TeV gamma rays. Given these successes and the suite of existing and planned instruments in the GeV and TeV regime (AGILE, GLAST, HESS, VERITAS, CTA, AGIS and IceCube) there are strong reasons for pursuing a next generation of EAS detectors. In conjunction with these other instruments the next generation of EAS instruments could answer long-standing problems in astrophysics.

  6. Radio Detection of Air Showers with LOFAR and AERA

    Science.gov (United States)

    Hörandel, Jörg R.

    Radio detection of extensive air showers is a new method to measure the properties of high-energy cosmic rays. Recent results are reviewed from the LOFAR radio telescope and the Auger Engineering Radio Array (AERA) at the Pierre Auger Observatory.

  7. Measurements of the muonic component of air showers at the Pierre Auger Observatory

    Directory of Open Access Journals (Sweden)

    Allen Jeff

    2013-06-01

    Full Text Available Several methods have been developed by the Pierre Auger Collaboration to estimate the muon content of air showers from ultra-high energy cosmic rays. The data of the Pierre Auger Observatory will be compared with predictions based upon EPOS 1.99 and QGSJET-II-3 hadronic interaction models. In addition to the direct measures of the muonic content, the combination of a fluorescence detector and a muon sensitive surface array allows for a direct test of air shower simulations which is sensitive to both the shower core and large distances from the core. These methods reveal a deficit of muons in air shower simulations with proton primaries and that the energy assignment basedupon simulations of the surface array signal is systematically higher than that derived from the florescence detector. Summary: I will discuss the deficit in the number of muons currently predicted by simulations when compared to the data of the Pierre Auger Observatory. I will describe the methods used to measure the muon content, including sources of systematic uncertainty, and give their current results. Finally, I will present the Collaborations current understanding of the nature of the discrepancy, which could arise from an energy scale problem, composition, or deficiencies in the hadronic interaction models. See references [1, 2].

  8. The all-particle spectrum of primary cosmic rays in the wide energy range from 10^14 eV to 10^17 eV observed with the Tibet-III air-shower array

    CERN Document Server

    Amenomori, M

    2008-01-01

    We present an updated all-particle energy spectrum of primary cosmic rays in a wide range from 10^14 eV to 10^17 eV using 5.5 times 10^7 events collected in the period from 2000 November through 2004 October by the Tibet-III air-shower array located at 4300 m above sea level (atmospheric depth of 606 g/cm^2). The size spectrum exhibits a sharp knee at a corresponding primary energy around 4 PeV. This work uses increased statistics and new simulation calculations for the analysis. We performed extensive Monte Carlo calculations and discuss the model dependences involved in the final result assuming interaction models of QGSJET01c and SIBYLL2.1 and primary composition models of heavy dominant (HD) and proton dominant (PD) ones. Pure proton and pure iron primary models are also examined as extreme cases. The detector simulation was also made to improve the accuracy of determining the size of the air showers and the energy of the primary particle. We confirmed that the all-particle energy spectra obtained under v...

  9. Muon production in extended air shower simulations.

    Science.gov (United States)

    Pierog, T; Werner, K

    2008-10-24

    Whereas air shower simulations are very valuable tools for interpreting cosmic ray data, there is a long-standing problem: it is difficult to accommodate at the same time the longitudinal development of air showers and the number of muons measured on the ground. Using a new hadronic interaction model (EPOS) in air shower simulations produces much more muons, in agreement with results from the HiRes-MIA experiment. We find that this is mainly due to a better description of (anti) baryon production in hadronic interactions. This is an aspect of air shower physics which has been neglected so far. PMID:18999734

  10. LHC data and extensive air showers

    Directory of Open Access Journals (Sweden)

    Pierog Tanguy

    2013-06-01

    Full Text Available Currently the uncertainty in the prediction of shower observables for different primary particles and energies is dominated by differences between hadronic interaction models. The LHC data on minimum bias measurements can be used to test Monte Carlo generators and these new constraints will help to reduce the uncertainties in air shower predictions. In this article, after a short introduction on air showers we will show the results of the comparison between the updated version of high energy hadronic interaction models EPOS LHC and QGSJETII-04 with LHC data. Results for air shower simulations and their consequences on comparisons with air shower data will be discussed.

  11. LHC data and extensive air showers

    International Nuclear Information System (INIS)

    Currently the uncertainty in the prediction of shower observables for different primary particles and energies is dominated by differences between hadronic interaction models. The LHC data on minimum bias measurements can be used to test Monte Carlo generators and these new constraints will help to reduce the uncertainties in air shower predictions. In this article, after a short introduction on air showers we will show the results of the comparison between the updated version of high energy hadronic interaction models EPOS LHC and QGSJETII-04 with LHC data. Results for air shower simulations and their consequences on comparisons with air shower data will be discussed. (authors)

  12. Air-Shower Spectroscopy at horizons

    OpenAIRE

    Fargion, D.

    2005-01-01

    Horizontal and Upward air-showers are suppressed by deep atmosphere opacity and by the Earth shadows. In such noise-free horizontal and upward directions rare Ultra High Cosmic rays and rarer neutrino induced air-showers may shine, mostly mediated by resonant PeVs interactions in air or by higher energy Tau Air-showers originated by neutrino tau skimming the Earth. At high altitude (mountains, planes, balloons) the air density is so rarefied that nearly all common air-showers might be observe...

  13. Estimation of the diffuse γ-flux in the PeV-region using the measurements of the KASCADE air shower array

    International Nuclear Information System (INIS)

    Data observed with the KASCADE extensive air shower experiment are analysed with respect to a possible contribution by primary gamma rays in the energy range of 0.3 to 10 PeV. The study makes use of the good reconstruction of the number of particles based on the signals measured with the electron and muon detectors of the experiment. Possible γ-induced events are mainly identified by their low muon to electron ratios but, in addition, the steepness and the smoothness of the electron lateral distributions are exploited. A comparison with simulation studies of γ-induced showers leads to several separation areas. No positive identifications can be claimed until now, but the results confirm and improve the upper limits of a possible gamma contribution made by previous experiments. The search for anisotropies of the γ-radiation based on the arrival directions of possible γ-induced events shows no significance with respect to point sources. (orig.)

  14. Large high altitude air shower observatory (LHAASO) project

    International Nuclear Information System (INIS)

    The Large High Altitude Air Shower Observatory (LHAASO) project focuses mainly on the study of 40 GeV-1 PeV gamma ray astronomy and 10 TeV-1 EeV cosmic ray physics. It consists of a 1 km2 extensive air shower array with 40 000 m2 muon detectors, 90,000m2 water Cerenkov detector array, 5 000 m2 shower core detector array and an air Cerenkov/fluorescence telescope array. Prototype detectors are designed with some of them already in operation. A prototype array of 1% size of LHAASO will be built at the Yangbajing Cosmic Ray Observatory and used to coincidently measure cosmic rays with the ARGO-YBJ experiment. (authors)

  15. LOPES Detecting Radio Emission from Cosmic Ray Air Showers

    CERN Document Server

    Horneffer, A; Apel, W D; Badea, F; Bekk, K; Bercuci, A; Bertaina, M; Blümer, H; Bozdog, H; Brancus, I M; Bruggemann, M; Buchholz, P; Büttner, C; Chiavassa, A; Daumiller, K; De Vos, C M; Doll, P; Engel, R; Engler, J; Falcke, H; Fessler, F; Ghia, P L; Gils, H J; Glasstetter, R; Haungs, A; Heck, D; Hörandel, J R; Huege, T; Kampert, K H; Kant, G W; Klages, H O; Kolotaev, Yu; Maier, G; Mathes, H J; Mayer, H J; Milke, J; Morello, C; Müller, M; Navarra, G; Obenland, R; Oehlschläger, J; Ostapchenko, S; Petcu, M; Plewnia, S; Rebel, H; Risse, A; Roth, M; Schieler, H; Scholz, J; Stumpert, M; Thouw, T; Trinchero, G C; Ulrich, H; Valchierotti, S; Van Buren, J; Walkowiak, W; Weindl, A; Wochele, J; Zabierowski, J; Zagromski, S

    2004-01-01

    Radio pulses emitted in the atmosphere during the air shower development of high-energy primary cosmic rays were measured during the late 1960ies in the frequency range from 2 MHz to 520 MHz. Mainly due to difficulties with radio interference these measurements ceased in the late 1970ies. LOFAR (Low Frequency Array) is a new digital radio interferometer under development. Using high bandwidth ADCs and fast data processing it will be able to filter out most of the interference. By storing the whole waveform information in digital form one can analyze transient events like air showers even after they have been recorded. To test this new technology and to demonstrate its ability to measure air showers a "LOFAR Prototype Station" (LOPES) is set up to operate in conjunction with an existing air shower array (KASCADE-Grande). The first phase consisting of 10 antennas is already running. It operates in the frequency range of 40 to 80 MHz, using simple short dipole antennas and direct 2nd Nyquist sampling of the inco...

  16. A likelihood method to cross-calibrate air-shower detectors

    Science.gov (United States)

    Dembinski, Hans Peter; Kégl, Balázs; Mariş, Ioana C.; Roth, Markus; Veberič, Darko

    2016-01-01

    We present a detailed statistical treatment of the energy calibration of hybrid air-shower detectors, which combine a surface detector array and a fluorescence detector, to obtain an unbiased estimate of the calibration curve. The special features of calibration data from air showers prevent unbiased results, if a standard least-squares fit is applied to the problem. We develop a general maximum-likelihood approach, based on the detailed statistical model, to solve the problem. Our approach was developed for the Pierre Auger Observatory, but the applied principles are general and can be transferred to other air-shower experiments, even to the cross-calibration of other observables. Since our general likelihood function is expensive to compute, we derive two approximations with significantly smaller computational cost. In the recent years both have been used to calibrate data of the Pierre Auger Observatory. We demonstrate that these approximations introduce negligible bias when they are applied to simulated toy experiments, which mimic realistic experimental conditions.

  17. Microwave detection of air showers with MIDAS

    Czech Academy of Sciences Publication Activity Database

    Facal San Luis, P.; Alekotte, I.; Alvarez, J.; Berlin, A.; Bertou, X.; Bogdan, M.; Boháčová, Martina; Bonifazi, C.; Carvalho, W.R.; de Mello Neto, J.R.T.; Genat, J.F.; Mills, E.; Monasor, M.; Privitera, P.; Reyes, I.C.; d´Orfeuil, B.R.; Santos, E.M.; Wayne, S.; Williams, C.; Zas, E.

    2012-01-01

    Roč. 662, Sup. 1 (2012), "S118"-"S123". ISSN 0168-9002 R&D Projects: GA MŠk(CZ) LA08016 Institutional research plan: CEZ:AV0Z10100502 Keywords : MIDAS (Microwave Detector of Air Showers) * extensive air showers Subject RIV: BF - Elementary Particles and High Energy Physics Impact factor: 1.142, year: 2012

  18. Extensive Air Showers in the Classroom

    Science.gov (United States)

    Badala, A.; Blanco, F.; La Rocca, P.; Pappalardo, G. S.; Pulvirenti, A.; Riggi, F.

    2007-01-01

    The basic properties of extensive air showers of particles produced in the interaction of a high-energy primary cosmic ray in the Earth's atmosphere are discussed in the context of educational cosmic ray projects involving undergraduate students and high-school teams. Simulation results produced by an air shower development code were made…

  19. Disentangling the air shower components using scintillator and water Cherenkov detectors

    Directory of Open Access Journals (Sweden)

    Roth Markus

    2013-06-01

    Full Text Available We consider a ground array of scintillation and water Cherenkov detectors with the purpose of determining the muon content of air showers. The different response characteristics of these two types of detectors to the components of the air shower provide a way to infer their relative contributions. We use a detailed simulation to estimate the impact of parameters, such as scintillation detector size, in the determination of the size of the muon component.

  20. Study of nuclear interactions by observing family and air showers at Mt. Chacaltaya

    International Nuclear Information System (INIS)

    It was operated an air shower array and an emulsion chamber simultaneously at Mt. Chacaltaya (5200 m, Bolivia), in order to study high energy nuclear interactions, induced by cosmic rays. It was showed that high energy electromagnetic component and hadronic component in the air shower are not described by the simulations, indicating that the energy spectrum of produced particles in multiple particle production is suppressed strongly in the forward region

  1. Energetic delayed hadrons in large air showers observed at 5200m above sea level

    Science.gov (United States)

    Kaneko, T.; Hagiwara, K.; Yoshii, H.; Martinic, N.; Siles, L.; Miranda, P.; Kakimoto, F.; Tsuchimoto, I.; Inoue, N.; Suga, K.

    1985-01-01

    Energetic 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.

  2. A New Approach to Mass Measurements of UHECR: Horizontal Air Showers

    OpenAIRE

    Zas, Enrique

    2000-01-01

    The role of Horizontal Showers induced by cosmic rays is discussed in detail. A new approach to the calculation of the muon component in horizontal air showers induced by protons, heavier nuclei or photons is presented which allows a simple analytical evaluation of the muon density profiles at ground level. The results of the first application of these results to horizontal air showers detected at the Haverah Park Array by the recently started {\\sl Leeds-Santiago collaboration}, leading to im...

  3. Air shower simulation and hadronic interactions

    Directory of Open Access Journals (Sweden)

    Ulrich Ralf

    2013-06-01

    Full Text Available The aim of this report of the Working Group on Hadronic Interactions and Air Shower Simulation is to give an overview of the status of the field, emphasizing open questions and a comparison of relevant results of the different experiments. It is shown that an approximate overall understanding of extensive air showers and the corresponding hadronic interactions has been reached. The simulations provide a qualitative description of the bulk of the air shower observables. Discrepancies are however found when the correlation between measurements of the longitudinal shower profile are compared to that of the lateral particle distributions at ground. The report concludes with a list of important problems that should be addressed to make progress in understanding hadronic interactions and, hence, improve the reliability of air shower simulations.

  4. Microwave detection of air showers with MIDAS

    Energy Technology Data Exchange (ETDEWEB)

    Facal San Luis, P., E-mail: facal@kicp.uchicago.edu [University of Chicago, Enrico Fermi Institue and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Alekotte, I. [Centro Atomico Bariloche and Instituto Balseiro (CNEA-UNCuyo-CONICET), 8400 San Carlos de Bariloche, Rio Negro (Argentina); Alvarez, J. [Universidad de Santiago de Compostela, Departamento de Fisica de Particulas, Campus Sur, E-15782 Santiago de Compostela (Spain); Berlin, A. [University of Chicago, Enrico Fermi Institue and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Bertou, X. [Centro Atomico Bariloche and Instituto Balseiro (CNEA-UNCuyo-CONICET), 8400 San Carlos de Bariloche, Rio Negro (Argentina); Bogdan, M.; Bohacova, M. [University of Chicago, Enrico Fermi Institue and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Bonifazi, C. [Univ. Federal do Rio de Janeiro (UFRJ), Instituto de Fisica, Cidade Universitaria, Caixa Postal 68528, 21945-970 Rio de Janeiro, RJ (Brazil); Carvalho, W.R. [Universidad de Santiago de Compostela, Departamento de Fisica de Particulas, Campus Sur, E-15782 Santiago de Compostela (Spain); Mello Neto, J.R.T. de [Univ. Federal do Rio de Janeiro (UFRJ), Instituto de Fisica, Cidade Universitaria, Caixa Postal 68528, 21945-970 Rio de Janeiro, RJ (Brazil); Genat, J.F.; Mills, E.; Monasor, M.; Privitera, P.; Reyes, I.C.; Rouille d& #x27; Orfeuil, B. [University of Chicago, Enrico Fermi Institue and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); and others

    2012-01-11

    MIDAS (MIcrowave Detector of Air Showers) is a prototype of a microwave telescope to detect extensive air showers: it images a 20{sup Degree-Sign } Multiplication-Sign 10{sup Degree-Sign} region of the sky with a 4.5 m parabolic reflector and 53 feeds in the focal plane. It has been commissioned in March 2010 and is currently taking data. We present the design, performance and first results of MIDAS.

  5. Microwave detection of air showers with MIDAS

    Science.gov (United States)

    Facal San Luis, P.; Alekotte, I.; Alvarez, J.; Berlin, A.; Bertou, X.; Bogdan, M.; Bohacova, M.; Bonifazi, C.; Carvalho, W. R.; de Mello Neto, J. R. T.; Genat, J. F.; Mills, E.; Monasor, M.; Privitera, P.; Reyes, I. C.; Rouille D'Orfeuil, B.; Santos, E. M.; Wayne, S.; Williams, C.; Zas, E.

    2012-01-01

    MIDAS (MIcrowave Detector of Air Showers) is a prototype of a microwave telescope to detect extensive air showers: it images a 20°×10° region of the sky with a 4.5 m parabolic reflector and 53 feeds in the focal plane. It has been commissioned in March 2010 and is currently taking data. We present the design, performance and first results of MIDAS.

  6. Microwave detection of air showers with MIDAS

    International Nuclear Information System (INIS)

    MIDAS (MIcrowave Detector of Air Showers) is a prototype of a microwave telescope to detect extensive air showers: it images a 20°×10° region of the sky with a 4.5 m parabolic reflector and 53 feeds in the focal plane. It has been commissioned in March 2010 and is currently taking data. We present the design, performance and first results of MIDAS.

  7. Cosmic ray air showers from sphalerons

    CERN Document Server

    Brooijmans, Gustaaf; Spannowsky, Michael

    2016-01-01

    The discovery of the Higgs boson marks a key ingredient to establish the electroweak structure of the Standard Model. Its non-abelian gauge structure gives rise to, yet unobserved, non-perturbative baryon and lepton number violating processes. We propose to use cosmic ray air showers, as measured at the Pierre Auger Observatory, to set a limit on the hadronic production cross section of sphalerons. We identify several observables to discriminate between sphaleron and QCD induced air showers.

  8. Lateral distribution of electrons of air showers

    Science.gov (United States)

    Asakimori, K.; Maeda, T.; Kameda, T.; Mizushima, K.; Misaki, Y.

    1985-01-01

    The lateral distribution of electrons (LDE) of the air showers of size 10 to the 5th power to 10 to the 6th power was studied within one MU. It was found that the LDE of the air showers observed is well represented by NKG function except for vicinity of the core. It was also found that LDE measured by thin scintillators does not differ from that measured by thick ones of 50mm thickness.

  9. High energy interactions and extensive air showers

    International Nuclear Information System (INIS)

    We report on papers presented in the high energy sessions of the conference that do not deal with the theory and observations of muons and neutrinos. We concentrate on the development and testing of hadronic interaction models, their extension to ultrahigh energy and their importance for the analysis and interpretation of air shower data. We also summarize data on the cosmic ray spectrum and composition obtained with air showers

  10. First Experimental Characterization of Microwave Emission from Cosmic Ray Air Showers.

    Science.gov (United States)

    Smída, R; Werner, F; Engel, R; Arteaga-Velázquez, J C; Bekk, K; Bertaina, M; Blümer, J; Bozdog, H; Brancus, I M; Chiavassa, A; Cossavella, F; Di Pierro, F; Doll, P; Fuchs, B; Fuhrmann, D; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Huber, D; Huege, T; Kampert, K-H; Kang, D; Klages, H; Kleifges, M; Krömer, O; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Mathys, S; Mayer, H J; Melissas, M; Morello, C; Neunteufel, P; Oehlschläger, J; Palmieri, N; Pekala, J; Pierog, T; Rautenberg, J; Rebel, H; Riegel, M; Roth, M; Salamida, F; Schieler, H; Schoo, S; Schröder, F G; Sima, O; Stasielak, J; Toma, G; Trinchero, G C; Unger, M; Weber, M; Weindl, A; Wilczyński, H; Will, M; Wochele, J; Zabierowski, J

    2014-11-28

    We report the first direct measurement of the overall characteristics of microwave radio emission from extensive air showers. Using a trigger provided by the KASCADE-Grande air shower array, the signals of the microwave antennas of the Cosmic-Ray Observation via Microwave Emission experiment have been read out and searched for signatures of radio emission by high-energy air showers in the GHz frequency range. Microwave signals have been detected for more than 30 showers with energies above 3×10^{16}  eV. The observations presented in this Letter are consistent with a mainly forward-directed and polarized emission process in the GHz frequency range. The measurements show that microwave radiation offers a new means of studying air showers at E≥10^{17}  eV. PMID:25494064

  11. First Experimental Characterization of Microwave Emission from Cosmic Ray Air Showers

    CERN Document Server

    Smida, R; Engel, R; Arteaga-Velazquez, J C; Bekk, K; Bertaina, M; Bluemer, J; Bozdog, H; Brancus, I M; Chiavassa, A; Cossavella, F; Di Pierro, F; Doll, P; Fuchs, B; Fuhrmann, D; Grupen, C; Haungs, A; Heck, D; Hoerandel, J R; Huber, D; Huege, T; Kampert, K -H; Kang, D; Klages, H; Kleifges, M; Kroemer, O; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Mathys, S; Mayer, H J; Melissas, M; Morello, C; Neunteufel, P; Oehlschlaeger, J; Palmieri, N; Pekala, J; Pierog, T; Rautenberg, J; Rebel, H; Riegel, M; Roth, M; Salamida, F; Schieler, H; Schoo, S; Schroeder, F G; Sima, O; Stasielak, J; Toma, G; Trinchero, G C; Unger, M; Weber, M; Weindl, A; Wilczynski, H; Will, M; Wochele, J; Zabierowski, J

    2014-01-01

    We report the first direct measurement of the overall characteristics of microwave radio emission from extensive air showers. Using a trigger provided by the KASCADE-Grande air shower array, the signals of the microwave antennas of the CROME (Cosmic-Ray Observation via Microwave Emission) experiment have been read out and searched for signatures of radio emission by high-energy air showers in the GHz frequency range. Microwave signals have been detected for more than 30 showers with energies above 3*10^16 eV. The observations presented in this Letter are consistent with a mainly forward-directed and polarised emission process in the GHz frequency range. The measurements show that microwave radiation offers a new means of studying air showers at energies above 10^17 eV.

  12. First Upper Limits on the Radar Cross Section of Cosmic-Ray Induced Extensive Air Showers

    CERN Document Server

    Abbasi, R U; Othman, M Abou Bakr; Abu-Zayyad, T; Allen, M; Anderson, R; Azuma, R; Barcikowski, E; Belz, J W; Bergman, D R; Besson, D; Blake, S A; Byrne, M; Cady, R; Chae, M J; Cheon, B G; Chiba, J; Chikawa, M; Cho, W R; Farhang-Boroujeny, B; Fujii, T; Fukushima, M; Gillman, W H; Goto, T; Hanlon, W; Hanson, J C; Hayashi, Y; Hayashida, N; Hibino, K; Honda, K; Ikeda, D; Inoue, N; Ishii, T; Ishimori, R; Ito, H; Ivanov, D; Jayanthmurthy, C; Jui, C C H; Kadota, K; Kakimoto, F; Kalashev, O; Kasahara, K; Kawai, H; Kawakami, S; Kawana, S; Kawata, K; Kido, E; Kim, H B; Kim, J H; Kitamura, S; Kitamura, Y; Kunwar, S; Kuzmin, V; Kwon, Y J; Lan, J; Lim, S I; Lundquist, J P; Machida, K; Martens, K; Matsuda, T; Matsuyama, T; Matthews, J N; Minamino, M; Mukai, K; Myers, I; Nagasawa, K; Nagataki, S; Nakamura, T; Nonaka, T; Nozato, A; Ogio, S; Ogura, J; Ohnishi, M; Ohoka, H; Oki, K; Okuda, T; Ono, M; Oshima, A; Ozawa, S; Park, I H; Prohira, S; Pshirkov, M S; Rezazadeh-Reyhani, A; Rodriguez, D C; Rubtsov, G; Ryu, D; Sagawa, H; Sakurai, N; Sampson, A L; Scott, L M; Schurig, D; Shah, P D; Shibata, F; Shibata, T; Shimodaira, H; Shin, B K; Smith, J D; Sokolsky, P; Springer, R W; Stokes, B T; Stratton, S R; Stroman, T A; Suzawa, T; Takai, H; Takamura, M; Takeda, M; Takeishi, R; Taketa, A; Takita, M; Tameda, Y; Tanaka, H; Tanaka, K; Tanaka, M; Thomas, S B; Thomson, G B; Tinyakov, P; Tkachev, I; Tokuno, H; Tomida, T; Troitsky, S; Tsunesada, Y; Tsutsumi, K; Uchihori, Y; Udo, S; Urban, F; Vasiloff, G; Venkatesh, S; Wong, T; Yamane, R; Yamaoka, H; Yamazaki, K; Yang, J; Yashiro, K; Yoneda, Y; Yoshida, S; Yoshii, H; Zollinger, R; Zundel, Z

    2016-01-01

    TARA (Telescope Array Radar) is a cosmic ray radar detection experiment colocated with Telescope Array, the conventional surface scintillation detector (SD) and fluorescence telescope detector (FD) near Delta, Utah, U.S.A. The TARA detector combines a 40 kW, 54.1 MHz VHF transmitter and high-gain transmitting antenna which broadcasts the radar carrier over the SD array and within the FD field of view, towards a 250 MS/s DAQ receiver. TARA has been collecting data since 2013 with the primary goal of observing the radar signatures of extensive air showers (EAS). Simulations indicate that echoes are expected to be short in duration (~10 microseconds) and exhibit rapidly changing frequency, with rates on the order of 1 MHz/microsecond. The EAS radar cross-section (RCS) is currently unknown although it is the subject of over 70 years of speculation. A novel signal search technique is described in which the expected radar echo of a particular air shower is used as a matched filter template and compared to waveforms...

  13. The radio signal from extensive air showers

    CERN Document Server

    Revenu, Benoît

    2014-01-01

    The field of ultra-high energy cosmic rays made a lot of progresses last years with large area experiments such as the Pierre Auger Observatory, HiRes and the Telescope Array. A suppression of the cosmic ray flux at energies above $5.5x10^{19}$ eV is observed at a very high level of significance but the origin of this cut-off is not established: it can be due to the Greisen-Zatsepin-Kuzmin suppression but it can also reflect the upper limit of particle acceleration in astrophysical objects. The key characteristics to be measured on cosmic rays is their composition. Upper limits are set above $10^{18}$ eV on primary photons and neutrinos and primary cosmic rays are expected to be hadrons. Identifying the precise composition (light or heavy nuclei) will permit to solve the puzzle. It has been proven that the radio signal emitted by the extensive air showers initiated by ultra-high energy cosmic rays reflects their longitudinal profile and can help in constraining the primary particle. We review in this paper th...

  14. Modelling geo-magnetic radiation from extensive air showers

    International Nuclear Information System (INIS)

    An incoming ultra high energy cosmic ray (UHECR) entering our atmosphere will create a so called extensive air shower (EAS). A cascade of particles flying toward the Earth's surface with extremely high velocities. As a result of this they are concentrated in a thin shower front, which can be visualized by a pancake of particles flying toward the Earth. The deflection of electrons and positrons due to the Earth magnetic field in combination with retardation effects is responsible for an electromagnetic pulse to be emitted within the radio frequency range. Concentrating on a macroscopic description, focussing on the net current created due to the deflection of the electrons and positrons in the Earth magnetic field, a model has been made to simulate the radio signal for a realistic air shower. Several different contributions to the electric pulse have been included to obtain more realistic simulations and have a better comparison with measured data.

  15. First detection of extensive air showers with the EEE experiment

    CERN Document Server

    Abbrescia, M; Fabbri, F L; Bressan, E; Librizzi, F; Sartorelli, G; Piragino, G; Ferroli, R Baldini; Maggiora, A; Siddi, E; Zuyeuski, R; Frolov, V; Serci, S; Selvi, M; Zichichi, A; Romano, F; La Rocca, P; Williams, M C S; Cicalo, C; D'Incecco, M; Panareo, M; Menghetti, H; Garbini, M; Moro, R; Cifarelli, L; Riggi, F; Hatzifotiadou, D; Scapparone, E; Chiavassa, A; Gustavino, C; De Gruttola, D; Coccetti, F; Bencivenni, C; Miozzi, S; De Pasquale, S

    2010-01-01

    The Extreme Energy Events (EEE) Project is devoted to the study of extremely high energy cosmic rays by means of an array of particle detectors distributed all over the Italian territory. Each element of the array (called telescope in the following) is installed in a High School, with the further goal to introduce students to particle and astroparticle physics, and consists of three Multigap Resistive Plate Chambers (MRPC), that have excellent time resolution and good tracking capability. In this paper the first results on the detection of extensive air showers by means of time coincidences between two telescopes are presented.

  16. Precision measurements of cosmic ray air showers

    CERN Document Server

    Huege, T; Buitink, S; Dallier, R; Ekers, R D; Falcke, H; James, C W; Martin, L; Revenu, B; Scholten, O; Schröder, F G

    2014-01-01

    Supplemented with suitable buffering techniques, the low-frequency part of the SKA can be used as an ultra-precise detector for cosmic-ray air showers at very high energies. This would enable a wealth of scientific applications: the physics of the transition from Galactic to extragalactic cosmic rays could be probed with very high precision mass measurements, hadronic interactions could be studied up to energies well beyond the reach of man-made particle accelerators, air shower tomography could be performed with very high spatial resolution exploiting the large instantaneous bandwidth and very uniform instantaneous $u$-$v$ coverage of SKA1-LOW, and the physics of thunderstorms and possible connections between cosmic rays and lightning initiation could be studied in unprecedented levels of detail. In this article, we describe the potential of SKA as an air shower radio detector from the perspective of existing radio detection efforts and discuss the associated technical requirements.

  17. Hadronic interaction models and air shower simulations

    International Nuclear Information System (INIS)

    Extensive air showers can only be interpreted by comparison of the measured observables with simulations, using a suitable model for the shower development in the atmosphere. Due to the complexity of the phenomenon, in the past the models were quite simple and results from air showers were to interpret qualitatively, at best. With a new generation of experiments more advanced detectors became operational and the need for detailed simulations grew. In recent years several new air shower programs were developed. Using the rapid increase of the computing power they have now reached a high level of sophistication. Particle transport, electromagnetic interactions and decay of unstable particles are treated in great detail. However the most crucial ingredient to all these programs is the modeling of hadronic interactions since it requires extrapolation in energy, primary mass and kinematics to regions where no accelerator data exist and where theoretical guidelines are only vague. As a consequence of the model uncertainties, experiments using different models occasionally reached very different conclusions on energy spectra and composition of the cosmic rays. CORSIKA is an extensive air shower simulation program that contains five different hadronic interaction models (VENUS, QGSJET, SIBYLL, HDPM, and DPMJET). It is widely used throughout the cosmic ray community and allows the study of model dependencies and the systematic effects of measurement and event reconstruction. Results for different models concerning inelastic cross-sections and particle production and their influence on air shower variables are discussed and the systematic uncertainties for air shower analyses are investigated. The capability of precise multi-parameter measurements to discriminate between the models is emphasised

  18. Supervision of double extensive air showers

    International Nuclear Information System (INIS)

    Double extensive air showers were investigated at Tien-Shan high mountain scientific station of P.N. Lebedev Institute by means of two various installations. One installation registered electron-photon air shower component, another – Vavilov-Cherenkov radiation. On both installations the double showers divided by a time interval of ∼100 nanoseconds have been registered. In the present work frequency of occurrence of such showers in each of installations is analysed, and is shown that at supervision of vertical showers (zenith angle θ <60°) these frequencies coincide.

  19. Lateral distribution of electrons in air showers

    International Nuclear Information System (INIS)

    We investigate the lateral distribution of electrons in extensive air showers generated by 105/109 GeV protons. It was found that the lateral distribution function in extensive air showers contains the same invariant part as the one in a pure electromagnetic cascade. This scaling property is poorly sensitive to the variation of basic parameters of the hadron-nucleus interactions model. We also report on some initial results obtained for the description of the transition effect of shower particles within scintillators of different thickness

  20. Coherent radiation from extensive air showers

    International Nuclear Information System (INIS)

    The generic properties of the emission of coherent radiation from a moving charge distribution are discussed. The general structure of the charge and current distributions in an extensive air shower are derived. These are subsequently used to develop a very intuitive picture for the properties of the emitted radio pulse. Using this picture can be seen that the structure of the pulse is a direct reflection of the shower profile. At higher frequencies the emission is suppressed because the wavelength is shorter than the important length scale in the shower. It is shown that radio emission can be used to distinguish proton- and iron-induced air showers.

  1. A branching model for hadronic air showers

    CERN Document Server

    Novotny, Vladimir; Ebr, Jan

    2015-01-01

    We introduce a simple branching model for the development of hadronic showers in the Earth's atmosphere. Based on this model, we show how the size of the pionic component followed by muons can be estimated. Several aspects of the subsequent muonic component are also discussed. We focus on the energy evolution of the muon production depth. We also estimate the impact of the primary particle mass on the size of the hadronic component. Even though a precise calculation of the development of air showers must be left to complex Monte Carlo simulations, the proposed model can reveal qualitative insight into the air shower physics.

  2. Application of an image intensifier to the study on hadrons in air shower, 4

    International Nuclear Information System (INIS)

    As the apparatus for observing cosmic ray air shower, the particle detection apparatus combining spark chamber, scintillator and photomultiplier tube is frequently used, but the exact detection of particle number is impossible with it when particle density is large. The authors have carried out the experiment to measure nuclear active particles in air shower and to grasp the central part of air shower as energy flow by utilizing an image intensifier tube. On the roof of building S, a laboratory was built, and a core detector of 2 m x 2 m area, 13 AS detectors of 0.25 m2 and an AS detector of 1 m2 were installed. The gate of the II was opened by utilizing coincidence pulses, and the position and amount of scintillation in the core detector was taken into a camera through the II. The time of observation was 289 hours, and the time of II operation was 113 hours. Total number of air shower recorded was 218 cases, and the centers of 120 cases among them were determined in the AS detectors at four corners. The centers of 39 cases were within the area of the core detector. In the coincident counting of air shower and burst carried out in the present experiment, the total delay time from the arrival of air shower to the gate pulse actuating the II was 1.6 sec. The core of air shower of about 106 size and 1.3 age was caught by this method. The problems for future are the determination of core position for the air shower of smaller size, and the meaning of spot images of II. (Kako, I.)

  3. Fluorescence Detection of Cosmic Ray Air Showers Between 1016.5 and 1018.5 eV with the Telescope Array Low Energy Extension (TALE)

    Science.gov (United States)

    Zundel, Zachary

    The Telescope Array (TA) Collaboration has completed construction of a low-energy extension to its Middle Drum telescope station. Ten new telescopes were added observing 32-59 degrees in elevation above the original telescopes. A graded array of scintillator detectors (SDs) with spacings of 400-600-1200 m is being installed in front of the telescope station. With these upgrades, the physics threshold will be lowered below 1016.5 eV. The TA Low Energy Extension (TALE) will explore the regime corresponding to the LHC center-of-mass energy. This is also the region where the transition from galactic to extra-galactic cosmic ray flux is suspected to occur. A brief overview of the physics is presented as well as a report on the progress toward measuring the cosmic ray spectrum between 1016.5 and 1018.5 eV.

  4. Search for bursts in air shower data

    Science.gov (United States)

    Bruce, T. E. G.; Clay, R. W.; Dawson, B. R.; Protheroe, R. J.; Blair, D. G.; Cinquini, P.

    1985-01-01

    There have been reports in recent years of the possible observation of bursts in air shower data. If such events are truly of an astrophysical nature then, they represent an important new class of phemonenon since no other bursts have been observed above the MeV level. The spectra of conventional gamma ray bursts are unknown at higher energies but their observed spectra at MeV energies appear generally to exhibit a steepening in the higher MeV range and are thus unlikely to extrapolate to measurable fluxes at air shower energies. An attempt has been made to look for deviations from randomness in the arrival times of air showers above approx. 10 to the 14th power eV with a number of systems and results so far are presented here. This work will be continued for a substantial period of ime with a system capable of recording bursts with multiple events down to a spacing of 4 microns. Earlier data have also been searched for the possible association of air shower events with a glitch of the Vela pulsar.

  5. Precision measurements of cosmic ray air showers

    NARCIS (Netherlands)

    Huege, T.; Bray, J. D.; Buitink, S.; Dallier, R.; Ekers, R. D.; Falcke, H.; James, C. W.; Martin, L.; Revenu, B.; Scholten, O.; Schröder, F. G.

    2014-01-01

    Supplemented with suitable buffering techniques, the low-frequency part of the SKA can be used as an ultra-precise detector for cosmic-ray air showers at very high energies. This would enable a wealth of scientific applications: the physics of the transition from Galactic to extragalactic cosmic ray

  6. Cosmic ray air showers in the knee energy region

    Indian Academy of Sciences (India)

    S Sanyal

    2003-03-01

    The cosmic ray extensive air showers in the knee energy region have been studied by the North Bengal University array. The differential size spectra at different atmospheric depths show a systematic shift of the knee towards smaller shower size with the increase in atmospheric depth. The measured values of spectral indices at below and above the knee are -2.45± 0.03 and -2.91± 0.05 respectively. Measurements at different atmospheric depths correspond to the same values within the error limits both for below and above the knee. The present experimental results have been compared with similar such experiments.

  7. Muons in Air Showers at the Pierre Auger Observatory

    Science.gov (United States)

    Unger, M.

    We present measurements of muons in air showers at ultra-high energies with the Pierre Auger Observatory. The number of muons at the ground in air showers detected at large zenith angles is determined as a function of energy and the results are compared to air shower simulations. Furthermore, using data collected at zenith angles smaller than 60°, rescaling factors are derived that quantify the deficit of muon production in air shower simulations.

  8. Photomultiplier tube selection for the Wide Field of view Cherenkov/fluorescence Telescope Array of the Large High Altitude Air Shower Observatory

    Science.gov (United States)

    Ge, Maomao; Zhang, Li; Chen, Yingtao; Cao, Zhen; Zhang, Shoushan; Wang, Chong; Bi, Baiyang

    2016-05-01

    For the purpose of selecting the most suitable photomultiplier tubes (PMTs) for the Wide Field of view Cherenkov/fluorescence Telescope Array (WFCTA), we have performed extensive tests on seven models of 25.4 mm PMTs: Hamamatsu R1924A and R7899, Beijing Hamamatsu CR303, CR332A and CR364, and HZC Photonics XP3102 and XP3182. A dedicated test system has been developed to measure the PMT characteristics such as single photo-electron spectrum, gain, linearity, and spatial uniformity of anode output. The XP3182 and CR364 (R7899) tubes both meet the pivotal requirement due to their superior pulse linearity. The PMT test system, techniques used for these measurements, and their results are also reported.

  9. Upgrading and testing the 3D reconstruction of gamma-ray air showers as observed with an array of Imaging Atmospheric Cherenkov telescopes

    CERN Document Server

    Naumann-Godó, M; Degrange, B

    2009-01-01

    Stereoscopic arrays of Imaging Atmospheric Cherenkov Telescopes allow to reconstruct gamma-ray-induced showers in 3 dimensions, which offers several advantages: direct access to the shower parameters in space and straightforward calorimetric measurement of the incident energy. In addition, correlations between the different images of the same shower are taken into account. An analysis method based on a simple 3D-model of electromagnetic showers was recently implemented in the framework of the H.E.S.S. experiment. In the present article, the method is completed by an additional quality criterion, which reduces the background contamination by a factor of about 2 in the case of extended sources, while keeping gamma-ray efficiency at a high level. On the other hand, the dramatic flares of the blazar PKS 2155-304 in July 2006, which provided H.E.S.S. data with an almost pure gamma-ray sample, offered the unique opportunity of a precision test of the 3D-reconstruction method as well as of the H.E.S.S. simulations u...

  10. Thickness of the particle swarm in cosmic ray air showers

    Science.gov (United States)

    Linsley, J.

    1985-01-01

    The average dispersion in arrival time of air shower particles detected with a scintillator at an impact parameter r is described with accuracy 5-10% by the empirical formula sigma = Sigma sub to (1+r/r sub t) sup b, where Sigma sub to = 2.6 ns, r sub t = 30m and b = (1.94 + or - .08) (0.39 + or - .06) sec Theta, for r 2 km, 10 to the 8th power E 10 to the 11th power GeV, and Theta 60 deg. (E is the primary energy and theta is the zenith angle). The amount of fluctuation in sigma sub t due to fluctuations in the level of origin and shower development is less than 20%. These results provide a basis for estimating the impact parameters of very larger showers with data from very small detector arrays (mini-arrays). The energy of such showers can then be estimated from the local particle density. The formula also provides a basis for estimating the angular resolution of air shower array-telescopes.

  11. The Chicago Air Shower Array (CASA)

    International Nuclear Information System (INIS)

    In order to improve the ultrahigh energy flux sensitivity beyond that of existing detectors a new class of very large detectors must be built. In this paper we will discuss one approach to this goal. (orig.)

  12. Character of energy flow in air shower core

    Science.gov (United States)

    Mizushima, K.; Asakimori, K.; Maeda, T.; Kameda, T.; Misaki, Y.

    1985-01-01

    Energy per charged particle near the core of air showers was measured by 9 energy flow detectors, which were the combination of Cerenkov counters and scintillators. Energy per particle of each detector was normalized to energy at 2m from the core. The following results were obtained as to the energy flow: (1) integral frequency distribution of mean energy per particle (averaged over 9 detectors) is composed of two groups separated distinctly; and (2) showers contained in one group show an anisotropy of arrival direction.

  13. A phenomenological model of the muon density profile on the ground of very inclined air showers

    OpenAIRE

    Dembinski, Hans; Billoir, Pierre; Deligny, Olivier; Hebbeker, Thomas

    2009-01-01

    Ultra-high energy cosmic rays generate extensive air showers in Earth's atmosphere. A standard approach to reconstruct the energy of an ultra-high energy cosmic rays is to sample the lateral profile of the particle density on the ground of the air shower with an array of surface detectors. For cosmic rays with large inclinations, this reconstruction is based on a model of the lateral profile of the muon density observed on the ground, which is fitted to the observed muon densities in individu...

  14. Detection and analysis of radio pulses from extensive air showers

    International Nuclear Information System (INIS)

    Radio pulses from extensive air showers(EAS) at 30, 44 and 60 MHz frequencies have been studied, using wide band broad-side arrays of half-wave dipole antenna systems. The experimental results support the theoretical prediction that the field strength of radioemission depends on the shower size. An asymmetry has been noticed in the pulse height distributions of radio pulses detected by North-South and East-West directed arrays. These observations are in agreement with the theory that the charge separation mechanism is predominant in generating radio pulses from EAS and radio emission is polarised in the East-West direction. Experimental data are compared with those of earlier workers. (author)

  15. Status of the large high altitude air shower observatory project

    International Nuclear Information System (INIS)

    The Large High Altitude Air Shower Observatory (LHAASO) project is a multipurpose project. The main scientific tasks can be summarized as follows: (1) searching for galactic cosmic ray origins through gamma ray source detection above 30 TeV; (2) wide field of view survey for gamma ray sources at energies higher than 100 GeV; (3) energy spectrum measurements for individual cosmic ray species from 30 TeV to 10 PeV. To target above tasks, a complex detector array is designed. This paper describes the progress on the research and development of all kind of detectors. Construction and operation of a prototype detector array at Tibet site with 4300 m a.s.l. are also presented.

  16. Computer simulation and experimental development of an air shower core detector

    International Nuclear Information System (INIS)

    In order to check the hadronic interaction models in the forward region at primary energies of above 10 TeV, a detailed computer simulation and an experimental development of the Yangbajing Air shower Core detector array (YAC) is described. YAC, consisting of 124 detectors for which 100 are arranged into 10 × 10 grid and 24 are surrounded, will be operated together with the Tibet-ASgamma Extensive Air Shower array (Tibet-Ⅲ). By using the hybrid experiment (Tibet-Ⅲ + YAC), the high energy electromagnetic particles in the core region of air showers with primary energies higher than 10 TeV can be recorded. Their number distribution, their energy distribution, their lateral spread distribution and other information, together with the primary energy estimated by the accompanied air shower event recorded by the Tibet-Ⅲ array, can provide important information in checking the interaction models in the corresponding energy region. A sufficient big data sample of about 5.6 × 107 high energy core events in three years observation are expected by the hybrid experiment. (authors)

  17. Simulation of Radiation Energy Release in Air Showers

    OpenAIRE

    Glaser, Christian; Erdmann, Martin; Hörandel, Jörg R.; Huege, Tim; Schulz, Johannes

    2016-01-01

    A simulation study of the energy released by extensive air showers in the form of MHz radiation is performed using the CoREAS simulation code. We develop an efficient method to extract this radiation energy from air-shower simulations. We determine the longitudinal profile of the radiation energy release and compare it to the longitudinal profile of the energy deposit by the electromagnetic component of the air shower. We find that the radiation energy corrected for the geometric dependence o...

  18. High energy hadrons in extensive air showers

    Science.gov (United States)

    Tonwar, S. C.

    1985-01-01

    Experimental data on the high energy hadronic component in extensive air showers of energies approx. 10 to the 14 to 10 to the 16 eV when compared with expectations from Monte Carlo simulations have shown the observed showers to be deficient in high energy hadrons relative to simulated showers. An attempt is made to understand these anomalous features with more accurate comparison of observations with expectations, taking into account the details of the experimental system. Results obtained from this analysis and their implications for the high energy physics of particle interactions at energy approx. 10 to the 15 eV are presented.

  19. Radar reflection off extensive air showers

    Directory of Open Access Journals (Sweden)

    Werner F.

    2013-06-01

    Full Text Available We investigate the possibility of detecting extensive air showers by the radar technique. Considering a bistatic radar system and different shower geometries, we simulate reflection of radio waves off the static plasma produced by the shower in the air. Using the Thomson cross-section for radio wave reflection, we obtain the time evolution of the signal received by the antennas. The frequency upshift of the radar echo and the power received are studied to verify the feasibility of the radar detection technique.

  20. What can we study through families and accompanied air showers?

    International Nuclear Information System (INIS)

    At mountain altitudes, high energy γ-ray bundles (γ-rays in parallel trajectories and with the same direction of an air shower) can be observed in the central part of air showers. These γ-ray bundles (≥ 1 TeV) and their associated air showers are observed simultaneously at Mt. Chacaltaya (5200 m) by our detectors. The γ-ray bundle in the air shower can give information on the primary composition and the characteristics of proton interaction. In this paper, we report on experimental results, simulations calculated for the present experiments, and also problems in simulations

  1. Observation of time correlation in cosmic air shower network

    International Nuclear Information System (INIS)

    In order to measure time correlation of primary cosmic rays, a network observation of extensive air showers started in Japan. The network as Large Area Air Shower (LAAS) group consists of nine air-shower-stations (seven institutes and 26,000 km2) using the Global Positioning System (GPS). We propose an analytical procedure to extract time-limited fractal structure from time series of arrival time intervals of successive air showers and present the results of the analysis by using the network data

  2. New facts about muon production in Extended Air Shower simulations

    CERN Document Server

    Pierog, T

    2006-01-01

    Whereas air shower simulations are very valuable tools for interpreting cosmic ray data, there is a long standing problem: is seems to be impossible to accommodate at the same time the longitudinal development of air showers and the number of muons measured at ground. Using a new hadronic interaction model (EPOS) in air shower simulations produces considerably more muons, in agreement with results from the HiRes-MIA experiment. We find that this is mainly due to a better description of baryon-antibaryon production in hadronic interactions. This is a new aspect of air shower physics which has never been considered so far.

  3. Cosmic Ray-Air Shower Measurement from Space

    Science.gov (United States)

    Takahashi, Yoshiyuki

    1997-01-01

    A feasibility study has been initiated to observe from space the highest energy cosmic rays above 1021 eV. A satellite observatory concept, the Maximum-energy Auger (Air)-Shower Satellite (MASS), is recently renamed as the Orbital Wide-angle Collector (OWL) by taking its unique feature of using a very wide field-of-view (FOV) optics. A huge array of imaging devices (about 10(exp 6) pixels) is required to detect and record fluorescent light profiles of cosmic ray cascades in the atmosphere. The FOV of MASS could extend to as large as about 60 in. diameter, which views (500 - 1000 km) of earth's surface and more than 300 - 1000 cosmic ray events per year could be observed above 1020 eV. From far above the atmosphere, the MASS/OWL satellite should be capable of observing events at all angles including near horizontal tracks, and would have considerable aperture for high energy photon and neutrino observation. With a large aperture and the spatial and temporal resolution, MASS could determine the energy spectrum, the mass composition, and arrival anisotropy of cosmic rays from 1020 eV to 1022 eV; a region hitherto not explored by ground-based detectors such as the Fly's Eye and air-shower arrays. MASS/OWL's ability to identify cosmic neutrinos and gamma rays may help providing evidence for the theory which attributes the above cut-off cosmic ray flux to the decay of topological defects. Very wide FOV optics system of MASS/OWL with a large array of imaging devices is applicable to observe other atmospheric phenomena including upper atmospheric lightning. The wide FOV MASS optics being developed can also improve ground-based gamma-ray observatories by allowing simultaneous observation of many gamma ray sources located at different constellations.

  4. A parameterization for the radio emission of air showers as predicted by CoREAS simulations and applied to LOFAR measurements

    CERN Document Server

    Nelles, Anna; Falcke, Heino; Hörandel, Jörg; Huege, Tim; Schellart, Pim

    2014-01-01

    Measuring radio emission from air showers provides excellent opportunities to directly measure all air shower properties, including the shower development. To exploit this in large-scale experiments, a simple and analytic parameterization of the distribution of the pulse power at ground level is needed. Data taken with the Low-Frequency Array (LOFAR) show a complex two-dimensional pattern of pulse powers, which is sensitive to the shower geometry. Earlier parameterizations of the lateral signal distribution have proven insufficient to describe these data. In this article, we present a parameterization derived from air-shower simulations. We are able to fit the two-dimensional distribution with a double Gaussian, requiring five independent parameters. All parameters show strong correlations with air shower properties, such as the energy of the shower, the arrival direction, and the shower maximum. We successfully apply the parameterization to data taken with LOFAR and discuss implications for air shower experi...

  5. Extended air showers and muon interactions

    International Nuclear Information System (INIS)

    The objective of this work is to report on the influence of muon interactions on the development of air showers initiated by astroparticles. We make a comparative study of the different theoretical approaches to muon bremsstrahlung and muonic pair production interactions. A detailed algorithm that includes all the relevant characteristics of such processes has been implemented in the AIRES air shower simulation system. We have simulated ultrahigh energy showers in different conditions in order to measure the influence of these muonic electromagnetic interactions. We have found that during the late stages of the shower development (well beyond the shower maximum) many global observables are significantly modified in relative terms when the mentioned interactions are taken into account. This is most evident in the case of the electromagnetic component of very inclined showers. On the other hand, our simulations indicate that the studied processes do not induce significant changes either in the position of the shower maximum or the structure of the shower front surface

  6. A transient digitiser for fast air shower events

    Science.gov (United States)

    Wild, N. R.; Clay, R. W.

    1985-01-01

    Air shower structure are often measured on time scales of a few nanoseconds. Longitudinal disk structure near the core is of the order of meters in dimension, air Cerenkov pulses have full widths at half maximum of the order of tens of nanoseconds, and fast timing over typical arrays is usually measured to nanosecond accuracy. oscilloscopes can be used but have very limited dynamic range and are expensive if measurements down to a few nanoseconds are to be made. For the fast Cerenkov work, an instrument with better dynamic range than an oscilloscope and with a time resolution sufficient to allow measurements limited only by system risetime of a few nanoseconds is needed. A 16/32 channel, 8 bit, fast transient digitizer was designed and built which runs at sample intervals down to approx. 1 nanosecond per channel.

  7. Clock distribution system for large high altitude air shower observatory

    International Nuclear Information System (INIS)

    In this paper, we report a clock distribution system for Water Cherenkov Detector Arrays (WCDAs) in Large High Altitude Air Shower Observatory (LHAASO) project. The designed electronics system is of high performance in implementing the clock distribution among detectors of a large scale of dimension. Based on Serializer/Deserializer (SerDes) and fiber transmission, the clock distribution system is the modules of central back end to distributed front end. The clock distribution system has been evaluated with a two modules system. While all the four SerDes candidates for clock transmission with jitters below 17 ps, the DS92LV16 has a fixed phase relationship between transmission clock and recovered clock, hence its use in LHAASO WCDAs. (authors)

  8. Recent results of KASCADE phenomenology of extensive air showers

    International Nuclear Information System (INIS)

    KASCADE (KArlsruhe Shower Core and Array DEtector) is a multi-detector setup to observe the electromagnetic, muonic and hadronic air shower components simultaneously in the energy region around the 'knee' of the primary spectrum. Its main aim is to determine energy spectrum and composition of hadrons in primary cosmic rays. This is attempted by registering a large number of observables for each EAS including measurements of electrons, muons and hadrons. This contribution gives a short description of the experiment and then presents some results on the lateral distributions of various particle types and on the spectrum of hadrons. The status of our analyses to determine mass composition is presented in an accompanying contribution by A. Haungs

  9. Search for molecular bremsstrahlung radiation signals in Ku band with coincidental operations of radio telescopes with air shower detectors

    Directory of Open Access Journals (Sweden)

    Fukushima Masaki

    2013-06-01

    Full Text Available Microwave radiation from extensive air showers is expected to provide a new technique to observe UHECR. We insatlled and operate radio telescopes in Osaka and at Telescope Array site in Utah, USA. In Osaka, we are coincidentally operating two Ku band radio telescopes with an air shower array which consists of nine plastic scintillators with about 10 m separation. In Utah, we installed two telescopes just beside the Black Rock Mesa fluorescence detector (FD station of the Telescope Array experiment, and we operated the radio telescopes coincidentally with FD event triggers. We report the experimental setups and the results of these measurements.

  10. Measurements and polarization analysis of radio pulses from cosmic-ray-induced air showers at the Pierre Auger Observatory

    International Nuclear Information System (INIS)

    The Auger Engineering Radio Array (AERA) is designed to study the radio emissions from extensive air showers at the Pierre Auger Observatory. The array currently consists of a grid of 23 autonomous radio detector stations that measure the radio emissions from cosmic-ray-induced air showers since April 2011. The array is still under construction and is planned to be extended to 160 stations. The new detection technique provides an augmentation of the existing detectors, improves the sensitivity of the observatory and sheds new light on the shower physics. An analysis of the emission processes based on the polarization of the radio pulses is presented.

  11. Air Shower Events of High-Energy Cosmic Rays Measured at Seoul, South Korea

    Science.gov (United States)

    Cho, Wooram; Shin, Jae-Ik; Kim, Hongki; Lee, Seulgi; Lim, Sunin; Nam, Sinwoo; Yang, Jongmann; Cheon, Byunggu; Bang, Hyungchan; Kwon, Youngjoon

    2011-09-01

    The COsmic ray Research and Education Array (COREA) collaboration has installed an array of six detector stations at two high schools in and near Seoul, Korea for measurement of air-shower events from high-energy cosmic rays. Three stations are installed at each site, where each station consists of four plastic scintillation detectors covering an area of 2m2. In this presentation, we report the currenst status of the COREA project, describing the experimental equipment and measurement of coincident events.

  12. The hadronic component of extensive air showers and the hypothesis about high transverse momenta

    International Nuclear Information System (INIS)

    The hadronic component in air showers of size Nsub(e) >= 105 has been investigated at Tian-Shan complex array. This array allows to obtain reliable data on lateral and energetic characteristics of hadrons of energies Esub(h) >= 1 TeV. These data are in agreement with the hypothesis about an increasing of transverse momenta at ultra-high energy interactions. (orig.)

  13. Radio emission from cosmic ray air showers : Monte Carlo simulations

    NARCIS (Netherlands)

    Huege, T.; Falcke, H.D.E.

    2005-01-01

    We present time-domain Monte Carlo simulations of radio emission from cosmic ray air showers in the scheme of coherent geosynchrotron radiation. Our model takes into account the important air shower characteristics such as the lateral and longitudinal particle distributions, the particle track lengt

  14. Hadronic multiparticle production in extensive air showers and accelerator experiments

    OpenAIRE

    Meurer, Christine; Blümer, Johannes; Engel, Ralph; Haungs, Andreas; Roth, Markus

    2005-01-01

    Using CORSIKA for simulating extensive air showers, we study the relation between the shower characteristics and features of hadronic multiparticle production at low energies. We report about investigations of typical energies and phase space regions of secondary particles which are important for muon production in extensive air showers. Possibilities to measure relevant quantities of hadron production in existing and planned accelerator experiments are discussed.

  15. Calibrating the absolute amplitude scale for air showers measured at LOFAR

    International Nuclear Information System (INIS)

    Air showers induced by cosmic rays create nanosecond pulses detectable at radio frequencies. These pulses have been measured successfully in the past few years at the LOw-Frequency ARray (LOFAR) and are used to study the properties of cosmic rays. For a complete understanding of this phenomenon and the underlying physical processes, an absolute calibration of the detecting antenna system is needed. We present three approaches that were used to check and improve the antenna model of LOFAR and to provide an absolute calibration of the whole system for air shower measurements. Two methods are based on calibrated reference sources and one on a calibration approach using the diffuse radio emission of the Galaxy, optimized for short data-sets. An accuracy of 19% in amplitude is reached. The absolute calibration is also compared to predictions from air shower simulations. These results are used to set an absolute energy scale for air shower measurements and can be used as a basis for an absolute scale for the measurement of astronomical transients with LOFAR

  16. Radio detection of extensive air showers at the Pierre Auger Observatory

    International Nuclear Information System (INIS)

    The Pierre Auger Observatory explores the potential of radio-detection techniques to measure extensive air showers (EAS) induced by ultra-high energy cosmic rays. To study in detail the mechanisms responsible for radio emission in the MHz range, the Auger Engineering Radio Array has been installed at the Observatory. Presently consisting of 24 radio-detection stations, this number will grow to 150 units covering an area of almost 20 km2. Novel detection techniques based on the GHz emission from the EAS are currently being studied. AMBER (Air-shower Microwave Bremsstrahlung Experimental Radiometer) and MIDAS (Microwave Detection of Air Showers) are prototypes for a large imaging dish antenna. In EASIER (Extensive Air Shower Identification using Electron Radiometer), the microwave emission is detected by antenna horns located on each surface detector. MIDAS is a self-triggering system while AMBER and EASIER use the trigger from the Auger detectors to record the emission. The status of these radio-detection R and D efforts at the Pierre Auger Observatory will be reported

  17. Calibrating the absolute amplitude scale for air showers measured at LOFAR

    Science.gov (United States)

    Nelles, A.; Hörandel, J. R.; Karskens, T.; Krause, M.; Buitink, S.; Corstanje, A.; Enriquez, J. E.; Erdmann, M.; Falcke, H.; Haungs, A.; Hiller, R.; Huege, T.; Krause, R.; Link, K.; Norden, M. J.; Rachen, J. P.; Rossetto, L.; Schellart, P.; Scholten, O.; Schröder, F. G.; ter Veen, S.; Thoudam, S.; Trinh, T. N. G.; Weidenhaupt, K.; Wijnholds, S. J.; Anderson, J.; Bähren, L.; Bell, M. E.; Bentum, M. J.; Best, P.; Bonafede, A.; Bregman, J.; Brouw, W. N.; Brüggen, M.; Butcher, H. R.; Carbone, D.; Ciardi, B.; de Gasperin, F.; Duscha, S.; Eislöffel, J.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; van Haarlem, M. P.; Heald, G.; Hoeft, M.; Horneffer, A.; Iacobelli, M.; Juette, E.; Karastergiou, A.; Kohler, J.; Kondratiev, V. I.; Kuniyoshi, M.; Kuper, G.; van Leeuwen, J.; Maat, P.; McFadden, R.; McKay-Bukowski, D.; Orru, E.; Paas, H.; Pandey-Pommier, M.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Reich, W.; Röttgering, H.; Schwarz, D.; Serylak, M.; Sluman, J.; Smirnov, O.; Tasse, C.; Toribio, M. C.; Vermeulen, R.; van Weeren, R. J.; Wijers, R. A. M. J.; Wucknitz, O.; Zarka, P.

    2015-11-01

    Air showers induced by cosmic rays create nanosecond pulses detectable at radio frequencies. These pulses have been measured successfully in the past few years at the LOw-Frequency ARray (LOFAR) and are used to study the properties of cosmic rays. For a complete understanding of this phenomenon and the underlying physical processes, an absolute calibration of the detecting antenna system is needed. We present three approaches that were used to check and improve the antenna model of LOFAR and to provide an absolute calibration of the whole system for air shower measurements. Two methods are based on calibrated reference sources and one on a calibration approach using the diffuse radio emission of the Galaxy, optimized for short data-sets. An accuracy of 19% in amplitude is reached. The absolute calibration is also compared to predictions from air shower simulations. These results are used to set an absolute energy scale for air shower measurements and can be used as a basis for an absolute scale for the measurement of astronomical transients with LOFAR.

  18. High-precision measurements of extensive air showers with the SKA

    CERN Document Server

    Huege, T; Buitink, S; Dallier, R; Ekers, R D; Falcke, H; Haungs, A; James, C W; Martin, L; Revenu, B; Scholten, O; Schröder, F G; Zilles, A

    2015-01-01

    As of 2023, the Square Kilometre Array will constitute the world's largest radio telescope, offering unprecedented capabilities for a diverse science programme in radio astronomy. At the same time, the SKA will be ideally suited to detect extensive air showers initiated by cosmic rays in the Earth's atmosphere via their radio emission. With its very dense and uniform antenna spacing in a fiducial area of one km$^2$ and its large bandwidth of 50-350 MHz, the low-frequency part of the SKA will provide very precise measurements of individual cosmic ray air showers. These precision measurements will allow detailed studies of the mass composition of cosmic rays in the energy region of transition from a Galactic to an extragalactic origin. Also, the SKA will facilitate three-dimensional "tomography" of the electromagnetic cascades of air showers, allowing the study of particle interactions at energies beyond the reach of the LHC. Finally, studies of possible connections between air showers and lightning initiation ...

  19. pp Interaction in Extended Air Showers

    CERN Document Server

    Kohara, A Kendi; Kodama, Takeshi

    2014-01-01

    Applying the recently constructed analytic representation for the pp scattering amplitudes, we present a study of p-air cross sections, with comparison to the data from Extensive Air Shower (EAS) measurements. The amplitudes describe with precision all available accelerator data at ISR, SPS and LHC energies, and its theoretical basis, together with the very smooth energy dependence of parameters controlled by unitarity and dispersion relations, permit reliable extrapolation to higher energies and to asymptotic ranges. The comparison with cosmic ray data is very satisfactory in the whole pp energy interval from 1 to 100 TeV. High energy asymptotic behaviour of cross sections is investigated in view of the geometric scaling property of the amplitudes. The amplitudes predict that the proton does not behave as a black disk even at asymptotically high enegies, and we discuss possible non-trivial consequences of this fact for pA collision cross sections at higher energies.

  20. Phenomenological model of nuclear primary air showers

    Science.gov (United States)

    Tompkins, D. R., Jr.; Saterlie, S. F.

    1976-01-01

    The development of proton primary air showers is described in terms of a model based on a hadron core plus an electromagnetic cascade. The muon component is neglected. The model uses three parameters: a rate at which hadron core energy is converted into electromagnetic cascade energy and a two-parameter sea-level shower-age function. By assuming an interaction length for the primary nucleus, the model is extended to nuclear primaries. Both models are applied over the energy range from 10 to the 13th power to 10 to the 21st power eV. Both models describe the size and age structure (neglecting muons) from a depth of 342 to 2052 g/sq cm.

  1. pp interactions in extended air showers

    Directory of Open Access Journals (Sweden)

    Kendi Kohara A.

    2015-01-01

    Full Text Available Applying the recently constructed analytic representation for the pp scattering amplitudes, we present a study of p-air cross sections, with comparison to the data from Extensive Air Shower (EAS measurements. The amplitudes describe with precision all available accelerator data at ISR, SPS and LHC energies, and its theoretical basis, together with the very smooth energy dependence of parameters controlled by unitarity and dispersion relations, permit reliable extrapolation to higher energies and to asymptotic ranges. The comparison with cosmic ray data is very satisfactory in the whole pp energy interval from 1 to 100 TeV. High energy asymptotic behaviour of cross sections is investigated in view of the geometric scaling property of the amplitudes. The amplitudes predict that the proton does not behave as a black disk even at asymptotically high enegies, and we discuss possible non-trivial consequences of this fact for pA collision cross sections at higher energies.

  2. Arrival direction of successive air showers

    International Nuclear Information System (INIS)

    It was studied the features of series of air shower events (AS cluster) concentrated within short intervals of time of arrival. When the number of events in the cluster reaches the maximum values in the considered data set, the arrival directions of the AS are prevailingly observed around values of right ascension α asymptotically equal to 5 h and α asymptotically equal to 20 h. These values indicate parallelism of directions between the shower directions and the galactic plane. This can be explained by the presence of Ultra-High Energy (UHE) gamma-ray sources, generating showers from their specific direction. The analysis uses three data set of 253k, 664k and 231k events. The results are similar in the three data set

  3. A search for microwave emission from cosmic ray air showers

    Science.gov (United States)

    Williams, Christopher Lee

    At the highest energies, the sources of cosmic rays should be among the most powerful extragalactic accelerators. Large observatories have revealed a flux suppression above a few 1019 eV, similar to the expected effect of the interaction of ultrahigh energy cosmic rays (UHECR) with the cosmic microwave background. The Pierre Auger Observatory has measured the largest sample of cosmic ray induced extensive air showers (EAS) at the highest energies leading to a precise measurement of the energy spectrum, hints of spatial anisotropy, and a surprising change in the chemical composition at the highest energies. To answer the question of the origin of UHECRs a larger sample of high quality data will be required to reach a statistically significant result. One of the possible techniques suggested to achieve this much larger data sample, in a cost effective way, is ultra-wide field of view microwave telescopes which would operate in an analogous way to the already successful fluorescence detection (FD) technique. Detecting EAS in microwaves could be done with 100% duty cycle and essentially no atmospheric effects. This presents many advantages over the FD which has a 10% duty cycle and requires extensive atmospheric monitoring for calibration. We have pursued both prototype detector designs and improved laboratory measurements, the results of which are reported herein, and published in (Alvarez-Muniz et al., 2013; Alvarez-Muniz et al., 2012a; Williams et al., 2013; Alvarez-Muniz et al., 2013). The Microwave Detection of Air Showers (MIDAS) experiment is the first ultra-wide field of view imaging telescope deployed to detect isotropic microwave emission from EAS. With 61 days of livetime data operating on the University of Chicago campus we were able to set new limits on isotropic microwave emission from extensive air showers. The new limits rule out current laboratory air plasma measurements (Gorham et al., 2008) by more than five sigma. The MIDAS experiment continues to

  4. Detailed studies of the electron lateral distribution in extensive air showers with energies around 10(16) eV

    Science.gov (United States)

    Dzikowski, T.; Gawin, J.; Wdowczyk, J.

    1984-01-01

    Detailed studies have been performed of the electron lateral distribution in extensive air showers using the Lodz extensive air shower array. The showers were grouped according to their particle densities around 20 m from the core. The grouping was made in very narrow intervals of the densities. For every group of showers and for every distance interval /changing by 5 m/ histograms of the numbers of electron counters discharged have been obtained. The trays of G.M counters were located at following distances from the center of the triggering detectors array: 16 m, 76 m, 117 m, 137 m, 141 m and 147 m.

  5. Coherent radio emission from cosmic ray air showers computed by Monte-Carlo simulation with SElFAS

    International Nuclear Information System (INIS)

    We present here the first results of SElFAS (Simulation of Electric Field emitted by Air Shower), a new Monte-Carlo simulation of the radio emission by cosmic ray extensive air shower. The simulation is based on the complete geometrical description of secondary electrons and positrons created in air showers generated by protons above 10 PeV. The energy, position and angular distributions of secondary particles are extracted from CORSIKA simulations . The electric field is then computed for each secondary particle during its travel in the atmosphere using the well-known equation of a moving charge which undergoes an acceleration. The total signal emitted by the air shower is per consequent the superposition of all particles contributions and it is computable for any ground position. We present the results obtained for the east-west and north-south polarizations of the total electric field. These polarizations are usually measured by radio detectors such as CODALEMA, LOPES, RAuger and AERA (Auger Engineering Radio Array). The characteristics and the comprehension of the radio emission of cosmic ray extensive air shower are crucial for the development of large radio detectors array.

  6. LOPES — Recent Results and Open Questions on the Radio Detection of Air Showers

    Science.gov (United States)

    Schröder, F. G.; Apel, W. D.; Arteaga-Velázquez, J. C.; Bähren, L.; Bekk, K.; Bertaina, M.; Biermann, P. L.; Blümer, J.; Bozdog, H.; Brancus, I. M.; Cantoni, E.; Chiavassa, A.; Daumiller, K.; de Souza, V.; Di Pierro, F.; Doll, P.; Engel, R.; Falcke, H.; Fuchs, B.; Gemmeke, H.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J. R.; Horneffer, A.; Huber, D.; Huege, T.; Isar, P. G.; Kampert, K.-H.; Kang, D.; Krömer, O.; Kuijpers, J.; Link, K.; Łuczak, P.; Ludwig, M.; Mathes, H. J.; Melissas, M.; Morello, C.; Oehlschläger, J.; Palmieri, N.; Pierog, T.; Rautenberg, J.; Rebel, H.; Roth, M.; Rühle, C.; Saftoiu, A.; Schieler, H.; Schmidt, A.; Schoo, S.; Sima, O.; Toma, G.; Trinchero, G. C.; Weindl, A.; Wochele, J.; Zabierowski, J.; Zensus, J. A.

    2015-08-01

    LOPES was a digital antenna array operating for approximately 10 years until spring 2013 at the Karlsruhe Institute of Technology (KIT). Triggered by the co-located KASCADE-Grande air-shower experiment, it measured the radio signal of around 1000 cosmic-ray air showers with energies E ≳ 1017 eV in an effective band of 43 - 74 MHz. Using the interferometric technique of cross-correlation beamforming, LOPES could reconstruct the shower direction with an accuracy environment of the site. This article summarizes our latest results on the reconstruction of the shower maximum, using two independent methods: the steepness of the hyperbolic radio wavefront and the slope of the lateral distribution of the radio amplitude. Moreover, we show vectorial measurements of the electric field with the tripole antennas of the latest LOPES setup. Finally, we discuss open questions as well as the potential impact of the lessons learned at LOPES for future antenna arrays.

  7. Muon bremsstrahlung and muonic pair production in air showers

    International Nuclear Information System (INIS)

    The objective of this work is to report on the modifications in air shower development due to muon bremsstrahlung and muonic pair production. In order to do that we have implemented new muon bremsstrahlung and muonic pair production procedures in the AIRES air shower simulation system, and have used it to simulate ultra high energy showers in different conditions. The influence of the mentioned processes in the global development of the air shower is important for primary particles of large zenith angles, while they do not introduce significant changes in the position of the shower maximum

  8. Nuclear interactions and the highest energy air showers

    International Nuclear Information System (INIS)

    Based on the energy distribution of particles produced in multiple particle production, which is formulated phenomenologically by the data of direct observation, it was calculated the air shower development at E0=1020 eV. The calculation shows that the formula, extrapolated into the higher energy region, does not describe the highest energy air showers. It was also argued that the energy estimation of the highest energy air showers may have an ambiguity of a factor ∼ 2, due to the incomplete knowledge on high energy interactions

  9. Frequency spectra of cosmic ray air shower radio emission measured with LOPES

    CERN Document Server

    Nigl, A

    2008-01-01

    AIMS: We wish to study the spectral dependence of the radio emission from cosmic-ray air showers around 100 PeV (1017 eV). METHODS: We observe short radio pulses in a broad frequency band with the dipole-interferometer LOPES (LOFAR Prototype Station), which is triggered by a particle detector array named Karlsruhe Shower Core and Array Detector (KASCADE). LOFAR is the Low Frequency Array. For this analysis, 23 strong air shower events are selected using parameters from KASCADE. RESULTS: The resulting electric field spectra fall off to higher frequencies. An average electric field spectrum is fitted with an exponential, or alternatively, with a power law. The spectral slope obtained is not consistent within uncertainties and it is slightly steeper than the slope obtained from Monte Carlo simulations based on air showers simulated with CORSIKA (Cosmic Ray Simulations for KASCADE). One of the strongest events was measured during thunderstorm activity in the vicinity of LOPES and shows the longest pulse length me...

  10. Computational simulation of the extensive air shower

    International Nuclear Information System (INIS)

    Full text: Cosmic Rays (CRs) are defined as particles of cosmic origin reaching at the top of Earth's atmosphere. Two central questions guide the research of CRs. The detection of CRs occurs by indirect experimental techniques, due to the very low flux of primaries. The primary particle interacts with the atmosphere and generates secondary particles in a large cascade called Extensive Air Shower (EAS). The code CORSIKA (COsmic Ray SImulations for KAscade) is a detailed Monte Carlo, whose aim is to simulate the evolution of EASs through the atmosphere. With this project we aim to produce an extensive library of showers, using several interaction models and different energies (from very-high to ultra-high energies), generating important data to be studied by the cosmic rays group of UFABC. The project aim is to simulate EAS through the CORSIKA code, generating a wide library for understanding the influence of the models of high energy hadronic interactions in the particles production of their physical parameters. After performing some simulations, studying the elongation rate from different primary compositions and determining the ratio of events formation and energy the threshold of the main current events. Finally, we will propose processes not contemplated in the simulation or possible improvements in existing models. (author)

  11. Air shower arrival directions measured at Buckland Park

    International Nuclear Information System (INIS)

    The Buckland Park air shower array was operated for 3 years from 1979 to 1981 particularly for the study of anisotropies in the region of the knee of the size spectrum. The array which has been described in detail elsewhere was situated at a latitude of 35 S and had an effective size threshold of approx 3 x 10 to the 5th power particles (approx 3 x 10 to the 15th power Ev for vertical showers). A number of results from this experiment have already been published including anisotropy analyses (Gerhardy and Clay, 1983) and searches for very high energy gamma ray sources. The final distribution of measured shower arrival directions are presented here. These 1.3 x 10 to the 5th power events were selected as indicated in detail in Gerhardy and Clay (1983) and were essentially those events with well measured arrival directions. They are the same data set used in the above reference but no complete sky map has previously been presented

  12. Air shower arrival directions measured at Buckland Park

    Science.gov (United States)

    Gerhardy, P. R.; Prescott, J. R.; Protheroe, R. J.; Clay, R. W.; Patterson, J. R.; Gregory, A. G.

    1985-01-01

    The Buckland Park air shower array was operated for 3 years from 1979 to 1981 particularly for the study of anisotropies in the region of the knee of the size spectrum. The array which has been described in detail elsewhere was situated at a latitude of 35 S and had an effective size threshold of approx 3 x 10 to the 5th power particles (approx 3 x 10 to the 15th power Ev for vertical showers). A number of results from this experiment have already been published including anisotropy analyses (Gerhardy and Clay, 1983) and searches for very high energy gamma ray sources. The final distribution of measured shower arrival directions are presented here. These 1.3 x 10 to the 5th power events were selected as indicated in detail in Gerhardy and Clay (1983) and were essentially those events with well measured arrival directions. They are the same data set used in the above reference but no complete sky map has previously been presented.

  13. Methods of determination of the energy and mass of primary cosmic ray particles at extensive air shower energies

    International Nuclear Information System (INIS)

    Measurements of cosmic ray particles at energies above E > or ∼ 5x1014 eV are performed by large-area ground-based air shower experiments. Only they provide the collection power required to obtain sufficient statistics at the low flux levels involved. In this review we briefly outline the physics and astrophysics interest of such measurements and discuss in more detail various experimental techniques applied for reconstructing the energy and mass of the primary particles. These include surface arrays of particle detectors as well as observations of Cherenkov and of fluorescence light. A large variety of air shower observables is then reconstructed from such data and used to infer the properties of the primary particles via comparisons to air shower simulations. Advantages, limitations and systematic uncertainties of different approaches will be critically discussed. (author)

  14. Microwave detection of air showers with the MIDAS experiment

    Science.gov (United States)

    Privitera, Paolo; Alekotte, I.; Alvarez-Muñiz, J.; Berlin, A.; Bertou, X.; Bogdan, M.; Boháčová, M.; Bonifazi, C.; Carvalho, W. R.; de Mello Neto, J. R. T.; Facal San Luis, P.; Genat, J. F.; Hollon, N.; Mills, E.; Monasor, M.; Reyes, L. C.; Rouille d'Orfeuil, B.; Santos, E. M.; Wayne, S.; Williams, C.; Zas, E.

    2011-03-01

    Microwave emission from Extensive Air Showers could provide a novel technique for ultra-high energy cosmic rays detection over large area and with 100% duty cycle. We describe the design, performance and first results of the MIDAS (MIcrowave Detection of Air Showers) detector, a 4.5 m parabolic dish with 53 feeds in its focal plane, currently installed at the University of Chicago.

  15. Microwave detection of air showers with the MIDAS experiment

    Energy Technology Data Exchange (ETDEWEB)

    Privitera, Paolo [University of Chicago, Enrico Fermi Institute and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Alekotte, I. [Centro Atomico Bariloche and Instituto Balseiro (CNEA-UNCuyo-CONICET), 8400 San Carlos de Bariloche, Rio Negro (Argentina); Alvarez-Muniz, J. [Universidad de Santiago de Compostela, Departamento de Fisica de Particulas, Campus Sur, E-15782 Santiago de Compostela (Spain); Berlin, A. [University of Chicago, Enrico Fermi Institute and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Bertou, X. [Centro Atomico Bariloche and Instituto Balseiro (CNEA-UNCuyo-CONICET), 8400 San Carlos de Bariloche, Rio Negro (Argentina); Bogdan, M.; Bohacova, M. [University of Chicago, Enrico Fermi Institute and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Bonifazi, C. [Univ. Federal do Rio de Janeiro (UFRJ), Instituto de Fisica, Cidade Universitaria, Caixa Postal 68528, 21945- 970 Rio de Janeiro, RJ (Brazil); Carvalho, W.R. [Universidad de Santiago de Compostela, Departamento de Fisica de Particulas, Campus Sur, E-15782 Santiago de Compostela (Spain); Mello Neto, J.R.T. de [Univ. Federal do Rio de Janeiro (UFRJ), Instituto de Fisica, Cidade Universitaria, Caixa Postal 68528, 21945- 970 Rio de Janeiro, RJ (Brazil); Facal San Luis, P.; Genat, J.F.; Hollon, N.; Mills, E.; Monasor, M.; Reyes, L.C.; Rouille d' Orfeuil, B. [University of Chicago, Enrico Fermi Institute and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Santos, E.M. [Univ. Federal do Rio de Janeiro (UFRJ), Instituto de Fisica, Cidade Universitaria, Caixa Postal 68528, 21945- 970 Rio de Janeiro, RJ (Brazil); Wayne, S.; Williams, C. [University of Chicago, Enrico Fermi Institute and Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)

    2011-03-15

    Microwave emission from Extensive Air Showers could provide a novel technique for ultra-high energy cosmic rays detection over large area and with 100% duty cycle. We describe the design, performance and first results of the MIDAS (MIcrowave Detection of Air Showers) detector, a 4.5 m parabolic dish with 53 feeds in its focal plane, currently installed at the University of Chicago.

  16. Transition effect of air shower particles in plastic scintillators

    Science.gov (United States)

    Asakimori, K.; Maeda, T.; Kameda, T.; Mizushima, K.; Misaki, Y.

    1985-01-01

    The transition effect of air shower particles in the plastic scintillators near the core was measured by scintillators of various thickness. The air showers selected for the measurement were of 10,000. Results obtained are as follows: (1) the multiplication of shower particles in the scintillators is less than 20% for that of 50 mm thickness; (2) dependence of the transition effect on age parameter is not recognized within the experimental errors.

  17. Macroscopic model of radio emission from extensive air showers

    International Nuclear Information System (INIS)

    A macroscopic model of radio emission from extensive air showers is developed. This model is appropriate for calculating this radio emission at frequencies below 100 MHz. It is constructed on the basis of an analysis of the radiation integral and is verified by comparing field observables predicted by the model with the respective results obtained within the microscopic approach to calculating radio emission from extensive air showers.

  18. Arrival time distribution of muons in large air showers observed at 900m above sea level

    International Nuclear Information System (INIS)

    The arrival time distribution of muons (>1GeV) in large air showers above 1017 eV has been measured at core distances from 100m to 250m in the Akeno air shower array (900m a.s.1.) using four 2m2 scintillation detectors and an equipment with a time response of 3.5ns in rise time and 7.0ns in FWHM. The time from 20% to 70% in integral arrival time distribution (tsub(20-70)) suggests a very fast development of muons expected from the enhanced Esup(1/2) multiplicity law and the rising cross section for primary protons. This result is consistent with thoose obtained from the measurement of arrival time distribution of muons and the equi-intensity cuts of muon-size spectra at Chacaltaya (5200m a.s.1.)

  19. Search for large-scale coincidences in network observation of cosmic ray air showers

    International Nuclear Information System (INIS)

    The Large Area Air Shower (LAAS) group has been performing a network observation of extensive air showers (EAS) since 1996 in Japan. Eight compact EAS arrays (ten in the near future) are operating simultaneously and independently at distant stations (up to ∼ 1000 km), constituting a gigantic detector system as a whole. Using five stations' datasets, large-scale coincidences of EAS have been searched for with the aim of detecting signals from extremely short bursts in the universe. By comparing arrival times and arrival directions of all registered EAS, three coincident and parallel EAS pairs were extracted out of a sea of background cosmic rays. One of them was observed almost from the direction of the Crab Nebula, a previously reported ultra-high-energy γ-ray source. The first application reported here allows the analysis techniques to be tested and demonstrates the potential of observations with the full operation of the network detector system

  20. Correlation of high energy muons with primary composition in extensive air shower

    Science.gov (United States)

    Chou, C.; Higashi, S.; Hiraoka, N.; Ozaki, S.; Sato, T.; Suwada, T.; Takahasi, T.; Umeda, H.

    1985-01-01

    An experimental investigation of high energy muons above 200 GeV in extensive air showers has been made for studying high energy interaction and primary composition of cosmic rays of energies in the range 10 to the 14th power approx. 10 to the 15th power eV. The muon energies are estimated from the burst sizes initiated by the muons in the rock, which are measured by four layers of proportional counters, each of area 5 x 2.6 sq m, placed at 30 m.w.e. deep, Funasaka tunnel vertically below the air shower array. These results are compared with Monte Carlo simulations based on the scaling model and the fireball model for two primary compositions, all proton and mixed.

  1. Radio detection of Cosmic-Ray Air Showers and High-Energy Neutrinos

    CERN Document Server

    Schröder, Frank G

    2016-01-01

    This review provides an introduction to the radio emission by particle cascades, an overview on the various experiments, and explains methods for the radio measurement of air-shower properties. Furthermore, potential applications of the radio technique in high-energy astroparticle physics are discussed. Due to the successful operation of digital radio experiments and due to the improved quantitative understanding of the emission, radio detection is back on the list of promising techniques for extensive air showers. With a threshold of about 100 PeV radio detectors are particularly useful to study the highest-energy galactic cosmic rays and ultra-high-energy extragalactic particles of all types. Various antenna arrays like LOPES, CODALEMA, AERA, LOFAR, and Tunka-Rex have shown that radio measurements can compete in precision with other techniques, in particular for the arrival direction, the energy, and the position of the shower maximum. The scientific potential of the radio technique seems to be maximum in c...

  2. Reconstruction of air-shower parameters for large-scale radio detectors using the lateral distribution

    Science.gov (United States)

    Kostunin, D.; Bezyazeekov, P. A.; Hiller, R.; Schröder, F. G.; Lenok, V.; Levinson, E.

    2016-02-01

    We investigate features of the lateral distribution function (LDF) of the radio signal emitted by cosmic ray air-showers with primary energies Epr > 0.1 EeV and its connection to air-shower parameters such as energy and shower maximum using CoREAS simulations made for the configuration of the Tunka-Rex antenna array. Taking into account all significant contributions to the total radio emission, such as by the geomagnetic effect, the charge excess, and the atmospheric refraction we parameterize the radio LDF. This parameterization is two-dimensional and has several free parameters. The large number of free parameters is not suitable for experiments of sparse arrays operating at low SNR (signal-to-noise ratios). Thus, exploiting symmetries, we decrease the number of free parameters based on the shower geometry and reduce the LDF to a simple one-dimensional function. The remaining parameters can be fit with a small number of points, i.e. as few as the signal from three antennas above detection threshold. Finally, we present a method for the reconstruction of air-shower parameters, in particular, energy and Xmax (shower maximum), which can be reached with a theoretical accuracy of better than 15% and 30 g/cm2, respectively.

  3. Analysis of the muon spectra for inclined air showers measured with the KASCADE-grande experiment

    Energy Technology Data Exchange (ETDEWEB)

    Arteaga-Velazquez, Juan Carlos [Institut fuer Experimentelle Kernphysik, Universitaet Karlsruhe (Germany)

    2008-07-01

    The solving of the mystery of the second knee in the cosmic ray spectrum is one of the main objectives of the KASCADE-grande observatory. KASCADE-grande is a ground array composed of different subsystems of detectors that, as a whole, allows to study simultaneously the electromagnetic and penetrating component of cosmic ray air showers in the energy range between 100 TeV and 1 EeV. Vertical showers (with zenith angles below 40 ) are studied in detail at KASCADE-grande. Now, the analyses are being extended to higher zenith angles as a way to study the muon content of air showers and to increase the statistics of the experiment. In this talk, the muon spectra reconstructed for vertical and inclined air showers measured by the KASCADE-grande observatory are presented and also confronted with Monte Carlos simulations based on the hadronic interaction models QGSJET II and EPOS. In addition, the result of the analysis of the observed spectra with the ''constant intensity cut method'' is shown. This method was applied in a first attempt to understand the origin of a systematic discrepancy found between the predicted and measured muon spectra, which increases with the zenith angle.

  4. Polarized radio emission from extensive air showers measured with LOFAR

    International Nuclear Information System (INIS)

    We present LOFAR measurements of radio emission from extensive air showers. We find that this emission is strongly polarized, with a median degree of polarization of nearly 99%, and that the angle between the polarization direction of the electric field and the Lorentz force acting on the particles, depends on the observer location in the shower plane. This can be understood as a superposition of the radially polarized charge-excess emission mechanism, first proposed by Askaryan and the geomagnetic emission mechanism proposed by Kahn and Lerche. We calculate the relative strengths of both contributions, as quantified by the charge-excess fraction, for 163 individual air showers. We find that the measured charge-excess fraction is higher for air showers arriving from closer to the zenith. Furthermore, the measured charge-excess fraction also increases with increasing observer distance from the air shower symmetry axis. The measured values range from (3.3± 1.0)% for very inclined air showers at 25 m to (20.3± 1.3)% for almost vertical showers at 225 m. Both dependencies are in qualitative agreement with theoretical predictions

  5. Nitrogen fluorescence in air for observing extensive air showers

    Directory of Open Access Journals (Sweden)

    Tsunesada Y.

    2013-06-01

    Full Text Available Extensive air showers initiate the fluorescence emissions from nitrogen molecules in air. The UV-light is emitted isotropically and can be used for observing the longitudinal development of extensive air showers in the atmosphere over tenth of kilometers. This measurement technique is well-established since it is exploited for many decades by several cosmic ray experiments. However, a fundamental aspect of the air shower analyses is the description of the fluorescence emission in dependence on varying atmospheric conditions. Different fluorescence yields affect directly the energy scaling of air shower reconstruction. In order to explore the various details of the nitrogen fluorescence emission in air, a few experimental groups have been performing dedicated measurements over the last decade. Most of the measurements are now finished. These experimental groups have been discussing their techniques and results in a series of Air Fluorescence Workshops commenced in 2002. At the 8th Air Fluorescence Workshop 2011, it was suggested to develop a common way of describing the nitrogen fluorescence for application to air shower observations. Here, first analyses for a common treatment of the major dependences of the emission procedure are presented. Aspects like the contributions at different wavelengths, the dependence on pressure as it is decreasing with increasing altitude in the atmosphere, the temperature dependence, in particular that of the collisional cross sections between molecules involved, and the collisional de-excitation by water vapor are discussed.

  6. Simulation of Radiation Energy Release in Air Showers

    CERN Document Server

    Glaser, Christian; Hörandel, Jörg R; Huege, Tim; Schulz, Johannes

    2016-01-01

    A simulation study of the energy released by extensive air showers in the form of MHz radiation is performed using the CoREAS simulation code. We develop an efficient method to extract this radiation energy from air-shower simulations. We determine the longitudinal profile of the radiation energy release and compare it to the longitudinal profile of the energy deposit by the electromagnetic component of the air shower. We find that the radiation energy corrected for the geometric dependence of the geomagnetic emission scales quadratically with the energy in the electromagnetic component of the air shower with a second-order dependence on the atmospheric density at the position of the maximum shower development $X_\\mathrm{max}$. In a measurement where $X_\\mathrm{max}$ is not accessible, this second order dependence can be approximated using the zenith angle of the incoming direction of the air shower with only a minor loss in accuracy. Our method results in an intrinsic uncertainty of 4% in the determination o...

  7. A new model-independent approach for finding the arrival direction of an extensive air shower

    CERN Document Server

    Kh, H Hedayati

    2016-01-01

    A new accurate method for reconstructing the arrival direction of an extensive air shower (EAS) is described. Compared to existing methods, it is not subject to minimization of a function and, therefore, is fast and stable. This method also does not need to know detailed curvature or thickness structure of an EAS. It can have angular resolution of about 1 degree for a typical surface array in central regions. Also, it has better angular resolution than other methods in the marginal area of arrays.

  8. Feasibility of radar detection of extensive air showers

    Science.gov (United States)

    Stasielak, J.; Engel, R.; Baur, S.; Neunteufel, P.; Šmída, R.; Werner, F.; Wilczyński, H.

    2016-01-01

    Reflection of radio waves off the short-lived plasma produced by the high-energy shower particles in the air is simulated, considering various radar setups and shower geometries. We show that the plasma produced by air showers has to be treated always as underdense. Therefore, we use the Thomson cross-section for scattering of radio waves corrected for molecular quenching and we sum coherently contributions of the reflected radio wave over the volume of the plasma disk to obtain the time evolution of the signal arriving at the receiver antenna. The received power and the spectral power density of the radar echo are analyzed. Based on the obtained results, we discuss possible modes of radar detection of extensive air showers. We conclude that the scattered signal is too weak for the radar method to provide an efficient and inexpensive method of air shower detection.

  9. Feasibility of radar detection of extensive air showers

    CERN Document Server

    Stasielak, J; Baur, S; Neunteufel, P; Šmída, R; Werner, F; Wilczyński, H

    2014-01-01

    Reflection of radio waves off the short-lived plasma produced by the high-energy shower particles in the air is simulated, considering various radar setups and shower geometries. We show that the plasma produced by air showers has to be treated always as underdense. Therefore, we use the Thomson cross-section for scattering of radio waves corrected for molecular quenching and we sum coherently contributions of the reflected radio wave over the volume of the plasma disk to obtain the time evolution of the signal arriving at the receiver antenna. The received power and the spectral power density of the radar echo are analyzed. Based on the obtained results, we discuss possible modes of radar detection of extensive air showers. We conclude that the scattered signal is too weak for the radar method to provide an efficient and inexpensive method of air shower detection.

  10. The air shower simulation program CORSIKA and hadronic interaction models

    International Nuclear Information System (INIS)

    CORSIKA is a program for detailed simulation of the evolution of extensive air showers initiated by high-energy cosmic ray particles. Protons, light nuclei up to iron, photons, and many other particles may be treated as primaries. The particles are tracked through the atmosphere until they undergo reactions with the air nuclei or - in the case of instable secondaries - decay. The hadronic interactions at high energies may be described by six reaction models alternatively. The influence of these models on simulation predictions of measurable air shower features is demonstrated with examples. (orig.)

  11. Cosmic ray radio emission as air shower detection

    International Nuclear Information System (INIS)

    The possibility of radio-detection of ultra-high energy cosmic rays (within the 10 to 100 MHz range) are discussed. Currently, air showers are detected by various methods, mainly based on particle detectors (KASCADE, Auger) or optical detection (Cerenkov radiation). Recently,to detect radio emission from cosmic ray air showers a method using electromagnetic radiation in low frequency domain (LOFAR) was proposed. We are investigating this possibility, using simulation codes created to investigate electromagnetic radiation of intricate antennae structure, for example fractal antennas. Some of the preliminary results will be communicated in this session. (authors)

  12. Algorithms for reconstruction of shower core and arrival direction of extensive air showers

    International Nuclear Information System (INIS)

    Two important observables that describe extensive air showers (EAS) are the center of particle distribution in the shower front (the center of gravity of the particle distribution) and the arrival direction (the zenithal and azimuthal angle of the shower axis). A program was developed that, using results given by CORSIKA simulations, reconstructs the center of the EAS front and the arrival direction as well. The program uses different algorithms and a study of reconstructing efficiency has been done for each algorithm or even for the same algorithm relative to where an extensive air shower hits the detector array. As geometrical model for the detector array, the KASCADE - Grande detector array (Karlsruhe, Germany) has been used. The reconstruction of the center of the shower front has been done by using an algorithm that calculates the center of gravity of particle mass distribution in detectors. A good reconstruction efficiency has been achieved for showers hitting near the center of the array. Also, an increase in the reconstruction error as the shower front hits the array closer to the border occurred. The arrival direction reconstruction algorithms were used as input data while the arrival time of particles in detectors was deduced by approximating the shower front with a plane, a conic or a spherical surface. Efficiency of these algorithms has also been studied. (authors)

  13. Search for molecular bremsstrahlung radiation signals in Ku band with coincidental operations of radio telescopes with air shower detectors

    International Nuclear Information System (INIS)

    Microwave radiation from extensive air showers is expected to provide a new technique to observe UHECR. We developed three set of radio telescopes in Osaka, in Kobe and at Telescope Array site in Utah, USA. In Osaka, we are coincidentally operating two Ku band radio telescopes with an air shower array which consists of nine plastic scintillators with about 10 m separation. In Kobe, we have started the operation of twelve radio telescopes of 1.2 m diameter in March 2012. In Utah, we installed two telescopes just beside the Black Rock Mesa fluorescence detector (FD) station of the Telescope Array experiment, and we operated the radio telescopes coincidentally with FD event triggers. We report the experimental setups and the results of these measurements.

  14. Observation of Horizontal Air Showers with ARGO-YBJ

    International Nuclear Information System (INIS)

    A preliminary analysis of Extensive Air Showers reconstructed by ARGO-YBJ with zenith angle greater than 80° is reported. The measurement of the size spectrum and of the azimuthal distribution is discussed. A description of the topology of these events is also provided.

  15. Muon spectrum in air showers initiated by gamma rays

    Science.gov (United States)

    Stephens, S. A.; Streitmatter, R. E.

    1985-01-01

    An analytic representation for the invariant cross-section for the production of charged pions in gamma P interactions was derived by using the available cross-sections. Using this the abundance of muons in a gamma ray initiated air shower is calculated.

  16. The development of air shower in the iron absorber

    Science.gov (United States)

    Hazama, M.; Dake, S.; Harada, K.; Kawamoto, M.; Sakata, M.; Yamamoto, Y.; Sugihara, T.

    1985-01-01

    The iron open-sandwich experiments to observe one dimensional development of individual air showers were carried out at Akeno Observatory. One dimensional energy flow, incident energy and production height of shower is estimated using the data of size and age obtained from the above experiment and simple calculation.

  17. Precision measurements of cosmic ray air showers with the SKA

    NARCIS (Netherlands)

    Huege, T.; Bray, J.; Buitink, S.; Dallier, R.; Ekers, R. D.; Falcke, H. D. E.; James, C. W.; Martin, L.; Revenu, B.; Scholten, O.; Schroeder, F.

    2014-01-01

    Supplemented with suitable buffering techniques, the low-frequency part of the SKA can be used as an ultra-precise detector for cosmic-ray air showers at very high energies. This would enable a wealth of scientific applications: the physics of the transition from Galactic to extragalactic cosmic ray

  18. Analysis of the extensive air showers of ultra-high energy

    International Nuclear Information System (INIS)

    When we study extensive air showers (EAS), which correlate with pulsars, we had been found showers without a muon component. Here we analyzed the arrival directions of EAS with poor and without a muon component. We find that the arrival directions of these showers correlate with some pulsars which are distributed more isotropy. Among these pulsars with the short period of rotation around their axis are prevailed than it is expected by the catalogue of pulsars. In this connection the data of world arrays are considered.

  19. A Statistical Method for Reconstructing the Core Location of an Extensive Air Shower

    Science.gov (United States)

    Hedayati Kh., H.; Moradi, A.; Emami, M.

    2015-09-01

    Conventional methods of reconstructing extensive air showers (EASs) depend on a lateral density function which itself depends on shower size, age parameter, and core location. In the fitting procedure of a lateral density function to surface array information, the only parameter whose initial value is essential is core location. In this paper, we describe a refined version of a statistical method which can be used to find the initial trial core location of EASs with better precision than the conventional methods. In this method, we use arrival time information of secondary particles for finding not only arrival direction, but also core location.

  20. Full Monte-Carlo description of the Moscow State University Extensive Air Shower experiment

    CERN Document Server

    Fomin, Yu A; Karpikov, I S; Kulikov, G V; Kuznetsov, M Yu; Rubtsov, G I; Sulakov, V P; Troitsky, S V

    2016-01-01

    The Moscow State University Extensive Air Shower (EAS-MSU) array studied high-energy cosmic rays with primary energies ~(1-500) PeV in the Northern hemisphere. The EAS-MSU data are being revisited following recently found indications to an excess of muonless showers, which may be interpreted as the first observation of cosmic gamma rays at ~100 PeV. In this paper, we present a complete Monte-Carlo model of the surface detector which results in a good agreement between data and simulations. The model allows us to study the performance of the detector and will be used in further studies of the muon data.

  1. Nanosecond-level time synchronization of autonomous radio detector stations for extensive air showers

    International Nuclear Information System (INIS)

    To exploit the full potential of radio measurements of cosmic-ray air showers at MHz frequencies, a detector timing synchronization within 1 ns is needed. Large distributed radio detector arrays such as the Auger Engineering Radio Array (AERA) rely on timing via the Global Positioning System (GPS) for the synchronization of individual detector station clocks. Unfortunately, GPS timing is expected to have an accuracy no better than about 5 ns. In practice, in particular in AERA, the GPS clocks exhibit drifts on the order of tens of ns. We developed a technique to correct for the GPS drifts, and an independent method is used to cross-check that indeed we reach a nanosecond-scale timing accuracy by this correction. First, we operate a ''beacon transmitter'' which emits defined sine waves detected by AERA antennas recorded within the physics data. The relative phasing of these sine waves can be used to correct for GPS clock drifts. In addition to this, we observe radio pulses emitted by commercial airplanes, the position of which we determine in real time from Automatic Dependent Surveillance Broadcasts intercepted with a software-defined radio. From the known source location and the measured arrival times of the pulses we determine relative timing offsets between radio detector stations. We demonstrate with a combined analysis that the two methods give a consistent timing calibration with an accuracy of 2 ns or better. Consequently, the beacon method alone can be used in the future to continuously determine and correct for GPS clock drifts in each individual event measured by AERA

  2. Nanosecond-level time synchronization of autonomous radio detector stations for extensive air showers

    Science.gov (United States)

    The Pierre Auger Collaboration

    2016-01-01

    To exploit the full potential of radio measurements of cosmic-ray air showers at MHz frequencies, a detector timing synchronization within 1 ns is needed. Large distributed radio detector arrays such as the Auger Engineering Radio Array (AERA) rely on timing via the Global Positioning System (GPS) for the synchronization of individual detector station clocks. Unfortunately, GPS timing is expected to have an accuracy no better than about 5 ns. In practice, in particular in AERA, the GPS clocks exhibit drifts on the order of tens of ns. We developed a technique to correct for the GPS drifts, and an independent method is used to cross-check that indeed we reach a nanosecond-scale timing accuracy by this correction. First, we operate a ``beacon transmitter'' which emits defined sine waves detected by AERA antennas recorded within the physics data. The relative phasing of these sine waves can be used to correct for GPS clock drifts. In addition to this, we observe radio pulses emitted by commercial airplanes, the position of which we determine in real time from Automatic Dependent Surveillance Broadcasts intercepted with a software-defined radio. From the known source location and the measured arrival times of the pulses we determine relative timing offsets between radio detector stations. We demonstrate with a combined analysis that the two methods give a consistent timing calibration with an accuracy of 2 ns or better. Consequently, the beacon method alone can be used in the future to continuously determine and correct for GPS clock drifts in each individual event measured by AERA.

  3. The search for extended air showers at the Jicamarca Radio Observatory

    International Nuclear Information System (INIS)

    This paper presents the status of the project to detect extended air showers at the Jicamarca Radio Observatory. We report on detected anomalous signals and present a toy model to estimate at what altitudes we might expect to see air shower signals. According to this model, a significant number of high altitude horizontal air showers could be observed by radar techniques.

  4. Tunka-Rex: the Cost-Effective Radio Extension of the Tunka Air-Shower Observatory

    CERN Document Server

    Schröder, F G; Budnev, N M; Gress, O A; Haungs, A; Hiller, R; Huege, T; Kazarina, Y; Kleifges, M; Konstantinov, E N; Korosteleva, E E; Kostunin, D; Krömer, O; Kuzmichev, L A; Mirgazov, R R; Pankov, L; Prosin, V V; Rubtsov, G I; Savinov, V; Wischnewski, R; Zagorodnikov, A

    2015-01-01

    Tunka-Rex is the radio extension of the Tunka cosmic-ray observatory in Siberia close to Lake Baikal. Since October 2012 Tunka-Rex measures the radio signal of air-showers in coincidence with the non-imaging air-Cherenkov array Tunka-133. Furthermore, this year additional antennas will go into operation triggered by the new scintillator array Tunka-Grande measuring the secondary electrons and muons of air showers. Tunka-Rex is a demonstrator for how economic an antenna array can be without losing significant performance: we have decided for simple and robust SALLA antennas, and we share the existing DAQ running in slave mode with the PMT detectors and the scintillators, respectively. This means that Tunka-Rex is triggered externally, and does not need its own infrastructure and DAQ for hybrid measurements. By this, the performance and the added value of the supplementary radio measurements can be studied, in particular, the precision for the reconstructed energy and the shower maximum in the energy range of a...

  5. Tunka-Rex: the Cost-Effective Radio Extension of the Tunka Air-Shower Observatory

    Science.gov (United States)

    Schröder, F. G.; Bezyazeekov, P.; Budnev, N. M.; Gress, O. A.; Haungs, A.; Hiller, R.; Huege, T.; Kazarina, Y.; Kleifges, M.; Konstantinov, E. N.; Korosteleva, E. E.; Kostunin, D.; Krömer, O.; Kuzmichev, L. A.; Mirgazov, R. R.; Pankov, L.; Prosin, V. V.; Rubtsov, G. I.; Savinov, V.; Wischnewski, R.; Zagorodnikov, A.

    Tunka-Rex is the radio extension of the Tunka cosmic-ray observatory in Siberia close to Lake Baikal. Since October 2012 Tunka-Rex measures the radio signal of air-showers in coincidence with the non-imaging air-Cherenkov array Tunka-133. Furthermore, this year additional antennas will go into operation triggered by the new scintillator array Tunka-Grande measuring the secondary electrons and muons of air showers. Tunka-Rex is a demonstrator for how economic an antenna array can be without losing significant performance: we have decided for simple and robust SALLA antennas, and we share the existing DAQ running in slave mode with the PMT detectors and the scintillators, respectively. This means that Tunka-Rex is triggered externally, and does not need its own infrastructure and DAQ for hybrid measurements. By this, the performance and the added value of the supplementary radio measurements can be studied, in particular, the precision for the reconstructed energy and the shower maximum in the energy range of approximately 1017-1018 eV. Here we show first results on the energy reconstruction indicating that radio measurements can compete with air-Cherenkov measurements in precision. Moreover, we discuss future plans for Tunka-Rex.

  6. Evidence for the charge-excess contribution in air shower radio emission observed by the CODALEMA experiment

    Science.gov (United States)

    Bellétoile, A.; Dallier, R.; Lecacheux, A.; Marin, V.; Martin, L.; Revenu, B.; Torres, D.

    2015-09-01

    CODALEMA is one of the pioneer experiments dedicated to the radio detection of ultra high energy cosmic rays (UHECR), located at the radio observatory of Nançay (France). The CODALEMA experiment uses both a particle detector array and a radio antenna array. Data from both detection systems have been used to determine the ground coordinates of the core of extensive air showers (EAS). We discuss the observed systematic shift of the core positions determined with these two detection techniques. We show that this shift is due to the charge-excess contribution to the total radio emission of air showers, using the simulation code SELFAS. The dependences of the radio core shift to the primary cosmic ray characteristics are studied in details. The observation of this systematic shift can be considered as an experimental signature of the charge excess contribution.

  7. Muons in large extensive air showers

    International Nuclear Information System (INIS)

    The responses of shielded scintillators and flash tubes to muons in EAS have been compared. At low densities (-2) precise agreement is obtained but at higher densities the flash tubes tend to saturate. Experimental mean muon density lateral distributions as derived from different arrays show good agreement and indicate that such muon studies provide an accurate method of calibrating the EAS arrays relative to each other. An attempt to detect EAS fluctuations by sampling the muons with a 12 m2 detector shows the difficulty of this technique. However, by selecting the 10% of showers with densities 1.5 sigma above average density a significant anisotropy in celestial co-ordinates of the arrival direction of 'muon-rich' showers is observed. The implication of such an anisotropy (approximately 13 hr RA) is pointed out. (orig.)

  8. TRASGO: A proposal for a timing RPCs based detector for analyzing cosmic ray air showers

    International Nuclear Information System (INIS)

    The study of the properties of primary cosmic rays with energies above 100 TeV is only accessible indirectly through the use of detector arrays at the Earth surface. Despite the extremely high multiplicity of the air showers produced in their interactions at the highest layers of the atmosphere, only a fraction of those particles arrive to the ground over surfaces from ∼0.1 to ∼100km2. The lack of information on the primary interaction and the low density of particles at the detection plane make the event by event analysis very complicated and usually only mean analysis are possible, sometimes with the help of simulation programs. The necessity of covering big surfaces to gather a significant sample of information usually leads to the use of big volume detectors with limited performances, giving only access to a small part of the information carried out by the swarm of secondary particles of the shower. In this article, we propose the development of an affordable detector, the TRASGO, based on timing RPCs (Resistive Plate Chambers) offering at the same time very good timing and tracking performances. TRASGO would allow a better and more accurate reconstruction of the air shower properties either working stand-alone or in big surface arrays.

  9. Reconstruction of air-shower parameters for large-scale radio detectors using the lateral distribution

    CERN Document Server

    Kostunin, D; Hiller, R; Schröder, F G; Lenok, V; Levinson, E

    2016-01-01

    We investigate features of the lateral distribution function (LDF) of the radio signal emitted by cosmic ray air-showers with primary energies $> 0.1$~EeV and its connection to air-shower parameters such as energy and shower maximum using CoREAS simulations made for the configuration of the Tunka-Rex antenna array. Taking into account all significant contributions to the total radio emission, such as by the geomagnetic effect, the charge excess, and the atmospheric refraction we parameterize the radio LDF. This parameterization is two-dimensional and has several free parameters. The large number of free parameters is not suitable for experiments of sparse arrays operating at low SNR (signal-to-noise ratios). Thus, exploiting symmetries, we decrease the number of free parameters and reduce the LDF to a simple one-dimensional function. The remaining parameters can be fit with a small number of points, i.e. as few as the signal from three antennas above detection threshold. Finally, we present a method for the r...

  10. The MIDAS experiment: MIcrowave Detection of Air Showers

    Science.gov (United States)

    Facal, Pedro; Bohacova, Martina; Monasor, Maria; Privitera, Paolo; Reyes, Luis C.; Williams, Cristopher

    2010-02-01

    Recent measurements suggest that extensive air showers initiated by high energy cosmic rays (above 1 EeV) emit signals in the microwave band of the EM spectrum caused by the collisions of the free-electrons with the atmospheric neutral molecules in the plasma produced by the passage of the shower. Such emission is isotropic and could allow the detection of air showers with 100% duty cycle and a calorimetric-like energy measurement - a significant improvement over current detection techniques. We have built a MIDAS prototype, which consists of a 4.5 m diameter antenna with a cluster of 55 feed-horns in the 4 GHz range, covering a 10^o x10^o field of view, with self-triggering capability. The details of the prototype and first results will be presented. )

  11. Muon and neutrino collimation in extensive air shower cores

    International Nuclear Information System (INIS)

    Detailed simulations of extensive air showers have been carried out with the CORSIKA program in order to evaluate the energy brought by the different shower components at ground level and transmitted underground. A special attention is given to the angular distributions and to the collimation of beams penetrating deep underground or underwater. The natural collimation of high energy particles in extensive air shower cores results mainly from the ratio between the transverse and the longitudinal momenta of secondary particles generated in the earliest interactions. This collimation is partly conserved by the high energy muons and neutrinos. It is comparable to the magnetic focusing of charged pions and kaons decaying in tunnels of suitable length after production in accelerators. Such is the case for neutrino beams of KEK J-PARC/T2K (300 km to Kamiokande), OPERA (730 km to Gran Sasso) and MINOS (735 km to Irvine Mine)

  12. Amplified radio emission from cosmic ray air showers in thunderstorms

    CERN Document Server

    Buitink, S; Asch, T; Badea, F; Bähren, L; Bekk, K; Bercuci, A; Bertaina, M; Biermann, P L; Blumer, J; Bozdog, H; Brancus, I M; Bruggemann, M; Buchholz, P; Butcher, H; Chiavassa, A; Cossavella, F; Daumiller, K; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Gemmeke, H; Ghia, P L; Glasstetter, R; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huege, T; Kampert, K H; Kolotaev, Y; Krömer, O; Kuijpers, J; Lafebre, S; Mathes, H J; Mayer, H J; Meurer, C; Milke, J; Mitrica, B; Morello, C; Navarra, G; Nehls, S; Nigl, A; Obenland, R; Oehlschläger, J; Ostapchenko, S; Over, S; Petcu, M; Petrovic, J; Pierog, T; Plewnia, S; Rebel, H; Risse, A; Roth, M; Schieler, H; Sima, O; Singh, K; Stumpert, M; Toma, G; Trinchero, G C; Ulrich, H; Van Buren, J; Walkowiak, W; Weindl, A; Wochele, J; Zabierowski, J; Zensus, J A; Zimmermann, D; Buitink, Stijn

    2007-01-01

    Cosmic ray air showers produce radio emission, consisting in large part of geosynchrotron emission. Since the radiation mechanism is based on particle acceleration, the atmospheric electric field can play an important role. Especially inside thunderclouds large electric fields can be present. We examine the contribution of an electric field to the emission mechanism theoretically and experimentally. Two mechanisms of amplification of radio emission are considered: the acceleration radiation of the shower particles and the radiation from the current that is produced by ionization electrons moving in the electric field. We selected and evaluated LOPES data recorded during thunderstorms, periods of heavy cloudiness and periods of cloudless weather. We find that during thunderstorms the radio emission can be strongly enhanced. No amplified pulses were found during periods of cloudless sky or heavy cloudiness, suggesting that the electric field effect for radio air shower measurements can be safely ignored during ...

  13. Monte Carlo simulations of air showers in atmospheric electric fields

    CERN Document Server

    Buitink, S; Falcke, H; Heck, D; Kuijpers, J

    2009-01-01

    The development of cosmic ray air showers can be influenced by atmospheric electric fields. Under fair weather conditions these fields are small, but the strong fields inside thunderstorms can have a significant effect on the electromagnetic component of a shower. Understanding this effect is particularly important for radio detection of air showers, since the radio emission is produced by the shower electrons and positrons. We perform Monte Carlo simulations to calculate the effects of different electric field configurations on the shower development. We find that the electric field becomes important for values of the order of 1 kV/cm. Not only can the energy distribution of electrons and positrons change significantly for such field strengths, it is also possible that runaway electron breakdown occurs at high altitudes, which is an important effect in lightning initiation.

  14. Probing the radio emission from air showers with polarization measurements

    CERN Document Server

    ,

    2014-01-01

    The emission of radio waves from air showers has been attributed to the so-called geomagnetic emission process. At frequencies around 50 MHz this process leads to coherent radiation which can be observed with rather simple setups. The direction of the electric field induced by this emission process depends only on the local magnetic field vector and on the incoming direction of the air shower. We report on measurements of the electric field vector where, in addition to this geomagnetic component, another component has been observed which cannot be described by the geomagnetic emission process. The data provide strong evidence that the other electric field component is polarized radially with respect to the shower axis, in agreement with predictions made by Askaryan who described radio emission from particle showers due to a negative charge-excess in the front of the shower. Our results are compared to calculations which include the radiation mechanism induced by this charge-excess process.

  15. Construction of a cosmic ray air shower telescope

    Science.gov (United States)

    Ng, L. K.; Chan, S. K.

    1985-01-01

    The telescope under construction is mainly for the purpose of locating the arrival directions of energetic particles and quanta which generate air showers of sizes 10 to the 5th power to 10 to the 6th power. Both fast timing method and visual track method are incorporated in determining the arrival directions. The telescope is composed of four stations using scintillators and neon flash tubes as detectors. The system directional resolution is better than 1.5 deg.

  16. The QCD Black Disk Limit in Cosmic Ray Air Showers

    OpenAIRE

    Drescher, H. J.

    2004-01-01

    We discuss particle production in the high energy limit of QCD. Due to a large gluon density, the interaction reaches the black disk limit and the projectile is resolved into its partonic structure at the saturation scale. This leads to suppression of forward particle production and hereby to a faster absorption of cosmic ray air showers. This property is most suitable for the distinction of evolution scenarios for the saturation scale, e.g. fixed and running coupling BFKL, the latter of whic...

  17. Measurement of Radio Emission from Extensive Air Showers with LOPES

    OpenAIRE

    Hoerandel, J. R.; Collaboration, for the LOPES

    2009-01-01

    A new method is explored to detect extensive air showers: the measurement of radio waves emitted during the propagation of the electromagnetic shower component in the magnetic field of the Earth. Recent results of the pioneering experiment LOPES are discussed. It registers radio signals in the frequency range between 40 and 80 MHz. The intensity of the measured radio emission is investigated as a function of different shower parameters, such as shower energy, angle of incidence, and distance ...

  18. Synchrotron Radiation at Radio Frequencies from Cosmic Ray Air Showers

    OpenAIRE

    Suprun, Denis A.; Gorham, Peter W.; Rosner, Jonathan L.

    2002-01-01

    We review some of the properties of extensive cosmic ray air showers and describe a simple model of the radio-frequency radiation generated by shower electrons and positrons as they bend in the Earth's magnetic field. We perform simulations by calculating the trajectory and radiation of a few thousand charged shower particles. The results are then transformed to predict the strength and polarization of the electromagnetic radiation emitted by the whole shower.

  19. Ordered structure of the directions of arrival of E0 ≅ 5 x 1017 eV cosmic rays according to data from the Yakutsk array for recording extensive air showers

    International Nuclear Information System (INIS)

    Results are presented that were obtained by analyzing arrival directions for cosmic rays recorded by the Yakutsk array between 1974 and 2001 in the energy range E0 = 1017.6-17.9 eV for zenith angles in the region θ ≤ 53 deg. It is shown that their flux consists of two components - an isotropic (about 75%) and a cluster (about 25%) one - that are characterized by sharply different degrees of anisotropy. At E0 1017.7-17.8 eV, the observed showers are found to be strongly correlated with the Supergalaxy plane

  20. Antennas for the Detection of Radio Emission Pulses from Cosmic-Ray induced Air Showers at the Pierre Auger Observatory

    CERN Document Server

    Abreu, P; Ahlers, M; Ahn, E J; Albuquerque, I F M; Allard, D; Allekotte, I; Allen, J; Allison, P; Almela, A; Castillo, J Alvarez; Alvarez-Muñiz, J; Batista, R Alves; Ambrosio, M; Aminaei, A; Anchordoqui, L; Andringa, S; Antičić, T; Aramo, C; Arganda, E; Arqueros, F; Asorey, H; Assis, P; Aublin, J; Ave, M; Avenier, M; Avila, G; Badescu, A M; Balzer, M; Barber, K B; Barbosa, A F; Bardenet, R; Barroso, S L C; Baughman, B; Bäuml, J; Baus, C; Beatty, J J; Becker, K H; Bellétoile, A; Bellido, J A; BenZvi, S; Berat, C; Bertou, X; Biermann, P L; Billoir, P; Blanco, F; Blanco, M; Bleve, C; Blümer, H; Boh\\'{čová, M; Boncioli, D; Bonifazi, C; Bonino, R; Borodai, N; Brack, J; Brancus, I; Brogueira, P; Brown, W C; Bruijn, R; Buchholz, P; Bueno, A; Buroker, L; Burton, R E; Caballero-Mora, K S; Caccianiga, B; Caramete, L; Caruso, R; Castellina, A; Catalano, O; Cataldi, G; Cazon, L; Cester, R; Chauvin, J; Cheng, S H; Chiavassa, A; Chinellato, J A; Diaz, J Chirinos; Chudoba, J; Cilmo, M; Clay, R W; Cocciolo, G; Collica, L; Coluccia, M R; Conceição, R; Contreras, F; Cook, H; Cooper, M J; Coppens, J; Cordier, A; Coutu, S; Covault, C E; Creusot, A; Criss, A; Cronin, J; Curutiu, A; Dagoret-Campagne, S; Dallier, R; Daniel, B; Dasso, S; Daumiller, K; Dawson, B R; de Almeida, R M; De Domenico, M; De Donato, C; de Jong, S J; De La Vega, G; Junior, W J M de Mello; Neto, J R T de Mello; De Mitri, I; de Souza, V; de Vries, K D; del Peral, L; del Río, M; Deligny, O; Dembinski, H; Dhital, N; Di Giulio, C; Castro, M L Díaz; Diep, P N; Diogo, F; Dobrigkeit, C; Docters, W; D'Olivo, J C; Dong, P N; Dorofeev, A; Anjos, J C dos; Dova, M T; D'Urso, D; Dutan, I; Ebr, J; Engel, R; Erdmann, M; Escobar, C O; Espadanal, J; Etchegoyen, A; Luis, P Facal San; Falcke, H; Farrar, G; Fauth, A C; Fazzini, N; Ferguson, A P; Fick, B; Figueira, J M; Filevich, A; Filipčič, A; Fliescher, S; Fracchiolla, C E; Fraenkel, E D; Fratu, O; Fröhlich, U; Fuchs, B; Gaior, R; Gamarra, R F; Gambetta, S; García, B; Roca, S T Garcia; Garcia-Gamez, D; Garcia-Pinto, D; Bravo, A Gascon; Gemmeke, H; Ghia, P L; Giller, M; Gitto, J; Glass, H; Gold, M S; Golup, G; Albarracin, F Gomez; Berisso, M Gómez; Vitale, P F Gómez; Gonçalves, P; Gonzalez, J G; Gookin, B; Gorgi, A; Gouffon, P; Grashorn, E; Grebe, S; Griffith, N; Grigat, M; Grillo, A F; Guardincerri, Y; Guarino, F; Guedes, G P; Hansen, P; Harari, D; Harrison, T A; Harton, J L; Haungs, A; Hebbeker, T; Heck, D; Herve, A E; Hojvat, C; Hollon, N; Holmes, V C; Homola, P; Hörandel, J R; Horvath, P; Hrabovský, M; Huber, D; Huege, T; Insolia, A; Ionita, F; Italiano, A; Jansen, S; Jarne, C; Jiraskova, S; Josebachuili, M; Kadija, K; Kampert, K H; Karhan, P; Kasper, P; Katkov, I; Kégl, B; Keilhauer, B; Keivani, A; Kelley, J L; Kemp, E; Kieckhafer, R M; Klages, H O; Kleifges, M; Kleinfeller, J; Knapp, J; Koang, D -H; Kotera, K; Krohm, N; Krömer, O; Kruppke-Hansen, D; Kuempel, D; Kulbartz, J K; Kunka, N; La Rosa, G; Lachaud, C; LaHurd, D; Latronico, L; Lauer, R; Lautridou, P; Coz, S Le; Leão, M S A B; Lebrun, D; Lebrun, P; de Oliveira, M A Leigui; Letessier-Selvon, A; Lhenry-Yvon, I; Link, K; López, R; Agüera, A Lopez; Louedec, K; Bahilo, J Lozano; Lu, L; Lucero, A; Ludwig, M; Lyberis, H; Maccarone, M C; Macolino, C; Maldera, S; Maller, J; Mandat, D; Mantsch, P; Mariazzi, A G; Marin, J; Marin, V; Maris, I C; Falcon, H R Marquez; Marsella, G; Martello, D; Martin, L; Martinez, H; Bravo, O Martínez; Martraire, D; Meza, J J Masías; Mathes, H J; Matthews, J; Matthews, J A J; Matthiae, G; Maurel, D; Maurizio, D; Mazur, P O; Medina-Tanco, G; Melissas, M; Melo, D; Menichetti, E; Menshikov, A; Mertsch, P; Meurer, C; Meyhandan, R; Mićanović, S; Micheletti, M I; Minaya, I A; Miramonti, L; Molina-Bueno, L; Mollerach, S; Monasor, M; Ragaigne, D Monnier; Montanet, F; Morales, B; Morello, C; Moreno, E; Moreno, J C; Mostafá, M; Moura, C A; Muller, M A; Müller, G; Münchmeyer, M; Mussa, R; Navarra, G; Navarro, J L; Navas, S; Necesal, P; Nellen, L; Nelles, A; Neuser, J; Nhung, P T; Niechciol, M; Niemietz, L; Nierstenhoefer, N; Nitz, D; Nosek, D; Nožka, L; Oehlschläger, J; Olinto, A; Ortiz, M; Pacheco, N; Selmi-Dei, D Pakk; Palatka, M; Pallotta, J; Palmieri, N; Parente, G; Parizot, E; Parra, A; Pastor, S; Paul, T; Pech, M; Pȩkala, J; Pelayo, R; Pepe, I M; Perrone, L; Pesce, R; Petermann, E; Petrera, S; Petrolini, A; Petrov, Y; Pfendner, C; Piegaia, R; Pierog, T; Pieroni, P; Pimenta, M; Pirronello, V; Platino, M; Plum, M; Ponce, V H; Pontz, M; Porcelli, A; Privitera, P; Prouza, M; Quel, E J; Querchfeld, S; Rautenberg, J; Ravel, O; Ravignani, D; Revenu, B; Ridky, J; Riggi, S; Risse, M; Ristori, P; Rivera, H; Rizi, V; Roberts, J; de Carvalho, W Rodrigues; Rodriguez, G; Cabo, I Rodriguez; Martino, J Rodriguez; Rojo, J Rodriguez; Rodríguez-Frías, M D; Ros, G; Rosado, J; Rossler, T; Roth, M; Rouillé-d'Orfeuil, B; Roulet, E; Rovero, A C; Rühle, C; Saftoiu, A; Salamida, F; Salazar, H; Greus, F Salesa; Salina, G; Sánchez, F; Santo, C E; Santos, E; Santos, E M; Sarazin, F; Sarkar, B; Sarkar, S; Sato, R; Scharf, N; Scherini, V; Schieler, H; Schiffer, P; Schmidt, A; Scholten, O; Schoorlemmer, H; Schovancova, J; Schovánek, P; Schröder, F; Schulte, S; Schuster, D; Sciutto, S J; Scuderi, M; Segreto, A; Settimo, M; Shadkam, A; Shellard, R C; Sidelnik, I; Sigl, G; Lopez, H H Silva; Sima, O; Śmia\\lkowski, A; Šmída, R; Snow, G R; Sommers, P; Sorokin, J; Spinka, H; Squartini, R; Srivastava, Y N; Stanic, S; Stapleton, J; Stasielak, J; Stephan, M; Stutz, A; Suarez, F; Suomijärvi, T; Supanitsky, A D; Šuša, T; Sutherland, M S; Swain, J; Szadkowski, Z; Szuba, M; Tapia, A; Tartare, M; Taşcău, O; Tcaciuc, R; Thao, N T; Thomas, D; Tiffenberg, J; Timmermans, C; Tkaczyk, W; Peixoto, C J Todero; Toma, G; Tomankova, L; Tomé, B; Tonachini, A; Travnicek, P; Tridapalli, D B; Tristram, G; Trovato, E; Tueros, M; Ulrich, R; Unger, M; Urban, M; Galicia, J F Valdés; Valiño, I; Valore, L; van Aar, G; Berg, A M van den; van Vliet, A; Varela, E; Cárdenas, B Vargas; Vázquez, J R; Vázquez, R A; Veberič, D; Verzi, V; Vicha, J; Videla, M; Villaseñor, L; Wahlberg, H; Wahrlich, P; Wainberg, O; Walz, D; Watson, A A; Weber, M; Weidenhaupt, K; Weindl, A; Werner, F; Westerhoff, S; Whelan, B J; Widom, A; Wieczorek, G; Wiencke, L; Wilczyńska, B; Wilczyński, H; Will, M; Williams, C; Winchen, T; Wommer, M; Wundheiler, B; Yamamoto, T; Yapici, T; Younk, P; Yuan, G; Yushkov, A; Garcia, B Zamorano; Zas, E; Zavrtanik, D; Zavrtanik, M; Zaw, I; Zepeda, A; Zhou, J; Zhu, Y; Silva, M Zimbres; Ziolkowski, M; Charrier, D; Denis, L; Hilgers, G; Mohrmann, L; Philipps, B; Seeger, O

    2012-01-01

    The Pierre Auger Observatory is exploring the potential of the radio detection technique to study extensive air showers induced by ultra-high energy cosmic rays. The Auger Engineering Radio Array (AERA) addresses both technological and scientific aspects of the radio technique. A first phase of AERA has been operating since September 2010 with detector stations observing radio signals at frequencies between 30 and 80 MHz. In this paper we present comparative studies to identify and optimize the antenna design for the final configuration of AERA consisting of 160 individual radio detector stations. The transient nature of the air shower signal requires a detailed description of the antenna sensor. As the ultra-wideband reception of pulses is not widely discussed in antenna literature, we review the relevant antenna characteristics and enhance theoretical considerations towards the impulse response of antennas including polarization effects and multiple signal reflections. On the basis of the vector effective l...

  1. Circular polarization of radio emission from air showers probes atmospheric electric fields in thunderclouds.

    Science.gov (United States)

    Gia Trinh, Thi Ngoc; Scholten, Olaf; Buitink, Stijn; Corstanje, Arthur; Ebert, Ute; Enriquez, Emilio; Falcke, Heino; Horandel, Jörg R.; Nelles, Anna; Schellart, Pim; Rachen, Jorg; Rossetto, Laura; Rutjes, Casper; ter Veen, Sander; Thoudam, Satyendra

    2016-04-01

    When a high-energy cosmic-ray particle enters the upper layer of the atmosphere, it generates many secondary high-energy particles and forms a cosmic-ray-induced air shower. In the leading plasma of this shower electric currents are induced that emit electromagnetic radiation. These radio waves can be detected with LOw-Frequency ARray (LOFAR) radio telescope. Events have been collected under fair-weather conditions as well as under atmospheric conditions where thunderstorms occur. For the events under the fair weather conditions the emission process is well understood by present models. For the events measured under the thunderstorm conditions, we observe a large fraction of the circular polarization near the core of the shower which is not shown in the events under the fair-weather conditions. This can be explained by the change of direction of the atmospheric electric fields with altitude. Therefore, measuring the circular polarization of radio emission from cosmic ray extensive air showers during the thunderstorm conditions helps to have a better understanding about the structure of atmospheric electric fields in the thunderclouds.

  2. Reconstruction of inclined air showers detected with the Pierre Auger Observatory

    International Nuclear Information System (INIS)

    We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than 60° detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory

  3. Reconstruction of inclined air showers detected with the Pierre Auger Observatory

    Energy Technology Data Exchange (ETDEWEB)

    Aab, Alexander; et al.

    2014-08-08

    We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than 60° detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory.

  4. Reconstruction of inclined air showers detected with the Pierre Auger Observatory

    CERN Document Server

    Aab, A; Aglietta, M; Ahlers, M; Ahn, E J; Samarai, I Al; Albuquerque, I F M; Allekotte, I; Allen, J; Allison, P; Almela, A; Castillo, J Alvarez; Alvarez-Muñiz, J; Batista, R Alves; Ambrosio, M; Aminaei, A; Anchordoqui, L; Andringa, S; Aramo, C; Arqueros, F; Asorey, H; Assis, P; Aublin, J; Ave, M; Avenier, M; Avila, G; Badescu, A M; Barber, K B; Bäuml, J; Baus, C; Beatty, J J; Becker, K H; Bellido, J A; Berat, C; Bertou, X; Biermann, P L; Billoir, P; Blanco, F; Blanco, M; Bleve, C; Blümer, H; Boháčová, M; Boncioli, D; Bonifazi, C; Bonino, R; Borodai, N; Brack, J; Brancus, I; Brogueira, P; Brown, W C; Buchholz, P; Bueno, A; Buscemi, M; Caballero-Mora, K S; Caccianiga, B; Caccianiga, L; Candusso, M; Caramete, L; Caruso, R; Castellina, A; Cataldi, G; Cazon, L; Cester, R; Chavez, A G; Cheng, S H; Chiavassa, A; Chinellato, J A; Chudoba, J; Cilmo, M; Clay, R W; Cocciolo, G; Colalillo, R; Collica, L; Coluccia, M R; Conceição, R; Contreras, F; Cooper, M J; Coutu, S; Covault, C E; Criss, A; Cronin, J; Curutiu, A; Dallier, R; Daniel, B; Dasso, S; Daumiller, K; Dawson, B R; de Almeida, R M; De Domenico, M; de Jong, S J; Neto, J R T de Mello; De Mitri, I; de Oliveira, J; de Souza, V; del Peral, L; Deligny, O; Dembinski, H; Dhital, N; Di Giulio, C; Di Matteo, A; Diaz, J C; Castro, M L D\\'\\iaz; Diep, P N; Diogo, F; Dobrigkeit, C; Docters, W; D'Olivo, J C; Dong, P N; Dorofeev, A; Hasankiadeh, Q Dorosti; Dova, M T; Ebr, J; Engel, R; Erdmann, M; Erfani, M; Escobar, C O; Espadanal, J; Etchegoyen, A; Luis, P Facal San; Falcke, H; Fang, K; Farrar, G; Fauth, A C; Fazzini, N; Ferguson, A P; Fernandes, M; Fick, B; Figueira, J M; Filevich, A; Filipčič, A; Fox, B D; Fratu, O; Fröhlich, U; Fuchs, B; Fuji, T; Gaior, R; Garc\\'\\ia, B; Roca, S T Garcia; Garcia-Gamez, D; Garcia-Pinto, D; Garilli, G; Bravo, A Gascon; Gate, F; Gemmeke, H; Ghia, P L; Giaccari, U; Giammarchi, M; Giller, M; Glaser, C; Glass, H; Albarracin, F Gomez; Berisso, M Gómez; Vitale, P F Gómez; Gonçalves, P; Gonzalez, J G; Gookin, B; Gorgi, A; Gorham, P; Gouffon, P; Grebe, S; Griffith, N; Grillo, A F; Grubb, T D; Guardincerri, Y; Guarino, F; Guedes, G P; Hansen, P; Harari, D; Harrison, T A; Harton, J L; Haungs, A; Hebbeker, T; Heck, D; Heimann, P; Herve, A E; Hill, G C; Hojvat, C; Hollon, N; Holt, E; Homola, P; Hörandel, J R; Horvath, P; Hrabovský, M; Huber, D; Huege, T; Insolia, A; Isar, P G; Islo, K; Jandt, I; Jansen, S; Jarne, C; Josebachuili, M; Kääpä, A; Kambeitz, O; Kampert, K H; Kasper, P; Katkov, I; Kégl, B; Keilhauer, B; Keivani, A; Kemp, E; Kieckhafer, R M; Klages, H O; Kleifges, M; Kleinfeller, J; Krause, R; Krohm, N; Krömer, O; Kruppke-Hansen, D; Kuempel, D; Kunka, N; La Rosa, G; LaHurd, D; Latronico, L; Lauer, R; Lauscher, M; Lautridou, P; Coz, S Le; Leão, M S A B; Lebrun, D; Lebrun, P; de Oliveira, M A Leigui; Letessier-Selvon, A; Lhenry-Yvon, I; Link, K; López, R; Agëra, A Lopez; Louedec, K; Bahilo, J Lozano; Lu, L; Lucero, A; Ludwig, M; Lyberis, H; Maccarone, M C; Malacari, M; Maldera, S; Maller, J; Mandat, D; Mantsch, P; Mariazzi, A G; Marin, V; Mariş, I C; Marsella, G; Martello, D; Martin, L; Martinez, H; Bravo, O Mart\\'\\inez; Martraire, D; Meza, J J Mas\\'\\ias; Mathes, H J; Mathys, S; Matthews, A J; Matthews, J; Matthiae, G; Maurel, D; Maurizio, D; Mayotte, E; Mazur, P O; Medina, C; Medina-Tanco, G; Melissas, M; Melo, D; Menichetti, E; Menshikov, A; Messina, S; Meyhandan, R; Mićanović, S; Micheletti, M I; Middendorf, L; Minaya, I A; Miramonti, L; Mitrica, B; Molina-Bueno, L; Mollerach, S; Monasor, M; Ragaigne, D Monnier; Montanet, F; Morello, C; Moreno, J C; Mostafá, M; Moura, C A; Muller, M A; Müller, G; Münchmeyer, M; Mussa, R; Navarra, G; Navas, S; Necesal, P; Nellen, L; Nelles, A; Neuser, J; Newton, D; Niechciol, M; Niemietz, L; Niggemann, T; Nitz, D; Nosek, D; Novotny, V; Nožka, L; Ochilo, L; Olinto, A; Oliveira, M; Olmos-Gilbaja, V M; Ortiz, M; Pacheco, N; Selmi-Dei, D Pakk; Palatka, M; Pallotta, J; Palmieri, N; Papenbreer, P; Parente, G; Parra, A; Pastor, S; Paul, T; Pech, M; Pȩkala, J; Pelayo, R; Pepe, I M; Perrone, L; Pesce, R; Petermann, E; Peters, C; Petrera, S; Petrolini, A; Petrov, Y; Piegaia, R; Pierog, T; Pieroni, P; Pimenta, M; Pirronello, V; Platino, M; Plum, M; Porcelli, A; Porowski, C; Privitera, P; Prouza, M; Purrello, V; Quel, E J; Querchfeld, S; Quinn, S; Rautenberg, J; Ravel, O; Ravignani, D; Revenu, B; Ridky, J; Riggi, S; Risse, M; Ristori, P; Rizi, V; Roberts, J; de Carvalho, W Rodrigues; Cabo, I Rodriguez; Fernandez, G Rodriguez; Rojo, J Rodriguez; Rodr\\'\\iguez-Fr\\'\\ias, M D; Ros, G; Rosado, J; Rossler, T; Roth, M; Roulet, E; Rovero, A C; Rühle, C; Saffi, S J; Saftoiu, A; Salamida, F; Salazar, H; Greus, F Salesa; Salina, G; Sánchez, F; Sanchez-Lucas, P; Santo, C E; Santos, E; Santos, E M; Sarazin, F; Sarkar, B; Sarmento, R; Sato, R; Scharf, N; Scherini, V; Schieler, H; Schiffer, P; Schmidt, A; Scholten, O; Schoorlemmer, H; Schovánek, P; Schulz, A; Schulz, J; Sciutto, S J; Segreto, A; Settimo, M; Shadkam, A; Shellard, R C; Sidelnik, I; Sigl, G; Sima, O; kowski, A Śmiał; Šm\\'\\ida, R; Snow, G R; Sommers, P; Sorokin, J; Squartini, R; Srivastava, Y N; Stanič, S; Stapleton, J; Stasielak, J; Stephan, M; Stutz, A; Suarez, F; Suomijärvi, T; Supanitsky, A D; Sutherland, M S; Swain, J; Szadkowski, Z; Szuba, M; Taborda, O A; Tapia, A; Tartare, M; Thao, N T; Theodoro, V M; Tiffenberg, J; Timmermans, C; Peixoto, C J Todero; Toma, G; Tomankova, L; Tomé, B; Tonachini, A; Elipe, G Torralba; Machado, D Torres; Travnicek, P; Trovato, E; Tueros, M; Ulrich, R; Unger, M; Urban, M; Galicia, J F Valdés; Valiño, I; Valore, L; van Aar, G; Berg, A M van den; van Velzen, S; van Vliet, A; Varela, E; Cárdenas, B Vargas; Varner, G; Vázquez, J R; Vázquez, R A; Veberič, D; Verzi, V; Vicha, J; Videla, M; Villaseñor, L; Vlcek, B; Vorobiov, S; Wahlberg, H; Wainberg, O; Walz, D; Watson, A A; Weber, M; Weidenhaupt, K; Weindl, A; Werner, F; Whelan, B J; Widom, A; Wiencke, L; Wilczyńska, B; Wilczyński, H; Will, M; Williams, C; Winchen, T; Wittkowski, D; Wundheiler, B; Wykes, S; Yamamoto, T; Yapici, T; Younk, P; Yuan, G; Yushkov, A; Zamorano, B; Zas, E; Zavrtanik, D; Zavrtanik, M; Zaw, I; Zepeda, A; Zhou, J; Zhu, Y; Silva, M Zimbres; Ziolkowski, M

    2014-01-01

    We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than $60^\\circ$ detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory.

  5. Receiver system for radio observation of high-energy cosmic ray air showers and its behaviour in self trigger mode

    International Nuclear Information System (INIS)

    The observation of high-energy cosmic rays is carried out by indirect measurements. Thereby the primary cosmic particle enters into the earth's atmosphere and generates a cosmic ray air shower by interactions with the air molecules. The secondary particles arriving at ground level are detected with particle detector arrays. The fluorescence light from the exited nitrogen molecules along the shower axis is observed with reflector telescopes in the near-ultraviolet range. In addition to these well-established detection methods, the radio observation of the geosynchrotron emission from cosmic ray air showers is investigated at present as a new observation method. Geosynchrotron emission is generated by the acceleration of the relativistic electron-positron-pairs contained in the air shower by Lorentz forces in the earth's magnetic field. At ground level this causes a single pulse of the electric field strength with a continuous frequency spectrum ranging from a few MHz to above 100 MHz. In this work, a suitable receiver concept is developed based on the signal properties of the geosynchrotron emission and the analysis of the superposed noise and radio frequency interferences. As the required receiver system was not commercially available, it was designed in the framework of this work and realised as system including the antenna, the receiver electronics and suitable data acquisition equipment. In this concept considerations for a large scale radio detector array have already been taken into account, like low power consumption to enable solar power supply and cost effectiveness. The result is a calibrated, multi-channel, digital wideband receiver for the complete range from 40 MHz to 80 MHz. Its inherent noise and RFI suppression essentially results from the antenna directional characteristic and frequency selectivity and allows effective radio observation of cosmic ray air showers also in populated environment. Several units of this receiver station have been deployed

  6. Arrival time distributions of electrons in air showers with primary energies above 10 (18)eV observed at 900m above sea level

    Science.gov (United States)

    Kakimoto, F.; Tsuchimoto, I.; Enoki, T.; Suga, K.; Nishi, K.

    1985-01-01

    Detection of air showers with primary energies above 10 to the 19th power eV with sufficient statistics is extremely important in an astrophysical aspect related to the Greisen cut off and the origin of such high energy cosmic rays. Recently, a method is proposed to observe such giant air showers by measuring the arrival time distributions of air-shower particles at large core distances with a mini array. Experiments to measure the arrival time distributions of muons were started in 1981 and those of electrons in early 1983 in the Akeno air-shower array (930 gcm cm squared atmospheric depth, 900m above sea level). During the time of observation, the detection area of the Akeno array was expanded from 1 sq km to sq km in 1982 and to 20 sq km in 1984. Now the arrival time distribution of electrons and muons can be measured for showers with primary energies above 1019eV at large core distances.

  7. Impact of Uncertainties in Hadron Production on Air-Shower Predictions

    OpenAIRE

    Pierog, T.; Engel, R.; Heck, D.

    2006-01-01

    At high energy, cosmic rays can only be studied by measuring the extensive air showers they produce in the atmosphere of the Earth. Although the main features of air showers can be understood within a simple model of successive interactions, detailed simulations and a realistic description of particle production are needed to calculate observables relevant to air shower experiments. Currently hadronic interaction models are the main source of uncertainty of such simulations. We will study the...

  8. Atmospheric multiple scattering of fluorescence and Cherenkov light emitted by extensive air showers

    OpenAIRE

    Pekala, J.; Homola, P.; Wilczynska, B.; Wilczynski, H.

    2009-01-01

    Atmospheric scattering of light emitted by an air shower not only attenuates direct fluorescence light from the shower, but also contributes to the observed shower light. So far only direct and singly-scattered Cherenkov photons have been taken into account in routine analyses of the observed optical image of air showers. In this paper a Monte Carlo method of evaluating the contribution of multiply scattered light to the optical air shower image is presented, as well as results of simulations...

  9. Transition effect of extensive air showers in thick scintillators

    International Nuclear Information System (INIS)

    Transition effect of extensive air showers has been measured by means of the ''Kover'' facility of the Baksan neutrino laboratory. The transition effect represents the ratio of ''scintillation'' particle density detected with detectors and particle density under the facility concrete roof (21 gxcm-2). Measurement results are compared with data obtained by means of the program of electron-photon cascade gaming. Good agreement of experimental and calculational data has been obtained. It follows from the data in the paper that the transition effect for one scintillator in the absence of roof can be produced by the gaming rather reliably

  10. Air shower universality from 1014 to 1022 eV

    International Nuclear Information System (INIS)

    Scaling properties of nuclei- and photon-initiated air showers are examined in wide primary energy range (1014 ÷ 1022 eV) taking into account Landau-Pomeranchuk-Migdal and geomagnetic field effects. It is shown that the invariance in lateral distribution and also the universal dependence between shower age and root mean square radius of electron component exist up to the highest energies. The implications of shower universality for reanalysis, crosschecking and validation of the results of different experiments together with decreasing of the influence of hadronic model uncertainties are discussed in detail.

  11. The longitudinal thickness of air-shower fronts

    Science.gov (United States)

    Clay, R. W.; Brissenden, R. J. V.; Elton, S. D.; Wild, N. R.

    1985-01-01

    Linsely (1983) has proposed a technique for the detection and analysis of air showers at large distances from the shower axis based on a measurement of the shower front thickness and the assumption that this thickness is closely related to the core distance. Some of the problems involved with realizing such a technique were investigated, and some related observations are reported. The practical problems of how consistent the measurements of the shower front would be, how one would use the measurement, and how the rate of triggered events would depend on the minimum pulse width required are studied.

  12. Considerations on the microwave radiation emitted by extended air showers

    CERN Document Server

    Conti, E

    2015-01-01

    The emission of microwave radiation by extended air showers produced by high energy cosmic rays has been investigated for more than half a century. We discuss the expected emitted power as a function of the cosmic ray energy and of the microwave frequency, for both coherent and incoherent emission mechanisms. We show that the available experimental data are not sufficient to clearly identify the emission mechanisms and quantify the emission yield. We infer that the bremsstralhung radiation emission could be exploited for the detection of astronomical $\\gamma$-rays with energy above 10 GeV in the 1-10 GHz frequency range, and propose an experimental scheme to verify such idea.

  13. Reconstruction of muon height of production in Extensive Air Showers

    International Nuclear Information System (INIS)

    An attempt has been made to select muons in Extensive Air Showers (EAS) by means of tracking telescopes and reconstruct their apparent height of production along the shower axis. By this way a reconstruction of shower longitudinal development in the Earth atmosphere can be obtained. Results indicate that the only information of muon arrival direction is not enough for the correct reconstruction of shower longitudinal development, mainly because of the distorting effect of the Earth geomagnetic field and multiple coulomb scattering by air nuclei

  14. Large muon tracking detector in the air shower experiment KASCADE

    International Nuclear Information System (INIS)

    A large area Streamer Tube (ST) detector, located within the KASCADE experiment, has been built with the aim to identify muons from extensive air showers (EAS) by track measurement under more than 18 r.l. shielding. 1000 ST detectors of 4 m length have been built and tested. Extensive tests led to many improvements in the detector construction. The construction of the whole detector together with its electronic is presented. The methods of precise determination of detector geometry as well as tools for detector angular resolution derivation are discussed. (orig.)

  15. Characteristics of superpower extensive air showers at the sea level

    International Nuclear Information System (INIS)

    The experimental data on the extensive air showers (EAS) have been examined at the sea level. The experiment has been staged at the Yakutsk EAS installation. The EAS spectrum has been determined by the number of particles at the 1,020 gxcm-2 atmospheric depth, taking into account the fluctuations of the spatial distribution function. Equal intensity lines have been produced from the EAS spectrum. More exactly the intensities of the showers have been computed when the particles number exceeds 4x108

  16. Longitudinal development of extensive air showers: hybrid code SENECA and full Monte Carlo

    CERN Document Server

    Ortiz, J A; De Souza, V; Ortiz, Jeferson A.; Tanco, Gustavo Medina

    2004-01-01

    New experiments, exploring the ultra-high energy tail of the cosmic ray spectrum with unprecedented detail, are exerting a severe pressure on extensive air hower modeling. Detailed fast codes are in need in order to extract and understand the richness of information now available. Some hybrid simulation codes have been proposed recently to this effect (e.g., the combination of the traditional Monte Carlo scheme and system of cascade equations or pre-simulated air showers). In this context, we explore the potential of SENECA, an efficient hybrid tridimensional simulation code, as a valid practical alternative to full Monte Carlo simulations of extensive air showers generated by ultra-high energy cosmic rays. We extensively compare hybrid method with the traditional, but time consuming, full Monte Carlo code CORSIKA which is the de facto standard in the field. The hybrid scheme of the SENECA code is based on the simulation of each particle with the traditional Monte Carlo method at two steps of the shower devel...

  17. Impact of Uncertainties in Hadron Production on Air-Shower Predictions

    CERN Document Server

    Pierog, T; Heck, D

    2006-01-01

    At high energy, cosmic rays can only be studied by measuring the extensive air showers they produce in the atmosphere of the Earth. Although the main features of air showers can be understood within a simple model of successive interactions, detailed simulations and a realistic description of particle production are needed to calculate observables relevant to air shower experiments. Currently hadronic interaction models are the main source of uncertainty of such simulations. We will study the effect of using different hadronic models available in CORSIKA and CONEX on extensive air shower predictions.

  18. The energy spectrum of primary cosmic rays estimated by using the arrival time spread of air shower particles

    International Nuclear Information System (INIS)

    The primary energy of cosmic rays in the energy region above 1016 eV has been studied with the use of a compact extensive air shower (EAS) array which consists of 8 scintillation counters in 200m2 area. We report on the simulation results for estimating the primary energy and its spectrum by using Linsley's method, and on the improvement of the determination accuracy of the primary energy by applying the zenith angle restricted observation of EAS muons with the new array as well as a brief description of the apparatus.

  19. Milagro: A low energy threshold extensive air shower array

    Energy Technology Data Exchange (ETDEWEB)

    Sinnis, C.

    1994-12-31

    Observations of high-energy gamma rays from astronomical sources have revolutionized our view of the cosmos. Gamma rays with energies up to {approximately}10 GeV can be observed directly with space-based instruments. Above 100 GeV the low flux of gamma rays requires one to utilize ground-based instruments. Milagro is a new type of gamma-ray detector based on water Cerenkov technology. This new design will enable to continuously observe the entire overhead sky, and be sensitive to cosmic rays with energies above {approximately}250 GeV. These attributes make Milagro an ideal detector for the study of high-energy transient phenomenon.

  20. Milagro: A low energy threshold extensive air shower array

    Science.gov (United States)

    Sinnis, Gus

    1995-07-01

    Observations of gamma-ray bursts, active galactic nuclei, and radio pulsars by CGRO have revolutionized our view of the cosmos. Sources may pop into existence for a few milliseconds never to appear again and galaxies can change their luminosity by an order of magnitude within a few days. In addition to these space-based measurements, there have been at least 2 sources detected at even higher energies, ~1 TeV, using earth-bound detectors. To date, ground-based detectors of high-energy gamma rays with energy thresholds low enough to make credible detections have all had narrow fields of view and low duty factors. While these detectors are well suited to perform detailed studies of selected sources, they can not perform surveys of the entire sky with adequate sensitivity in a reasonable amount of time. We have designed a new type of ground-based gamma-ray detector with a low energy threshold, ~250 GeV, large aperture (~1 sr), and a duty factor greater than 90%-Milagro.

  1. Light Transmission Fluctuations from Extended Air Showers Produced by Cosmic-Rays and Gamma-Rays

    Science.gov (United States)

    Taylor, Stuart

    Cosmic-ray and gamma-ray experiments that use the atmosphere as a calorimeter, such as the High Resolution Fly's Eye (HiRes) and the Telescope Array (TA), require understanding the transmission of the light from the air shower of particles produced by the cosmic-ray or gamma-ray striking the atmosphere. To better understand the scattering and transmission of light to the detectors, HiRes measures light from different calibrated sources. We compare scattered light from laser shots a few kilometers away from the two HiRes detectors with direct light from stable portable light sources placed a few meters in front of the phototubes. We use two HiRes detectors to study and isolate contributions to fluctuations of the measured light. These contributions include fluctuations in the source intensity, the night sky background, scattering and transmission of the laser beam, the phototubes and electronics, and photostatistics. N o rth Mirror Fields of View

  2. Muons in air showers at the Pierre Auger Observatory: Measurement of atmospheric production depth

    CERN Document Server

    ,

    2014-01-01

    The surface detector array of the Pierre Auger Observatory provides information about the longitudinal development of the muonic component of extensive air showers. Using the timing information from the flash analog-to-digital converter traces of surface detectors far from the shower core, it is possible to reconstruct a muon production depth distribution. We characterize the goodness of this reconstruction for zenith angles around 60 deg. and different energies of the primary particle. From these distributions we define X(mu)max as the depth along the shower axis where the production of muons reaches maximum. We explore the potentiality of X(mu)max as a useful observable to infer the mass composition of ultrahigh-energy cosmic rays. Likewise, we assess its ability to constrain hadronic interaction models.

  3. Probing atmospheric electric fields in thunderstorms through radio emission from cosmic-ray induced air showers

    NARCIS (Netherlands)

    Schellart, P.; Trinh, T.N.G.; Buitink, S.; Corstanje, A.; Enriquez, J.E; Falcke, H.; Bentum, M.J.

    2015-01-01

    We present measurements of radio emission from cosmic ray air showers that took place during thunder storms. The intensity and polarization patterns of these air showers are radically different from those measured during fair-weather conditions. With the use of a simple two-layer model for the atmos

  4. Data from accelerator-based experiments of relevance to the air shower observations

    Directory of Open Access Journals (Sweden)

    Itow Yoshitaka

    2013-06-01

    Full Text Available Implications of air shower of ultra high energy cosmic rays (UHECRs need precise knowledge on hadronic interactions at very high energy. From this point of view recent LHC data have great impacts on the UHECR observation. Here various data from accelerator experiments including recent LHC data, of relevance to the air shower measurements, are briefly overviewed.

  5. Relation between hadronic interactions and ultra-high energy extensive air showers

    Directory of Open Access Journals (Sweden)

    Ulrich Ralf

    2015-01-01

    Full Text Available The simulation of hadronic interactions is of fundamental importance for the analysis of extensive air showers. The details of the relation between the measurement of hadronic interactions at accelerators and the impact on the air shower development is very difficult to evaluate. Several possibilities to study this relation are presented here.

  6. Macroscopic treatment of radio emission from cosmic ray air showers based on shower simulations

    NARCIS (Netherlands)

    Werner, Klaus; Scholten, Olaf

    2008-01-01

    We present a macroscopic calculation of coherent electro-magnetic radiation from air showers initiated by ultra-high energy cosmic rays, based on currents obtained from Monte Carlo simulations of air showers in a realistic geo-magnetic field. We can clearly relate the time signal to the time depende

  7. Relation between hadronic interactions and ultra-high energy extensive air showers

    Science.gov (United States)

    Ulrich, Ralf; Baus, Colin; Engel, Ralph

    2015-08-01

    The simulation of hadronic interactions is of fundamental importance for the analysis of extensive air showers. The details of the relation between the measurement of hadronic interactions at accelerators and the impact on the air shower development is very difficult to evaluate. Several possibilities to study this relation are presented here.

  8. Lateral density and arrival time distributions of Cherenkov photons in extensive air showers: a simulation study

    CERN Document Server

    Hazarika, P; Chitnis, V R; Acharya, B S; Das, G S; Singh, B B; Britto, R

    2014-01-01

    We have investigated some features of the density and arrival time distributions of Cherenkov photons in extensive air showers using different high and low energy hadronic interaction models available in the CORSIKA simulation package. We have found that, for all primary particles, their energies and hadronic interaction model combinations, the density distribution patterns of Cherenkov photons follow the negative exponential function with different coefficients and slopes depending on the type of primary particle, its energy and the type of model combination. Whereas the arrival time distribution patterns of Cherenkov photons follow the function of the form $t (r) = t_{0}e^{\\Gamma/r^{\\lambda}}$, with different values of the function parameters. Flatness of the density distribution increases with decreasing energy and increasing mass of the primary particle. The shift from the spherical shape of the arrival time distribution near the shower core increases with increasing mass of the low energy primary particl...

  9. Extensive Air Showers: From the muonic smoking guns to the hadronic backbone

    International Nuclear Information System (INIS)

    Extensive Air Showers are complex macroscopic objects initiated by single ultra-high energy particles. They are the result of millions of high energy reactions in the atmosphere and can be described as the superposition of hadronic and electromagnetic cascades. The hadronic cascade is the air shower backbone, and it is mainly made of pions. Decays of neutral pions initiate electromagnetic cascades, while the decays of charged pions produce muons which leave the hadronic core and travel many kilometers almost unaffected. Muons are smoking guns of the hadronic cascade: the energy, transverse momentum, spatial distribution and depth of production are key to reconstruct the history of the air shower. In this work, we overview the phenomenology of muons on the air shower and its relation to the hadronic cascade. We briefly review the experimental efforts to analyze muons within air showers and discuss possible paths to use this information. (authors)

  10. Extensive Air Showers: from the muonic smoking guns to the hadronic backbone

    CERN Document Server

    Cazon, L

    2013-01-01

    Extensive Air Showers are complex macroscopic objects initiated by single ultra-high energy particles. They are the result of millions of high energy reactions in the atmosphere and can be described as the superposition of hadronic and electromagnetic cascades. The hadronic cascade is the air shower backbone, and it is mainly made of pions. Decays of neutral pions initiate electromagnetic cascades, while the decays of charged pions produce muons which leave the hadronic core and travel many kilometers almost unaffected. Muons are smoking guns of the hadronic cascade: the energy, transverse momentum, spatial distribution and depth of production are key to reconstruct the history of the air shower. In this work, we overview the phenomenology of muons on the air shower and its relation to the hadronic cascade. We briefly review the experimental efforts to analyze muons within air showers and discuss possible paths to use this information.

  11. Extensive Air Showers: from the muonic smoking guns to the hadronic backbone

    Directory of Open Access Journals (Sweden)

    Cazon L.

    2013-06-01

    Full Text Available Extensive Air Showers are complex macroscopic objects initiated by single ultra-high energy particles. They are the result of millions of high energy reactions in the atmosphere and can be described as the superposition of hadronic and electromagnetic cascades. The hadronic cascade is the air shower backbone, and it is mainly made of pions. Decays of neutral pions initiate electromagnetic cascades, while the decays of charged pions produce muons which leave the hadronic core and travel many kilometers almost unaffected. Muons are smoking guns of the hadronic cascade: the energy, transverse momentum, spatial distribution and depth of production are key to reconstruct the history of the air shower. In this work, we overview the phenomenology of muons on the air shower and its relation to the hadronic cascade. We briefly review the experimental efforts to analyze muons within air showers and discuss possible paths to use this information.

  12. Radio emission of extensive air showers at microwave frequencies

    Science.gov (United States)

    Filonenko, A. D.

    2016-05-01

    It is found that the power of the incoherent radiation of ionization electrons of an extensive air shower in the frequency range of 150 GHz is more than 10-24 W/m2Hz, with the shower energy ~1018 eV at a distance of 5 km from its axis. This means that, unlike fluorescent detectors, a radio telescope with an effective area of more than 300 m2 can monitor the trajectory of showers with an energy higher than 1018 eV at any time of the day regardless of the weather. The spectrum maximum near the frequency of 150 GHz is roughly three orders of magnitude higher than the value experimentally measured in the characteristic band (~5-10 GHz).

  13. On radiofrequency component of transition radiation of extensive air shower

    International Nuclear Information System (INIS)

    The mechanism of radio emission caused by the transition radiation of the contrarily charged particles of the expensive air shower in the magnetic field of the Earth is studied for the first time. It is established that for the showers with the energy about 1022 eV the maximum stage whereof is reached at the sea level the electrical field voltage constitutes 60 μV/m MHz at the distance of 500 km from the shower axis. The spectrum intensity maximum is in the area corresponding to the atmospheric disturbances minimum (∼ 1 μHz). These conditions stimulate the formulation of the experiment on the high-energy cosmic ray radio detection, the scheme whereof is proposed in this work

  14. Depth Distribution Of The Maxima Of Extensive Air Shower

    Science.gov (United States)

    Adams, J. H.; Howell, L. W.

    2003-01-01

    Observations of the extensive air showers from space can be free from interference by low altitude clouds and aerosols if the showers develop at a sufficiently high altitude. In this paper we explore the altitude distribution of shower maxima to determine the fraction of all showers that will reach their maxima at sufficient altitudes to avoid interference from these lower atmosphere phenomena. Typically the aerosols are confined within a planetary boundary layer that extends from only 2-3 km above the Earth's surface. Cloud top altitudes extend above 15 km but most are below 4 km. The results reported here show that more than 75% of the showers that will be observed by EUSO have maxima above the planetary boundary layer. The results also show that more than 50% of the showers that occur on cloudy days have their maxima above the cloud tops.

  15. Considerations on the radio emission from extended air showers

    Science.gov (United States)

    Conti, E.; Sartori, G.

    2016-05-01

    The process of radio emission from extended air showers produced by high energy cosmic rays has reached a good level of comprehension and prediction. It has a coherent nature, so the emitted power scales quadratically with the energy of the primary particle. Recently, a laboratory measurement has revealed that an incoherent radiation mechanism exists, namely, the bremsstrahlung emission. In this paper we expound why bremsstrahlung radiation, that should be present in showers produced by ultra high energy cosmic rays, has escaped detection so far, and why, on the other side, it could be exploited, in the 1–10 GHz frequency range, to detect astronomical γ-rays. We propose an experimental scheme to verify such hypothesis, which, if correct, would deeply impact on the observational γ-ray astronomy.

  16. Implications of Ultrahigh Energy Air Showers for Physics and Astrophysics

    Science.gov (United States)

    Stecker, F. W.; White, Nicholas E. (Technical Monitor)

    2002-01-01

    The primary ultrahigh energy particles which produce giant extensive air showers in the Earth atmosphere present an intriguing mystery from two points of view: (1) How are the base particles produced with such astounding energies, eight orders of magnitude higher than those produced by the best man-made terrestrial accelerators? (2) Since they are most likely extragalactic in origin, how do they reach us from extragalactic distances without suffering the severe losses expected from interactions with the 2.7 K thermal cosmic background photons, the so called GZK effect? The answers to these questions may involve new physics: violations of special relativity, grand unification theories, and quantum gravity theories involving large extra dimensions. They may involve new astrophysical sources, "zevatrons". Or some heretofore totally unknown physics or astrophysics may hold the answer. I will discuss here the mysteries involving the production and extragalactic propagation of ultrahigh energy cosmic rays and some suggested possible solutions.

  17. Simulating radio emission from air showers with CoREAS

    CERN Document Server

    Huege, T; James, C W

    2013-01-01

    CoREAS is a Monte Carlo code for the simulation of radio emission from extensive air showers. It implements the endpoint formalism for the calculation of electromagnetic radiation directly in CORSIKA. As such, it is parameter-free, makes no assumptions on the emission mechanism for the radio signals, and takes into account the complete complexity of the electron and positron distributions as simulated by CORSIKA. In this article, we illustrate the capabilities of CoREAS with simulations carried out in different frequency ranges from tens of MHz up to GHz frequencies, and describe in particular the emission characteristics at high frequencies due to Cherenkov effects arising from the varying refractive index of the atmosphere.

  18. The "Horizon-T" Experiment: Extensive Air Showers Detection

    CERN Document Server

    Beisembaev, R U; Dalkarov, O D; Ryabov, V A; Stepanov, A V; Vildanov, N G; Vildanova, M I; Zhukov, V V; Baigarin, K A; Beznosko, D; Sadykov, T X; Suleymenov, N S

    2016-01-01

    Horizon-T is an innovative detector system constructed to study Extensive Air Showers (EAS) in the energy range above 10^16 eV coming from a wide range of zenith angles (0 - 85 degrees). The system is located at Tien Shan high-altitude Science Station of Lebedev Physical Institute of the Russian Academy of Sciences at approximately 3340 meters above the sea level. It consists of eight charged particle detection points separated by the distance up to one kilometer as well as optical detector subsystem to view the Vavilov-Cerenkov light from the EAS. The time resolution of charged particles and Vavilov-Cerenkov light photons passage of the detector system is a few ns. This level of resolution allows conducting research of atmospheric development of individual EAS.

  19. Investigation of the muon component of extensive air showers

    International Nuclear Information System (INIS)

    Investigations regarding the spatial distribution of the muons in the extensive air showers (EAS) have been carried out. The experiment has been staged at the Moscow State University complex EAS installation. The data showing the spatial distribution correlation with the s age parameter are given. The obtained functions of the muon spatial distribution are used to plot the dependence of the muon number on the electron number and to compute the distribution dispersion by the muon number while the number of electrons is fixed. The test data are compared with the sealing model-computed data. The computation results, made on the assumption, that the primary cosmic rays are composed of protons, contradict the experimental data

  20. Spatial distribution of muons in extensive air showers: experiment, calculations

    International Nuclear Information System (INIS)

    Investigations regarding the spatial distribution of the muons, possessing an energy of more than 10 GeV, have been carried out in the extensive air showers (EAS) at the sea level. The experiment has been staged at the Moscow State University complex installation. The experimental data are compared with the computations carried out for the various models of the hadronic interactions. At the same time it was supposed that the EAS were generated by the primary protons and that the value of the average transverse momentum of the secondary particles was equal to 0.4 GeV/s. It has been shown that the theoretical results are consistent with the experimental data

  1. A new radiograpic method using electromagnetic component of air shower

    Science.gov (United States)

    Taketa, A.; Okubo, S.; Tanaka, H.

    2012-12-01

    We have developed a novel radiographic method to measure the density length with electromagnetic component of air shower. Air shower produced by a primary cosmic ray consists of muon component and electromagnetic component. Electromagnetic component is consists of electron, positron and photon. The penetration power of electromagnetic component is weaker than that of muon, so soft component is suitable for small scale structure thinner than 2 kg/cm^2 equivalent to 20m thick water, like buildings and small hills. But it requires particle identification which means distinguishing muon and electromagnetic component. Particle identification can be done with strong magnets and dense detectors, but it is very hard to use that kind of detector for radiography because of their weight and cost. We established the cheap and effective method to distinguish soft component and hard component statistically. We also performed measurements in Arimura observation vault of Mt. Sakurajima, Japan. As a result of this observation, we found there is an anti-correlation between soft component flux and rainfall. If the water content of the soil became larger, the amount of absorption increases. So this result can be interpreted as detecting the increase of the water content by soft component flux. This method can be applied for the quantitive compensation of the measurement data like absolute gravitymeter data and tiltmeter data which is easy to receive turbulence by rain. It is also expected that the quantitive compensation leads to the improvement in accuracy of diastrophism measurement and the improvement in presumed accuracy of magma movement inside a volcano.

  2. Air shower simulation for WASAVIES: warning system for aviation exposure to solar energetic particles.

    Science.gov (United States)

    Sato, T; Kataoka, R; Yasuda, H; Yashiro, S; Kuwabara, T; Shiota, D; Kubo, Y

    2014-10-01

    WASAVIES, a warning system for aviation exposure to solar energetic particles (SEPs), is under development by collaboration between several institutes in Japan and the USA. It is designed to deterministically forecast the SEP fluxes incident on the atmosphere within 6 h after flare onset using the latest space weather research. To immediately estimate the aircrew doses from the obtained SEP fluxes, the response functions of the particle fluxes generated by the incidence of monoenergetic protons into the atmosphere were developed by performing air shower simulations using the Particle and Heavy Ion Transport code system. The accuracy of the simulation was well verified by calculating the increase count rates of a neutron monitor during a ground-level enhancement, combining the response function with the SEP fluxes measured by the PAMELA spectrometer. The response function will be implemented in WASAVIES and used to protect aircrews from additional SEP exposure. PMID:24344351

  3. Studying the shower front curvature of extensive air showers with the Pierre Auger Observatory

    International Nuclear Information System (INIS)

    The shape of the shower front in extensive air showers (EAS) is related to the properties of the primary cosmic ray and to the shower development in the atmosphere. In particular the radius of curvature for ultra high energy cosmic rays (above 1018 eV) can be estimated using the large statistics of events collected by the Pierre Auger Observatory. The Observatory, located in Malargue (Argentina), consists of a Surface Detector (SD) and a Fluorescence Detector (FD) that can be combined in a hybrid detection mode providing precise measurements of the geometry and the energy of the primary particle. The surface detectors sample the lateral distribution and the arrival time of particles at the ground. These information are used to study the curvature of the shower front and its dependence on shower parameters. Results and implications for the reconstruction are discussed.

  4. GRASP. Development of an event reconstruction method using a gamma ray air shower parameterisation and applications to γ-ray sources with H.E.S.S

    International Nuclear Information System (INIS)

    The H.E.S.S. experiment, with its high sensitivity and large field-of-view, is an ideal instrument to survey the Milky Way in VHE γ-rays. An accurate reconstruction of the γ-ray direction as well as a strong reduction of the hadronic background is essential for the analysis of the data. In this work a reconstruction algorithm is developed that applies a fit of pixel amplitudes to an expected image obtained from a Gamma Ray Air Shower Parameterisation (GRASP). This parameterisation was obtained using Monte Carlo air shower simulations by parameterising the angular Cherenkov photon distribution with suitable analytical functions. Furthermore, it provides new classifying variables to differentiate γ-ray induced air showers from hadronic ones. The reconstruction of air shower parameters is achieved by a maximum likelihood fit and improves the angular resolution by 20-30% with respect to traditional image moment analysis methods. In combination with a MVA-based background rejection method using these new classifying variables the sensitivity can be improved by about 70%. An analysis of the Pulsar Wind Nebula MSH 15-5-2 and investigation of its morphology and spectral properties show an indication of energy dependent morphology in VHE γ-rays.

  5. Latest Results from the Air Shower Simulation Programs CORSIKA and CONEX

    CERN Document Server

    Pierog, T; Heck, D; Ostapchenko, S; Werner, K

    2008-01-01

    Interpretation of EAS measurements strongly depends on detailed air shower simulations. The uncertainty in the prediction of shower observables for different primary particles and energies is currently dominated by differences between hadronic interaction models. The new models QGSJETII-3 and EPOS 1.6, which reproduce all major results of existing accelerator data (including detailed data of RHIC experiments for EPOS), have been implemented in the air shower simulation programs CORSIKA and CONEX. We show predictions of these new models and compare them with those from older models such as QGSJET01 or SIBYLL. Results for important air shower observables are discussed in detail.

  6. A model for the transport of muons in extensive air showers

    CERN Document Server

    Cazon, L; Pimenta, M; Santos, E

    2012-01-01

    In this article we identify the key elements that govern the propagation of muons from the production in extensive air showers to ground. We describe a model based on simple assumptions that propagates the muons starting from the few relevant distributions at production. We compare the results to the ground distributions given by a full air shower Monte Carlo. This study is motivated by the need of modeling the muon component in extensive air showers with the goal of experimentally reconstructing their distributions at production, which act as a footprint of the hadronic cascade.

  7. Searching for mini black holes signatures in cosmic rays air shower

    International Nuclear Information System (INIS)

    Theories with extra dimensions at low Planck scale, offer the exciting possibility of mini black holes production in ultra high-energy particles interactions. In particular, cosmic neutrinos interaction can produce black holes deep in the Earth's atmosphere. These mini black holes then decay and produce ‘characteristic’ air showers. In this paper, we examine the properties of the mini black holes (mBH) air showers and compare them to the standard model (mSM) ones. We point out to some possible criteria that help distinguishing mBH air showers.

  8. Atmospheric multiple scattering of fluorescence and Cherenkov light emitted by extensive air showers

    CERN Document Server

    Pekala, J; Wilczynska, B; Wilczynski, H; 10.1016/j.nima.2009.03.244

    2009-01-01

    Atmospheric scattering of light emitted by an air shower not only attenuates direct fluorescence light from the shower, but also contributes to the observed shower light. So far only direct and singly-scattered Cherenkov photons have been taken into account in routine analyses of the observed optical image of air showers. In this paper a Monte Carlo method of evaluating the contribution of multiply scattered light to the optical air shower image is presented, as well as results of simulations and a parameterization of scattered light contribution to measured shower signal.

  9. Search for non-random features in arrival times of air showers

    International Nuclear Information System (INIS)

    It was searched for non-random components in arrival times of air showers of mean energy of 1 PeV. By counting the number of air showers observed within time windows of 20-60 minutes, it was found small deviation of air shower data from the conventional view of uniformly random cosmic ray injection. The arrival directions of the non-random events concentrate at the direction of the Galactic plane. Though the significance of these events is not so high because of the lack of statistics, they may be induced by sporadic non-random injection of ultra-high energy γ-rays from the Galactic plane

  10. Air shower simulation for WASAVIES: warning system for aviation exposure to solar energetic particles

    International Nuclear Information System (INIS)

    WASAVIES, a warning system for aviation exposure to solar energetic particles (SEPs), is under development by collaboration between several institutes in Japan and the USA. It is designed to deterministically forecast the SEP fluxes incident on the atmosphere within 6 h after flare onset using the latest space weather research. To immediately estimate the aircrew doses from the obtained SEP fluxes, the response functions of the particle fluxes generated by the incidence of monoenergetic protons into the atmosphere were developed by performing air shower simulations using the Particle and Heavy Ion Transport code system. The accuracy of the simulation was well verified by calculating the increase count rates of a neutron monitor during a ground-level enhancement, combining the response function with the SEP fluxes measured by the PAMELA spectrometer. The response function will be implemented in WASAVIES and used to protect air crews from additional SEP exposure. When galactic cosmic rays (GCRs) or solar energetic particles (SEPs) are incident on the atmosphere, they can induce air showers by producing various secondary particles. These secondary particles can reach conventional flight altitudes (∼12 km); hence, air crews are exposed to enhanced levels of radiation. The most important difference between GCR and SEP exposure arises from their temporal variations and dose rates; GCRs induce continuous exposure with low dose rates, usually up to several μSv h-1, whereas SEPs produce pulsed exposure with high dose rates, occasionally >1 mSv h-1, though such severe events rarely occur. Thus, subsequent evaluation is sufficient for estimating the aircrew dose due to GCR exposure, whereas forecasting is desirable for SEP exposure. Several calculation codes, e.g. CARI-6(3), EPCARD(4), JISCARD-EX(5), and PCAIRE(6), have been developed for post-exposure evaluation of GCR doses. On the other hand, empirical and phenomenological models have been developed for real-time or

  11. Sub-luminal pulses from cosmic ray air showers

    Science.gov (United States)

    Linsley, J.

    1985-01-01

    Some of the signals produced by air showers in scintillators possess a distinctive feature, a sub-luminal pulse (SLP) following the normal one with a time delay of approximately 1.5 r/c. The average amplitude of the SLP corresponds to an energy deposit of about 50 MeV, three times as much as is deposited in a typical scintillator by vertical minimum ionizing muons. The SLP account for approximately 5% of the energy deposited in the atmosphere by IR showers with energy 10 to the 10th power GeV at impact parameters 1 km. Assuming that these pulses are due to neutrons travelling with a speed slightly less than c, they provide a unique means of estimating E sub h, the energy deposited by slow hadrons, in showers of this very high energy. On the other hand, if not allowed for properly, these pulses are liable to cause errors in estimating the impact parameters of large showers from pulse width observations.

  12. Extensive Air Showers High Energy Phenomena and Astrophysical Aspects - A Tutorial, Reference Manual and Data Book

    CERN Document Server

    Grieder, Peter K.F

    2010-01-01

    Extensive air showers are a very unique phenomenon. In the more than six decades since their discovery by Auger et al. we have learned a great deal about these extremely energetic events and gained deep insights into high-energy phenomena, particle physics and astrophysics. In this Tutorial, Reference Manual and Data Book Peter K. F. Grieder provides the reader with a comprehensive view of the phenomenology and facts of the various types of interactions and cascades, theoretical background, experimental methods, data evaluation and interpretation, and air shower simulation. He discusses astrophysical aspects of the primary radiation and addresses the questions that continue to puzzle researchers. The book is divided into two parts, each in its own separate volume: Part I in Volume I deals mainly with the basic theoretical framework of the processes that determine an air shower and ends with a summary of ways to extract information on the primary radiation from air shower observations. It also presents a compi...

  13. Studies of Cosmic Ray Composition and Air Shower Structure with the Pierre Auger Observatory

    CERN Document Server

    Abraham, J; Aglietta, M; Aguirre, C; Ahn, E J; Allard, D; Allekotte, I; Allen, J; Alvarez-Muñiz, J; Ambrosio, M; Anchordoqui, L; Andringa, S; Anzalone, A; Aramo, C; Arganda, E; Argirò, S; Arisaka, K; Arneodo, F; Arqueros, F; Asch, T; Asorey, H; Assis, P; Aublin, J; Ave, M; Avila, G; Bäcker, T; Badagnani, D; Barber, K B; Barbosa-Ademarlaudo, F; Barroso, S L C; Baughman, B; Bauleo, P; Beatty, J J; Beau, T; Becker, B R; Becker, K H; Bellétoile, A; Bellido, J A; BenZvi, S; Bérat, C; Bernardini, P; Bertou, X; Biermann, P L; Billoir, P; Blanch-Bigas, O; Blanco, F; Bleve, C; Blümer, H; Boháčová, M; Boncioli, D; Bonifazi, C; Bonino, R; Borodai, N; Brack, J; Brogueira, P; Brown, W C; Bruijn, R; Buchholz, P; Bueno, A; Burton, R E; Busca, N G; Caballero-Mora, K S; Caramete, L; Caruso, R; Carvalho, W; Castellina, A; Catalano, O; Cazon, L; Cester, R; Chauvin, J; Chiavassa, A; Chinellato, J A; Chou, A; Chudoba, J; Chye, J; Clay, R W; Colombo, E; Conceição, R; Connolly, B; Contreras, F; Coppens, J; Cordier, A; Cotti, U; Coutu, S; Covault, C E; Creusot, A; Criss, A; Cronin, J; Curutiu, A; Dagoret-Campagne, S; Dallier, R; Daumiller, K; Dawson, B R; de Almeida, R M; De Domenico, M; De Donato, C; De Jong, S J; De La Vega, G; Junior, W J M de Mello; Neto, J R T de Mello; De Mitri, I; De Souza, V; de Vries, K D; Decerprit, G; Del Peral, L; Deligny, O; Della Selva, A; Fratte, C Delle; Dembinski, H; DiGiulio, C; Diaz, J C; Diep, P N; Dobrigkeit, C; D'Olivo, J C; Dong, P N; Dorofeev, A; Anjos, J C dos; Dova, M T; D'Urso, D; Dutan, I; Duvernois, M A; Engel, R; Erdmann, M; Escobar, C O; Etchegoyen, A; Luis, P Facal San; Falcke, H; Farrar, G; Fauth, A C; Fazzini, N; Ferrer, F; Ferrero, A; Fick, B; Filevich, A; Filipčič, A; Fleck, I; Fliescher, S; Fracchiolla, C E; Fraenkel, E D; Fulgione, W; Gamarra, R F; Gambetta, S; García, B; GarcíaGámez, D; Garcia-Pinto, D; Garrido, X; Gelmini, G; Gemmeke, H; Ghia, P L; Giaccari, U; Giller, M; Glass, H; Goggin, L M; Gold, M S; Golup, G; Albarracin, F Gomez; Berisso, M Gómez; Gonçalves, P; Amaral, M Gonçalves do; González, D; Gonzalez, J G; Góra, D; Gorgi, A; Gouffon, P; Gozzini, S R; Grashorn, E; Grebe, S; Grigat, M; Grillo, A F; Guardincerri, Y; Guarino, F; Guedes, G P; Gutiérrez, J; Hague, J D; Halenka, V; Hansen, P; Harari, D; Harmsma, S; Harton, J L; Haungs, A; Healy, M D; Hebbeker, T; Hebrero, G; Heck, D; Hojvat, C; Holmes, V C; Homola, P; Hörandel, J R; Horneffer, A; Hrabovský, M; Huege, T; Hussain, M; Iarlori, M; Insolia, A; Ionita, F; Italiano, A; Jiraskova, S; Kaducak, M; Kampert, K H; Karova, T; Kasper, P; Kégl, B; Keilhauer, B; Kemp, E; Kieckhafer, R M; Klages, H O; Kleifges, M; Kleinfeller, J; Knapik, R; Knapp, J; Koang, D -H; Krieger, A; Krömer, O; Kruppke-Hansen, D; Kühn, F; Kuempel, D; Kulbartz, K; Kunka, N; Kusenko, A; LaRosa, G; Lachaud, C; Lago, B L; Lautridou, P; Leão, M S A B; Lebrun, D; Lebrun, P; Lee, J; de Oliveira, M A Leigui; Lemiere, A; Letessier-Selvon, A A; Leuthold, M; Lhenry-Yvon, I; López, R; Agüera, A Lopez; Louedec, K; Bahilo, J Lozano; Lucero, A; Lyberis, H; Maccarone, M C; Macolino, C; Maldera, S; Mandat, D; Mantsch, P; Mariazzi, A G; Maris, I C; Falcon, H R Marquez; Martello, D; Bravo, O Martínez; Mathes, H J; Matthews, J; Matthews, J A J; Matthiae, G; Maurizio, D; Mazur, P O; McEwen, M; McNeil, R R; Medina-Tanco, G; Melissas, M; Melo, D; Menichetti, E; Menshikov, A; Meyhandan, R; Micheletti, M I; Miele, G; Miller, W; Miramonti, L; Mollerach, S; Monasor, M; Ragaigne, D Monnier; Montanet, F; Morales, B; Morello, C; Moreno, J C; Morris, C; Mostafá, M; Moura, C A; Müller, S; Muller, M A; Mussa, R; Navarra, G; Navarro, J L; Navas, S; Necesal, P; Nellen, L; Newman-Holmes, C; Newton, D; Nhung, P T; Nierstenhoefer, N; Nitz, D; Nosek, D; Nožka, L; Nyklicek, M; Oehlschläger, J; Olinto, A; Oliva, P; Olmos-Gilbaja, V M; Ortiz, M; Pacheco, N; Selmi-Dei, D Pakk; Palatka, M; Pallotta, J; Parente, G; Parizot, E; Parlati, S; Pastor, S; Patel, M; Paul, T; Pavlidou, V; Payet, K; Pech, M; Pȩkala, J; Pepe, I M; Perrone, L; Pesce, R; Petermann, E; Petrera, S; Petrinca, P; Petrolini, A; Petrov, Y; Petrovic, J; Pfendner, C; Piegaia, R; Pierog, T; Pimenta, M; Pinto, T; Pirronello, V; Pisanti, O; Platino, M; Pochon, J; Ponce, V H; Pontz, M; Privitera, P; Prouza, M; Quel, E J; Rautenberg, J; Ravel, O; Ravignani, D; Redondo, A; Revenu, B; Rezende, F A S; Rídky, J; Riggi, S; Risse, M; Rivière, C; Rizi, V; Robledo, C; Rodríguez, G; Martino, J Rodriguez; Rojo, J Rodriguez; Rodriguez-Cabo, I; Rodríguez-Frías, M D; Ros, G; Rosado, J; Rossler, T; Roth, M; Rouillé-d'Orfeuil, B; Roulet, E; Rovero, A C; Salamida, F; Salazar, H; Salina, G; Sánchez, F; Santander, M; Santo, C E; Santos, E M; Sarazin, F; Sarkar, S; Sato, R; Scharf, N; Scherini, V; Schieler, H; Schiffer, P; Schmidt, A; Schmidt, F; Schmidt, T; Scholten, O; Schoorlemmer, H; Schovancova, J; Schovánek, P; Schroeder, F; Schulte, S; Schüssler, F; Schuster, D; Sciutto, S J; Scuderi, M; Segreto, A; Semikoz, D; Settimo, M; Shellard, R C; Sidelnik, I; Siffert, B B; Sigl, G; Śmia\\lkowski, A; Šmída, R; Smith, B E; Snow, G R; Sommers, P; Sorokin, J; Spinka, H; Squartini, R; Strazzeri, E; Stutz, A; Suárez, F; Suomijärvi, T; Supanitsky, A D; Sutherland, M S; Swain, J; Szadkowski, Z; Tamashiro, A; Tamburro, A; Tarutina, T; Taşcuau, O; Tcaciuc, R; Tcherniakhovski, D; Tegolo, D; Thao, N T; Thomas, D; Ticona, R; Tiffenberg, J; Timmermans, C; Tkaczyk, W; Peixoto, C J Todero; Tomé, B; Tonachini, A; Torres, I; Travnicek, P; Tridapalli, D B; Tristram, G; Trovato, E; Tueros, M; Ulrich, R; Unger, M; Urban, M; Galicia, J F Valdés; Valiño, I; Valore, L; vandenBerg, A M; Vázquez, J R; Vázquez, R A; Veberič, D; Velarde, A; Venters, T; Verzi, V; Videla, M; Villaseñor, L; Vorobiov, S; Voyvodic, L; Wahlberg, H; Wahrlich, P; Wainberg, O; Warner, D; Watson, A A; Westerhoff, S; Whelan, B J; Wieczorek, G; Wiencke, L; Wilczyńska, B; Wilczyński, H; Wileman, C; Winnick, M G; Wu, H; Wundheiler, B; Yamamoto, T; Younk, P; Yuan, G; Yushkov, A; Zas, E; Zavrtanik, D; Zavrtanik, M; Zaw, I; Zepeda, A; Ziolkowski, M

    2009-01-01

    Studies of the composition of the highest energy cosmic rays with the Pierre Auger Observatory, including examination of hadronic physics effects on the structure of extensive air showers. Submissions to the 31st ICRC, Lodz, Poland (July 2009).

  14. Size distributions of air showers accompanied with high energy gamma ray bundles observed at Mt. Chacaltaya

    Science.gov (United States)

    Matano, T.; Machida, M.; Tsuchima, I.; Kawasumi, N.; Honda, K.; Hashimoto, K.; Martinic, N.; Zapata, J.; Navia, C. E.; Aquirre, C.

    1985-01-01

    Size distributions of air showers accompanied with bundle of high energy gamma rays and/or large size bursts under emulsion chambers, to study the composition of primary cosmic rays and also characteristics of high energy nuclear interaction. Air showers initiated by particles with a large cross section of interaction may develop from narrow region of the atmosphere near the top. Starting levels of air showers by particles with smaller cross section fluctuate in wider region of the atmosphere. Air showers of extremely small size accompanied with bundle of gamma rays may be ones initiated by protons at lower level after penetrating deep atmosphere without interaction. It is determined that the relative size distribution according to the total energy of bundle of gamma rays and the total burst size observed under 15 cm lead absorber.

  15. Some effects of first proton-air interactions on development of giant air showers

    International Nuclear Information System (INIS)

    Air shower simulations have been studied for dependence on features of the initial proton-air collisions at 1019 eV. Comparisons are made between results with Sibyll and QGSjet hadronic interaction event generators

  16. Atmospheric effects on extensive air showers observed with the Surface Detector of the Pierre Auger Observatory

    CERN Document Server

    2009-01-01

    Atmospheric parameters, such as pressure (P), temperature (T) and density, affect the development of extensive air showers initiated by energetic cosmic rays. We have studied the impact of atmospheric variations on extensive air showers by means of the surface detector of the Pierre Auger Observatory. The rate of events shows a ~10% seasonal modulation and ~2% diurnal one. We find that the observed behaviour is explained by a model including the effects associated with the variations of pressure and density. The former affects the longitudinal development of air showers while the latter influences the Moliere radius and hence the lateral distribution of the shower particles. The model is validated with full simulations of extensive air showers using atmospheric profiles measured at the site of the Pierre Auger Observatory.

  17. Muons in extensive air showers at E0 = 1016.6 - 1019.8 eV

    International Nuclear Information System (INIS)

    The results of combined analysis of the data on the muons in the extensive air showers with the energies of E0 ≥ 4 x 1016 eV are presented. Their comparison with the calculations by the QGSJET model is given. It is shown, that by the E0 ≤ 1018 eV this model does not contradict the measurements in the approximation of the primary particles changing composition from the mixture with prevalence of heavy nuclei over the protons. The experiments by the E0 ≥ 3 x 1018 eV indicate, that the showers are developed other wise as forecasted by the QGSJET model

  18. Nanosecond-level time synchronization of autonomous radio detector stations for extensive air showers

    CERN Document Server

    Aab, A; Aglietta, M; Ahn, E J; Samarai, I Al; Albuquerque, I F M; Allekotte, I; Allison, P; Almela, A; Castillo, J Alvarez; Alvarez-Muñiz, J; Batista, R Alves; Ambrosio, M; Aminaei, A; Anastasi, G A; Anchordoqui, L; Andringa, S; Aramo, C; Arqueros, F; Arsene, N; Asorey, H; Assis, P; Aublin, J; Avila, G; Awal, N; Badescu, A M; Baus, C; Beatty, J J; Becker, K H; Bellido, J A; Berat, C; Bertaina, M E; Bertou, X; Biermann, P L; Billoir, P; Blaess, S G; Blanco, A; Blanco, M; Blazek, J; Bleve, C; Blümer, H; Boháčová, M; Boncioli, D; Bonifazi, C; Borodai, N; Brack, J; Brancus, I; Bretz, T; Bridgeman, A; Brogueira, P; Buchholz, P; Bueno, A; Buitink, S; Buscemi, M; Caballero-Mora, K S; Caccianiga, B; Caccianiga, L; Candusso, M; Caramete, L; Caruso, R; Castellina, A; Cataldi, G; Cazon, L; Cester, R; Chavez, A G; Chiavassa, A; Chinellato, J A; Chudoba, J; Cilmo, M; Clay, R W; Cocciolo, G; Colalillo, R; Coleman, A; Collica, L; Coluccia, M R; Conceição, R; Contreras, F; Cooper, M J; Cordier, A; Coutu, S; Covault, C E; Cronin, J; Dallier, R; Daniel, B; Dasso, S; Daumiller, K; Dawson, B R; de Almeida, R M; de Jong, S J; De Mauro, G; Neto, J R T de Mello; De Mitri, I; de Oliveira, J; de Souza, V; del Peral, L; Deligny, O; Dhital, N; Di Giulio, C; Di Matteo, A; Diaz, J C; Castro, M L Díaz; Diogo, F; Dobrigkeit, C; Docters, W; D'Olivo, J C; Dorofeev, A; Hasankiadeh, Q Dorosti; Anjos, R C dos; Dova, M T; Ebr, J; Engel, R; Erdmann, M; Erfani, M; Escobar, C O; Eser, J; Espadanal, J; Etchegoyen, A; Falcke, H; Fang, K; Farrar, G; Fauth, A C; Fazzini, N; Ferguson, A P; Fick, B; Figueira, J M; Filevich, A; Filipčič, A; Fratu, O; Freire, M M; Fujii, T; García, B; García-Gámez, D; Garcia-Pinto, D; Gate, F; Gemmeke, H; Gherghel-Lascu, A; Ghia, P L; Giaccari, U; Giammarchi, M; Giller, M; Głas, D; Glaser, C; Glass, H; Golup, G; Berisso, M Gómez; Vitale, P F Gómez; González, N; Gookin, B; Gordon, J; Gorgi, A; Gorham, P; Gouffon, P; Griffith, N; Grillo, A F; Grubb, T D; Guarino, F; Guedes, G P; Hampel, M R; Hansen, P; Harari, D; Harrison, T A; Hartmann, S; Harton, J L; Haungs, A; Hebbeker, T; Heck, D; Heimann, P; Hervé, A E; Hill, G C; Hojvat, C; Hollon, N; Holt, E; Homola, P; Hörandel, J R; Horvath, P; Hrabovský, M; Huber, D; Huege, T; Insolia, A; Isar, P G; Jandt, I; Jansen, S; Jarne, C; Johnsen, J A; Josebachuili, M; Kääpä, A; Kambeitz, O; Kampert, K H; Kasper, P; Katkov, I; Keilhauer, B; Kemp, E; Kieckhafer, R M; Klages, H O; Kleifges, M; Kleinfeller, J; Krause, R; Krohm, N; Kuempel, D; Mezek, G Kukec; Kunka, N; Awad, A W Kuotb; LaHurd, D; Lang, A; Latronico, L; Lauer, R; Lauscher, M; Lautridou, P; Coz, S Le; Lebrun, D; Lebrun, P; de Oliveira, M A Leigui; Letessier-Selvon, A; Lhenry-Yvon, I; Link, K; Lopes, L; López, R; Casado, A López; Louedec, K; Lucero, A; Malacari, M; Mallamaci, M; Maller, J; Mandat, D; Mantsch, P; Mariazzi, A G; Marin, V; Mariş, I C; Marsella, G; Martello, D; Martinez, H; Bravo, O Martínez; Martraire, D; Meza, J J Masías; Mathes, H J; Mathys, S; Matthews, J; Matthews, J A J; Matthiae, G; Maurizio, D; Mayotte, E; Mazur, P O; Medina, C; Medina-Tanco, G; Meissner, R; Mello, V B B; Melo, D; Menshikov, A; Messina, S; Micheletti, M I; Middendorf, L; Minaya, I A; Miramonti, L; Mitrica, B; Molina-Bueno, L; Mollerach, S; Montanet, F; Morello, C; Mostafá, M; Moura, C A; Müller, G; Muller, M A; Müller, S; Navas, S; Necesal, P; Nellen, L; Nelles, A; Neuser, J; Nguyen, P H; Niculescu-Oglinzanu, M; Niechciol, M; Niemietz, L; Niggemann, T; Nitz, D; Nosek, D; Novotny, V; Nožka, L; Núñez, L A; Ochilo, L; Oikonomou, F; Olinto, A; Pacheco, N; Selmi-Dei, D Pakk; Palatka, M; Pallotta, J; Papenbreer, P; Parente, G; Parra, A; Paul, T; Pech, M; Pękala, J; Pelayo, R; Pepe, I M; Perrone, L; Petermann, E; Peters, C; Petrera, S; Petrov, Y; Phuntsok, J; Piegaia, R; Pierog, T; Pieroni, P; Pimenta, M; Pirronello, V; Platino, M; Plum, M; Porcelli, A; Porowski, C; Prado, R R; Privitera, P; Prouza, M; Quel, E J; Querchfeld, S; Quinn, S; Rautenberg, J; Ravel, O; Ravignani, D; Reinert, D; Revenu, B; Ridky, J; Risse, M; Ristori, P; Rizi, V; de Carvalho, W Rodrigues; Rojo, J Rodriguez; Rodríguez-Frías, M D; Rogozin, D; Rosado, J; Roth, M; Roulet, E; Rovero, A C; Saffi, S J; Saftoiu, A; Salazar, H; Saleh, A; Greus, F Salesa; Salina, G; Gomez, J D Sanabria; Sánchez, F; Sanchez-Lucas, P; Santos, E M; Santos, E; Sarazin, F; Sarkar, B; Sarmento, R; Sarmiento-Cano, C; Sato, R; Scarso, C; Schauer, M; Scherini, V; Schieler, H; Schmidt, D; Scholten, O; Schoorlemmer, H; Schovánek, P; Schröder, F G; Schulz, A; Schulz, J; Schumacher, J; Sciutto, S J; Segreto, A; Settimo, M; Shadkam, A; Shellard, R C; Sigl, G; Sima, O; Śmiałkowski, A; Šmída, R; Snow, G R; Sommers, P; Sonntag, S; Sorokin, J; Squartini, R; Srivastava, Y N; Stanca, D; Stanič, S; Stapleton, J; Stasielak, J

    2015-01-01

    To exploit the full potential of radio measurements of cosmic-ray air showers at MHz frequencies, a detector timing synchronization within 1 ns is needed. Large distributed radio detector arrays such as the Auger Engineering Radio Array (AERA) rely on timing via the Global Positioning System (GPS) for the synchronization of individual detector station clocks. Unfortunately, GPS timing is expected to have an accuracy no better than about 5 ns. In practice, in particular in AERA, the GPS clocks exhibit drifts on the order of tens of ns. We developed a technique to correct for the GPS drifts, and an independent method used for cross-checks that indeed we reach nanosecond-scale timing accuracy by this correction. First, we operate a "beacon transmitter" which emits defined sine waves detected by AERA antennas recorded within the physics data. The relative phasing of these sine waves can be used to correct for GPS clock drifts. In addition to this, we observe radio pulses emitted by commercial airplanes, the posit...

  19. Prospects for a radio air-shower detector at South Pole

    CERN Document Server

    ,

    2012-01-01

    IceCube is currently not only the largest neutrino telescope but also one of the world's most competitive instruments for studying cosmic rays in the PeV to EeV regime where the transition from galactic to extra-galactic sources should occur. Further augmenting this observatory with an array of radio sensors in the 10-100 MHz regime will additionally permit observation of the geomagnetic radio emission from the air shower. Yielding complementary information on the shower development a triple-technology array consisting of radio sensors, the ground sampling stations of IceTop and the in-ice optical modules of IceCube, should significantly improve the understanding of cosmic rays, as well as enhance many aspects of the physics reach of the observatory. Here we present first results from two exploratory setups deployed at the South Pole. Noise measurements from data taken in two consecutive seasons show a very good agreement of the predicted and observed response of the antennas designed specifically for this pu...

  20. Muons in air showers at the Pierre Auger Observatory: Mean number in highly inclined events

    CERN Document Server

    ,

    2014-01-01

    We present the first hybrid measurement of the average muon number in air showers at ultra-high energies, initiated by cosmic rays with zenith angles between 62{\\deg} and 80{\\deg}. The measurement is based on 174 hybrid events recorded simultaneously with the Surface Detector array and the Fluorescence Detector of the Pierre Auger Observatory. The muon number for each shower is derived by scaling a simulated reference profile of the lateral muon density distribution at the ground until it fits the data. A $10^{19}$ eV shower with a zenith angle of 67{\\deg}, which arrives at the Surface Detector array at an altitude of 1450 m above sea level, contains on average $(2.68 \\pm 0.04 \\pm 0.48\\,(\\mathrm{sys.})) \\times 10^{7}$ muons with energies larger than 0.3 GeV. The logarithmic gain $\\text{d}\\ln{N_\\mu} / \\text{d}\\ln{E}$ of muons with increasing energy between $4 \\times 10^{18}$ eV and $5\\times 10^{19}$ eV is measured to be $(1.029\\, \\pm\\, 0.024\\, \\pm 0.030\\,(\\mathrm{sys.}))$.

  1. Artificial Neural Network as a FPGA Trigger for a Detection of Very Inclined Air Showers

    CERN Document Server

    Szadkowski, Zbigniew

    2014-01-01

    The observation of ultra-high energy neutrinos has become a priority in experimental astroparticle physics. Neutrinos can interact in the atmosphere (downward-going) or in the Earth crust (Earth-skimming), producing air showers that can be observed with arrays of detectors at the ground. The surface detector array of the Pierre Auger Observatory can detect these types of cascades. The distinguishing signature for neutrino events is the presence of very inclined showers produced close to the ground (i.e., after having traversed a large amount of atmosphere). Up to now, the Pierre Auger Observatory did not find any candidate on a neutrino event. This imposes competitive limits to the diffuse flux of neutrinos. A very low rate of events potentially generated by neutrinos is a significant challenge for a detection technique and requires both sophisticated algorithms and high-resolution hardware. We present a trigger based on a pipeline artificial neural network implemented in a large FPGA which after learning can...

  2. Extensive Air Showers: from the muonic smoking guns to the hadronic backbone

    OpenAIRE

    Cazon L.

    2013-01-01

    Extensive Air Showers are complex macroscopic objects initiated by single ultra-high energy particles. They are the result of millions of high energy reactions in the atmosphere and can be described as the superposition of hadronic and electromagnetic cascades. The hadronic cascade is the air shower backbone, and it is mainly made of pions. Decays of neutral pions initiate electromagnetic cascades, while the decays of charged pions produce muons which leave the hadronic core and travel many k...

  3. What the radio signal tells about the cosmic-ray air shower

    Directory of Open Access Journals (Sweden)

    Werner Klaus

    2013-06-01

    Full Text Available The physics of radio emission from cosmic-ray induced air showers is shortly summarized. It will be shown that the radio signal at different distances from the shower axis provides complementary information on the longitudinal shower evolution, in particular the early part, and on the distribution of the electrons in the shower core. This complements the information obtained from surface, fluorescence, and muon detectors and is very useful in getting a comprehensive picture of an air shower.

  4. Search for tachyons associated with extensive air showers in the ground level cosmic radiation

    Science.gov (United States)

    Masjed, H. F.; Ashton, F.

    1985-01-01

    Events detected in a shielded plastic scintillation counter occurring in the 26 microsec preceding the arrival of an extensive air shower at ground level with local electron density or = 20 m to the -2 power and the 240 microsec after its arrival have been studied. No significant excess of events (tachyons) arriving in the early time domain have been observed in a sample of 11,585 air shower triggers.

  5. Probing Atmospheric Electric Fields in Thunderstorms through Radio Emission from Cosmic-Ray-Induced Air Showers.

    Science.gov (United States)

    Schellart, P; Trinh, T N G; Buitink, S; Corstanje, A; Enriquez, J E; Falcke, H; Hörandel, J R; Nelles, A; Rachen, J P; Rossetto, L; Scholten, O; Ter Veen, S; Thoudam, S; Ebert, U; Koehn, C; Rutjes, C; Alexov, A; Anderson, J M; Avruch, I M; Bentum, M J; Bernardi, G; Best, P; Bonafede, A; Breitling, F; Broderick, J W; Brüggen, M; Butcher, H R; Ciardi, B; de Geus, E; de Vos, M; Duscha, S; Eislöffel, J; Fallows, R A; Frieswijk, W; Garrett, M A; Grießmeier, J; Gunst, A W; Heald, G; Hessels, J W T; Hoeft, M; Holties, H A; Juette, E; Kondratiev, V I; Kuniyoshi, M; Kuper, G; Mann, G; McFadden, R; McKay-Bukowski, D; McKean, J P; Mevius, M; Moldon, J; Norden, M J; Orru, E; Paas, H; Pandey-Pommier, M; Pizzo, R; Polatidis, A G; Reich, W; Röttgering, H; Scaife, A M M; Schwarz, D J; Serylak, M; Smirnov, O; Steinmetz, M; Swinbank, J; Tagger, M; Tasse, C; Toribio, M C; van Weeren, R J; Vermeulen, R; Vocks, C; Wise, M W; Wucknitz, O; Zarka, P

    2015-04-24

    We present measurements of radio emission from cosmic ray air showers that took place during thunderstorms. The intensity and polarization patterns of these air showers are radically different from those measured during fair-weather conditions. With the use of a simple two-layer model for the atmospheric electric field, these patterns can be well reproduced by state-of-the-art simulation codes. This in turn provides a novel way to study atmospheric electric fields. PMID:25955053

  6. Probing Atmospheric Electric Fields in Thunderstorms through Radio Emission from Cosmic-Ray-Induced Air Showers

    CERN Document Server

    Schellart, P; Buitink, S; Corstanje, A; Enriquez, J E; Falcke, H; Hörandel, J R; Nelles, A; Rachen, J P; Rossetto, L; Scholten, O; ter Veen, S; Thoudam, S; Ebert, U; Koehn, C; Rutjes, C; Alexov, A; Anderson, J M; Avruch, I M; Bentum, M J; Bernardi, G; Best, P; Bonafede, A; Breitling, F; Broderick, J W; Brüggen, M; Butcher, H R; Ciardi, B; de Geus, E; de Vos, M; Duscha, S; Eislöffel, J; Fallows, R A; Frieswijk, W; Garrett, M A; Grießmeier, J; Gunst, A W; Heald, G; Hessels, J W T; Hoeft, M; Holties, H A; Juette, E; Kondratiev, V I; Kuniyoshi, M; Kuper, G; Mann, G; McFadden, R; McKay-Bukowski, D; McKean, J P; Mevius, M; Moldon, J; Norden, M J; Orru, E; Paas, H; Pandey-Pommier, M; Pizzo, R; Polatidis, A G; Reich, W; Röttgering, H; Scaife, A M M; Schwarz, D J; Serylak, M; Smirnov, O; Steinmetz, M; Swinbank, J; Tagger, M; Tasse, C; Toribio, M C; van Weeren, R J; Vermeulen, R; Vocks, C; Wise, M W; Wucknitz, O; Zarka, P

    2015-01-01

    We present measurements of radio emission from cosmic ray air showers that took place during thunderstorms. The intensity and polarization patterns of these air showers are radically different from those measured during fair-weather conditions. With the use of a simple two-layer model for the atmospheric electric field, these patterns can be well reproduced by state-of-the-art simulation codes. This in turn provides a novel way to study atmospheric electric fields.

  7. Monte Carlo simulations of geosynchrotron radio emission from CORSIKA-simulated air showers

    OpenAIRE

    Huege, T.; Ulrich, R.(Institut für Experimentelle Kernphysik, Karlsruhe, Germany); Engel, R.

    2006-01-01

    We present simulations performed with REAS2, a new Monte Carlo code for the calculation of geosynchrotron radio emission from extensive air showers. The code uses thoroughly tested time-domain radio emission routines in conjunction with a realistic air shower model based on per-shower multi-dimensional CORSIKA-generated histograms. We assess in detail how the transition from simpler, parametrised, to realistic, CORSIKA-based particle distributions affects the predicted radio emission from a t...

  8. A Realistic Treatment of Geomagnetic Cherenkov Radiation from Cosmic Ray Air Showers

    OpenAIRE

    Werner, Klaus; de Vries, Krijn D.; Scholten, Olaf

    2012-01-01

    We present a macroscopic calculation of coherent electro-magnetic radiation from air showers initiated by ultra-high energy cosmic rays, based on currents obtained from three-dimensional Monte Carlo simulations of air showers in a realistic geo-magnetic field. We discuss the importance of a correct treatment of the index of refraction in air, given by the law of Gladstone and Dale, which affects the pulses enormously for certain configurations, compared to a simplified treatment using a const...

  9. Longitudinal development of muons in large air showers studies from the arrival time distributions measured at 900m above sea level

    Science.gov (United States)

    Kakimoto, F.; Tsuchimoto, I.; Enoki, T.; Suga, K.; Nishi, K.

    1985-01-01

    The arrival time distributions of muons with energies above 1.0GeV and 0.5GeV have been measured in the Akeno air-shower array to study the longitudinal development of muons in air showers with primary energies in the range 10 to the 17th power to 10 to the 18th power ev. The average rise times of muons with energies above 1.0GeV at large core distances are consistent with those expected from very high multiplicity models and, on the contrary, with those expected from the low multiplicity models at small core distances. This implies that the longitudinal development at atmospheric depth smaller than 500 cm square is very fast and that at larger atmospheric depths is rather slow.

  10. Radio measurements of the energy and depth of maximum of cosmic-ray air showers by Tunka-Rex

    CERN Document Server

    Bezyazeekov, P A; Gress, O A; Haungs, A; Hiller, R; Huege, T; Kazarina, Y; Kleifges, M; Konstantinov, E N; Korosteleva, E E; Kostunin, D; Krömer, O; Kuzmichev, L A; Lubsandorzhiev, N; Mirgazov, R R; Monkhoev, R; Pakhorukov, A; Pankov, L; Prosin, V V; Rubtsov, G I; Schröder, F G

    2015-01-01

    We reconstructed the energy and the position of the shower maximum of air showers with energies $E \\gtrsim 100\\,$PeV using radio measurements performed with Tunka-Rex. A comparison to air-Cherenkov measurements of the same air showers with the Tunka-133 photomultiplier array confirms that the radio reconstruction works reliably. Splitting our data set into two seasons, we had blinded the Tunka-133 reconstruction for the second season, which we used as later, independent cross-check of the methods developed for the first season. This gives additional confidence in the radio reconstruction. An event-to-event comparison of Tunka-Rex and Tunka-133 shows that both experiments yield consistent values for energy and $X_{\\mathrm{max}}$. The energy precision of Tunka-Rex is comparable to the Tunka-133 precision of $15\\,\\%$, and comes with a $20\\,\\%$ uncertainty on the absolute scale dominated by the amplitude calibration of the antennas. For $X_{\\mathrm{max}}$, this is the first direct experimental correlation of radi...

  11. Arrival directions of large air showers, low-mu showers and old-age low-mu air showers observed at St. Chacaltaya

    International Nuclear Information System (INIS)

    Arrival 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

  12. Arrival directions of large air showers, low-mu showers and old-age low-mu air showers observed at St. Chacaltaya

    Science.gov (United States)

    Hagiwara, K.; Yoshii, H.; Martinic, N.; Siles, L.; Miranda, P.; Kakimoto, F.; Obara, T.; Suga, K.; Kaneko, T.; Inoue, N.

    1985-01-01

    Arrival 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.

  13. Investigating the Cherenkov light lateral distribution function for primary proton and iron nuclei in extensive air showers

    International Nuclear Information System (INIS)

    The lateral distribution function (LDF) of Cherenkov radiation in extensive air showers (EAS) was simulated by CORSIKA program for the conditions of Yakutsk Cherenkov array at high energy range (1013-1016 eV) for two primary particles (p and Fe) for different zenith angles. Using Breit-Wigner function for analyzing Cherenkov light LDF, a parameterization of Cherenkov light LDF was reconstructed by depending on CORSIKA simulation as a function of primary energy. The comparison between the estimated Cherenkov light LDF and the LDF that was measured on the Yakutsk EAS array gives the ability of particle identification that initiated the shower and determination of particle's energy around the knee region. The extrapolation of approximated Cherenkov light LDF for energies 20 and 30 PeV was obtained for primary particles (p and Fe)

  14. Investigating the Cherenkov light lateral distribution function for primary proton and iron nuclei in extensive air showers

    Science.gov (United States)

    Al-Rubaiee, A. A.; Hashim, U.; Al-Douri, Y.

    2015-11-01

    The lateral distribution function (LDF) of Cherenkov radiation in extensive air showers (EAS) was simulated by CORSIKA program for the conditions of Yakutsk Cherenkov array at the high energy range (1013-1016) eV for two primary particles (p and Fe) for different zenith angles. By depending on Breit-Wigner function for analyzing of Cherenkov light LDF, a parameterization of Cherenkov light LDF was reconstructed by depending on CORSIKA simulation as a function of primary energy. The comparison between the estimated Cherenkov light LDF with the LDF that measured on the Yakutsk EAS array gives the ability of particle identification that initiated the shower and determination of particle's energy around the knee region. The extrapolation of approximated Cherenkov light LDF for energies 20 and 30 PeV was obtained for primary particles (p and Fe).

  15. Measurement of muon production depth in cosmic ray induced extensive air showers by time structure of muons at observation level

    Science.gov (United States)

    Rastegarzadeh, Gohar; Khoshabadi, Sahar

    2016-04-01

    In the present work, muon production depth (MPD) of extensive air showers (EASs) are measured from time structure of muons at the observation level. A new method for calculating MPD is presented. Based on its relation to the maximum depth of development of electrons and muons (Xmax and Xmaxμ), this parameter has been used as a mass discriminator factor. Using CORSIKA simulation, different simulations for proton and iron primaries in the energy range of 1014-1015 eV are presented. It is found that MPD distribution is strongly related to Xmax and Xmaxμ. These are mass sensitive parameters and their potential as mass discriminator parameters between light and heavy primaries for ALBORZ prototype array and some arbitrary arrays are investigated.

  16. The current status of the GRAPES-3 extensive air shower experiment

    Science.gov (United States)

    Gupta, S. K.; Antia, H. M.; Dugad, S. R.; Goswami, U. D.; Hayashi, Y.; Iyer, A.; Ito, N.; Jagadeesan, P.; Jain, A.; Karthikeyan, S.; Kawakami, S.; Minamino, M.; Mohanty, P. K.; Morris, S. D.; Nayak, P. K.; Nonaka, T.; Oshima, A.; Rao, B. S.; Ravindran, K. C.; Tanaka, H.; Tonwar, S. C.; Grapes-3 Collaboration

    2009-12-01

    The GRAPES-3 is a dense extensive air shower array operating with ˜400 scintillator detectors and it also contains a 560 m 2 tracking muon detector ( E>1 GeV), at Ooty in India. 25% of scintillator detectors are instrumented with two fast photomultiplier tubes (PMTs) for extending the dynamic range to ˜5×10 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° at 30 TeV, is measured from the shadow of the Moon on the isotropic flux of cosmic rays. A sensitive limit on the diffuse flux of 100 TeV γ-rays is placed by using muon detector to filter the charged cosmic ray background. A tracking muon detector allows sensitive measurements on 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.

  17. The current status of the GRAPES-3 extensive air shower experiment

    Energy Technology Data Exchange (ETDEWEB)

    Gupta, S.K.; Antia, H.M.; Dugad, S.R.; Goswami, U.D. [Tata Institute of Fundamental Research, Mumbai 400005 (India); Hayashi, Y. [Graduate School of Science, Osaka City University, Osaka 558-8585 (Japan); Iyer, A. [Tata Institute of Fundamental Research, Mumbai 400005 (India); Ito, N. [Graduate School of Science, Osaka City University, Osaka 558-8585 (Japan); Jagadeesan, P.; Jain, A.; Karthikeyan, S. [Tata Institute of Fundamental Research, Mumbai 400005 (India); Kawakami, S.; Minamino, M. [Graduate School of Science, Osaka City University, Osaka 558-8585 (Japan); Mohanty, P.K.; Morris, S.D.; Nayak, P.K. [Tata Institute of Fundamental Research, Mumbai 400005 (India); Nonaka, T. [Graduate School of Science, Osaka City University, Osaka 558-8585 (Japan); Oshima, A.; Rao, B.S.; Ravindran, K.C.; Tanaka, H. [Tata Institute of Fundamental Research, Mumbai 400005 (India)

    2009-12-15

    The GRAPES-3 is a dense extensive air shower array operating with approx400 scintillator detectors and it also contains a 560 m{sup 2} tracking muon detector (E{sub m}u>1GeV), at Ooty in India. 25% of scintillator detectors are instrumented with two fast photomultiplier tubes (PMTs) for extending the dynamic range to approx5x10{sup 3} particles m{sup -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 gamma-rays from point sources is done with the aid of the muon detector. A good angular resolution of 0.7 deg. at 30 TeV, is measured from the shadow of the Moon on the isotropic flux of cosmic rays. A sensitive limit on the diffuse flux of 100 TeV gamma-rays is placed by using muon detector to filter the charged cosmic ray background. A tracking muon detector allows sensitive measurements on 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.

  18. The anisotropy of cosmic ray flux in Large Area Air Shower experiments

    International Nuclear Information System (INIS)

    The sidereal anisotropy of cosmic rays with energy in the range of 1014-1015eV was obtained by using Large Area Air Show (LAAS) experiments which deployed extensive air shower (EAS) arrays in large part of Japan. The first harmonic amplitude and phase in a function of right ascension axis are (0.23±0.04)x10-2 and 0.4±0.7 hour, respectively, and those of the second harmonics are (0.06±0.04)x10-2 and 7.5±2.6 hour, respectively. The first harmonic amplitude are compared with the diffusive mode of cosmic ray propagation, which predicts the dependence of anisotropy amplitudes on primary cosmic ray rigidities. The exponent value of rigidity dependence of diffusion coefficient is estimated as 0.34±0.01, in good agreement with Kolmogorov type spectrum of turbulence of galactic magnetic filed. Although a sky map in equatorial coordinates indicates excess and deficit regions above the isotropic expectation, their deviations were consistent with statistical ones, and more statistics are required to point the region and the opening angle of them

  19. Radio detection of extensive air showers at the Pierre Auger Observatory

    International Nuclear Information System (INIS)

    Deployed at the end of 2010 at the Pierre Auger Observatory, the first stage of the Auger Engineering Radio Array, AERA24, consists of 24 radio stations covering an area of 0.5 km2. AERA measures the radio emission from cosmic-ray induced air showers. The amplitude of this radio emission is used to constrain the characteristics of the primary particle: arrival direction, energy and nature. These studies are possible thanks to an instrumentation development allowing self-triggered and externally triggered measurements in the MHz domain and an improved understanding of radio emission processes. In May 2013, 100 new stations were installed to cover an area of ≃6 km2, for a total of 124 stations. This stage 2 will provide higher statistics and will enhance both the estimate of the nature of the primary cosmic ray and the energy resolution above 1017 eV as an addition to detectors such as the Auger fluorescence telescopes and particle detectors. We will present the main results obtained with the stage 1 of AERA and the current status of the experiment. We will end with a brief overview of the GHz-experiments installed at the Pierre Auger Observatory

  20. The wavefront of the radio signal emitted by cosmic ray air showers

    CERN Document Server

    Apel, W D; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Cantoni, E; Chiavassa, A; Daumiller, K; de Souza, V; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Fuchs, B; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmidt, A; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Zabierowski, J; Zensus, J A

    2014-01-01

    Analyzing measurements of the LOPES antenna array together with corresponding CoREAS simulations for more than 300 measured events with energy above $10^{17}$eV and zenith angles smaller than $45^\\circ$, we find that the radio wavefront of cosmic-ray air showers is of hyperbolic shape. At axis distances $\\gtrsim 50$m, the wavefront can be approximated by a simple cone. According to the simulations, the cone angle is clearly correlated with the shower maximum. Thus, we confirm earlier predictions that arrival time measurements can be used to study the longitudinal shower development, but now using a realistic wavefront. Moreover, we show that the hyperbolic wavefront is compatible with our measurement, and we present several experimental indications that the cone angle is indeed sensitive to the shower development. Consequently, the wavefront can be used to statistically study the primary composition of ultra-high energy cosmic rays. At LOPES, the experimentally achieved precision for the shower maximum is lim...

  1. Light Transmission From Extended Air Showers Produced By Cosmic-Rays and Gamma-Rays

    Science.gov (United States)

    Taylor, S. F.; Abu-Zayyad, T.; Belov, K.; Cao, Z.; Chen, G.; Jui, C. C. H.; Kieda, D. B.; Matthews, J. N.; Salamon, M.; Sokolsky, P. V.; Smith, J. D.; Sommers, P.; Springer, R. W.; Stokes, B. T.; Thomas, S. B.; Wiencke, L. R.; Matthews, J. A. J.; Clay, R. W.; Dawson, B. R.; Simpson, K.; Bells, J.; Boyer, J.; Knapp, B.; Song, B. H.; Zhang, X. Z.; SDSS Collaboration; High Resolution Fly's Eye Collaboration; Telescope Array/U. Tokyo Collaboration

    1999-05-01

    Cosmic-ray and gamma-ray experiments that use the atmosphere as a calorimeter, such as the High Resolution Fly's Eye (HiRes) and the Telescope Array (TA), require understanding the transmission of the light from the air shower of particles produced by the cosmic-ray or gamma-ray striking the atmosphere. To better understand the scattering and transmission of light to the detectors, HiRes measures light from different calibrated sources. We compare scattered light from laser shots a few kilometers away from the two HiRes detectors, with direct light from stable portable light sources placed a few meters in front of the phototubes. We use two HiRes detectors to study and isolate contributions to fluctuations of the measured light. These contributions include fluctuations in the source intensity, the night sky background, scattering and transmission of the laser beam, the phototubes and electronics, and photostatistics. The High Resolution Fly's Eye Collaboration gratefully acknowledges the support of the US National Science Foundation, DOE, the US Army's Dugway Proving Grounds, and the support of our member universities.

  2. Detection and imaging of atmospheric radio flashes from cosmic ray air showers.

    Science.gov (United States)

    Falcke, H; Apel, W D; Badea, A F; Bähren, L; Bekk, K; Bercuci, A; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Buitink, S; Brüggemann, M; Buchholz, P; Butcher, H; Chiavassa, A; Daumiller, K; de Bruyn, A G; de Vos, C M; Di Pierro, F; Doll, P; Engel, R; Gemmeke, H; Ghia, P L; Glasstetter, R; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huege, T; Kampert, K-H; Kant, G W; Klein, U; Kolotaev, Y; Koopman, Y; Krömer, O; Kuijpers, J; Lafebre, S; Maier, G; Mathes, H J; Mayer, H J; Milke, J; Mitrica, B; Morello, C; Navarra, G; Nehls, S; Nigl, A; Obenland, R; Oehlschläger, J; Ostapchenko, S; Over, S; Pepping, H J; Petcu, M; Petrovic, J; Plewnia, S; Rebel, H; Risse, A; Roth, M; Schieler, H; Schoonderbeek, G; Sima, O; Stümpert, M; Toma, G; Trinchero, G C; Ulrich, H; Valchierotti, S; van Buren, J; van Cappellen, W; Walkowiak, W; Weindl, A; Wijnholds, S; Wochele, J; Zabierowski, J; Zensus, J A; Zimmermann, D

    2005-05-19

    The nature of ultrahigh-energy cosmic rays (UHECRs) at energies >10(20) eV remains a mystery. They are likely to be of extragalactic origin, but should be absorbed within approximately 50 Mpc through interactions with the cosmic microwave background. As there are no sufficiently powerful accelerators within this distance from the Galaxy, explanations for UHECRs range from unusual astrophysical sources to exotic string physics. Also unclear is whether UHECRs consist of protons, heavy nuclei, neutrinos or gamma-rays. To resolve these questions, larger detectors with higher duty cycles and which combine multiple detection techniques are needed. Radio emission from UHECRs, on the other hand, is unaffected by attenuation, has a high duty cycle, gives calorimetric measurements and provides high directional accuracy. Here we report the detection of radio flashes from cosmic-ray air showers using low-cost digital radio receivers. We show that the radiation can be understood in terms of the geosynchrotron effect. Our results show that it should be possible to determine the nature and composition of UHECRs with combined radio and particle detectors, and to detect the ultrahigh-energy neutrinos expected from flavour mixing. PMID:15902250

  3. Comparison of big event with calculations of the air shower development

    Science.gov (United States)

    Niwa, M.; Misaki, A.; Matano, T.

    1985-01-01

    The incidence of high energy hadrons and electron-photons in air showers at various stages of development is calculated. Numerical calculation is used to solve the diffusion equation for a nuclear cascade and analytical calculation for cascade shower induced gamma rays. From these calculations, one can get the longitudinal development of the high energy hadron and electron-photon components, and the energy spectra of these components at various depths of air shower development. The total number of hadrons (N sub H) and electron-photon components (N sub gamma) are related according to stages of the air shower development and primary energy. The relation of the total energy of hadron and electron-photon component above the threshold energy is given. The energy balance between both components is also a useful parameter to study high energy events accompanying air showers. The relation of N sub H and fractional hadronic energy E (sum E sub H sup gamma/sum E sub H sup gamma + Sum E sub gamma) is calculated. This relation is helpful to understand the stage of air shower development(t) and primary energy (E sub p).

  4. Extensive Air Showers and Cosmic Ray Physics above 1017 eV

    Science.gov (United States)

    Bertaina, Mario

    2016-07-01

    Cosmic Rays above 1017 eV allow studying hadronic interactions at energies that can not be attained at accelerators yet. At the same time hadronic interaction models have to be applied to the cosmic-ray induced air-shower cascades in atmosphere to infer the nature of cosmic rays. The reliability of air-shower simulations has become the source of one of the largest systematic uncertainty in the interpretation of cosmic-ray data due to the uncertainties in modeling the hadronic interaction driving the air-shower development. This paper summarises in the first part the recent results on the cosmic ray energy spectrum, composition and anisotropy from the knee region to the GZK cutoff [1, 2] of the spectrum by means of ground-based experiments. Most of the information reported in this contribution is taken from [3-5]. Aspects interconnecting cosmic ray and particle physics are reviewed in the second part of the paper.

  5. The air shower maximum probed by Cherenkov effects from radio emission

    CERN Document Server

    de Vries, Krijn D; Werner, Klaus; 10.1016/j.astropartphys.2013.02.003

    2013-01-01

    Radio detection of cosmic-ray-induced air showers has come to a flight the last decade. Along with the experimental efforts, several theoretical models were developed. The main radio-emission mechanisms are established to be the geomagnetic emission due to deflection of electrons and positrons in Earth's magnetic field and the charge-excess emission due to a net electron excess in the air shower front. It was only recently shown that Cherenkov effects play an important role in the radio emission from air showers. In this article we show the importance of these effects to extract quantitatively the position of the shower maximum from the radio signal, which is a sensitive measure for the mass of the initial cosmic ray. We also show that the relative magnitude of the charge-excess and geomagnetic emission changes considerably at small observer distances where Cherenkov effects apply.

  6. Influence of atmospheric electric fields on the radio emission from extensive air showers

    Science.gov (United States)

    Trinh, T. N. G.; Scholten, O.; Buitink, S.; van den Berg, A. M.; Corstanje, A.; Ebert, U.; Enriquez, J. E.; Falcke, H.; Hörandel, J. R.; Köhn, C.; Nelles, A.; Rachen, J. P.; Rossetto, L.; Rutjes, C.; Schellart, P.; Thoudam, S.; ter Veen, S.; de Vries, K. D.

    2016-01-01

    The atmospheric electric fields in thunderclouds have been shown to significantly modify the intensity and polarization patterns of the radio footprint of cosmic-ray-induced extensive air showers. Simulations indicated a very nonlinear dependence of the signal strength in the frequency window of 30-80 MHz on the magnitude of the atmospheric electric field. In this work we present an explanation of this dependence based on Monte Carlo simulations, supported by arguments based on electron dynamics in air showers and expressed in terms of a simplified model. We show that by extending the frequency window to lower frequencies, additional sensitivity to the atmospheric electric field is obtained.

  7. Influence of Atmospheric Electric Fields on the Radio Emission from Extensive Air Showers

    CERN Document Server

    Trinh, T N G; Buitink, S; Berg, A M van den; Corstanje, A; Ebert, U; Enriquez, J E; Falcke, H; Hörandel, J R; Köhn, C; Nelles, A; Rachen, J P; Rossetto, L; Rutjes, C; Schellart, P; Thoudam, S; ter Veen, S; de Vries, K D

    2016-01-01

    The atmospheric electric fields in thunderclouds have been shown to significantly modify the intensity and polarization patterns of the radio footprint of cosmic-ray-induced extensive air showers. Simulations indicated a very non-linear dependence of the signal strength in the frequency window of 30-80 MHz on the magnitude of the atmospheric electric field. In this work we present an explanation of this dependence based on Monte-Carlo simulations, supported by arguments based on electron dynamics in air showers and expressed in terms of a simplified model. We show that by extending the frequency window to lower frequencies additional sensitivity to the atmospheric electric field is obtained.

  8. The Study of extensive air Shower (EAS)by four scintillation detectors

    International Nuclear Information System (INIS)

    Particles of an Extensive Air Shower, generated by a single high energy particle incident on the top of the atmosphere, may be delayed with respect to one another at the plane of observation because: (a) path lengths differ as the result of scattering, (b) velocities may differ, (c) the axis of the shower may not be perpendicular to the plane of observation. We have studied the distribution of cosmic rays in extensive air showers at Tehran level by measuring the relative delay between particles with four scintillation detectors. These measurements were carried out at department of physics, Sharif University of Technology, Tehran, Iran

  9. Effects of massive photons from the dark sector on the muon content in extensive air showers

    International Nuclear Information System (INIS)

    Inspired by recent astrophysical observations of leptonic excesses measured by satellite experiments, we consider the impact of some general models of the dark sector on the muon production in extensive air showers. We present a compact approximative expression for the bremsstrahlung of a massive photon from an electron and use it within Monte Carlo simulations to estimate the amount of weakly interacting photon-like massive particles that could be produced in an extensive air shower. We find that the resulting muon production is by many orders of magnitude below the average muon count in a shower and thus unobservable

  10. Sensitivity of the JEM-EUSO telescope to gravity effects in neutrino-induced air showers

    CERN Document Server

    Mladenov, Stefan; Tsenov, Roumen; Bertaina, Mario; Santangelo, Andrea

    2015-01-01

    We examine the JEM-EUSO sensitivity to gravity effects in the context of Randall-Sundrum (RS) model with a single extra dimension and small curvature of the metric. Exchanges of reggeized Kaluza-Klein gravitons in the $t$-channel contribute to the inelastic cross-section for scattering of ultra-high-energy neutrinos off nucleons. Such effects can be detected in deeply penetrating quasi-horizontal air showers induced by interactions of cosmic neutrinos with atmospheric nucleons. For this reason, we calculate the expected number of quasi-horizontal air showers at the JEM-EUSO observatory as a function of two parameters of the RS model.

  11. Muon Arrival Time Distributions of Simulated Extensive Air Showers in View of Mass Discrimination

    International Nuclear Information System (INIS)

    By extensive Monte Carlo simulations of Extensive Air Showers (EAS), using the EAS simulation co de CORSIKA, arrival time distributions of the EAS muon have been generated for iron, oxygen and proton induced air showers using different hadronic interaction models as Monte Carlo generators. The muon time profiles up to distances of 310 m from the core position have been obtained for different primaries. Applying non-parametric statistical inference methods it is shown that a reliable determination of the shower age, correlated with the time parameters would lead to a relatively good discrimination of showers of different primary mass. (author)

  12. Air-Showers in Space and Z-Showers in Universe for Neutrino Astronomy and Spectroscopy

    OpenAIRE

    Fargion, D.

    2006-01-01

    Amplified Tau-airshower at horizons may well open a novel powerful windows, at PeV-EeV energy, to Neutrino Astronomy. Neutrino induced air-showering astronomy rise because of neutrino masses, their mixing and the consequent replenishment of tau flavor during neutrino flight into spaces; Tau-Air-Showers escaping the Earth are the main traces amplified by its millions muon, billions gamma and thousand billions photon secondaries. Earth edges and its sharp shadows is the huge beam-dump detector ...

  13. The wavefront of the radio signal emitted by cosmic ray air showers

    International Nuclear Information System (INIS)

    Analyzing measurements of the LOPES antenna array together with corresponding CoREAS simulations for more than 300 measured events with energy above 1017 eV and zenith angles smaller than 45o, we find that the radio wavefront of cosmic-ray air showers is of approximately hyperbolic shape. The simulations predict a slightly steeper wavefront towards East than towards West, but this asymmetry is negligible against the measurement uncertainties of LOPES. At axis distances ∼> 50 m, the wavefront can be approximated by a simple cone. According to the simulations, the cone angle is clearly correlated with the shower maximum. Thus, we confirm earlier predictions that arrival time measurements can be used to study the longitudinal shower development, but now using a realistic wavefront. Moreover, we show that the hyperbolic wavefront is compatible with our measurement, and we present several experimental indications that the cone angle is indeed sensitive to the shower development. Consequently, the wavefront can be used to statistically study the primary composition of ultra-high energy cosmic rays. At LOPES, the experimentally achieved precision for the shower maximum is limited by measurement uncertainties to approximately 140 g/c 2. But the simulations indicate that under better conditions this method might yield an accuracy for the atmospheric depth of the shower maximum, Xmax, better than 30 g/c 2. This would be competitive with the established air-fluorescence and air-Cherenkov techniques, where the radio technique offers the advantage of a significantly higher duty-cycle. Finally, the hyperbolic wavefront can be used to reconstruct the shower geometry more accurately, which potentially allows a better reconstruction of all other shower parameters, too

  14. The wavefront of the radio signal emitted by cosmic ray air showers

    Science.gov (United States)

    Apel, W. D.; Arteaga-Velázquez, J. C.; Bähren, L.; Bekk, K.; Bertaina, M.; Biermann, P. L.; Blümer, J.; Bozdog, H.; Brancus, I. M.; Cantoni, E.; Chiavassa, A.; Daumiller, K.; de Souza, V.; Di Pierro, F.; Doll, P.; Engel, R.; Falcke, H.; Fuchs, B.; Gemmeke, H.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J. R.; Horneffer, A.; Huber, D.; Huege, T.; Isar, P. G.; Kampert, K.-H.; Kang, D.; Krömer, O.; Kuijpers, J.; Link, K.; Łuczak, P.; Ludwig, M.; Mathes, H. J.; Melissas, M.; Morello, C.; Oehlschläger, J.; Palmieri, N.; Pierog, T.; Rautenberg, J.; Rebel, H.; Roth, M.; Rühle, C.; Saftoiu, A.; Schieler, H.; Schmidt, A.; Schoo, S.; Schröder, F. G.; Sima, O.; Toma, G.; Trinchero, G. C.; Weindl, A.; Wochele, J.; Zabierowski, J.; Zensus, J. A.

    2014-09-01

    Analyzing measurements of the LOPES antenna array together with corresponding CoREAS simulations for more than 300 measured events with energy above 1017 eV and zenith angles smaller than 45o, we find that the radio wavefront of cosmic-ray air showers is of approximately hyperbolic shape. The simulations predict a slightly steeper wavefront towards East than towards West, but this asymmetry is negligible against the measurement uncertainties of LOPES. At axis distances gtrsim 50 m, the wavefront can be approximated by a simple cone. According to the simulations, the cone angle is clearly correlated with the shower maximum. Thus, we confirm earlier predictions that arrival time measurements can be used to study the longitudinal shower development, but now using a realistic wavefront. Moreover, we show that the hyperbolic wavefront is compatible with our measurement, and we present several experimental indications that the cone angle is indeed sensitive to the shower development. Consequently, the wavefront can be used to statistically study the primary composition of ultra-high energy cosmic rays. At LOPES, the experimentally achieved precision for the shower maximum is limited by measurement uncertainties to approximately 140 g/c 2. But the simulations indicate that under better conditions this method might yield an accuracy for the atmospheric depth of the shower maximum, Xmax, better than 30 g/c 2. This would be competitive with the established air-fluorescence and air-Cherenkov techniques, where the radio technique offers the advantage of a significantly higher duty-cycle. Finally, the hyperbolic wavefront can be used to reconstruct the shower geometry more accurately, which potentially allows a better reconstruction of all other shower parameters, too.

  15. Atmospheric Cerenkov light from large air showers observed at 5200m above sea level

    International Nuclear Information System (INIS)

    A preliminary result is presented on the arrival-time distribution of atmospheric Cerenkov light from air showers of 1017 eV observed at Chacaltaya. The rise time and the FWHM are consistent with those expected from high multiplicity models, indicating the very fast development of electrons at the early stage

  16. The EHISTORY option of the air-shower simulation program CORSIKA

    Energy Technology Data Exchange (ETDEWEB)

    Heck, D.; Engel, R.

    2009-07-01

    This report describes the EHISTORY option, which gives additional information for all muons arriving at the detector level on their precursors, the grandmother and mother particles. These may help to improve the understanding of the production and propagation of muons in air showers. (orig.)

  17. Detection of extensive cosmic air showers by small scintillation detectors with wavelength-shifting fibres

    International Nuclear Information System (INIS)

    A set of three small scintillation detectors was employed to measure correlated events due to the passage of cosmic muons originating from extensive air showers. The coincidence rate between (any) two detectors was extracted as a function of their relative distance. The difference between the arrival times in three non-aligned detectors was used to reconstruct the orientation of the shower axis. (paper)

  18. Lateral distribution of radio emission and its dependence on air shower longitudinal development

    International Nuclear Information System (INIS)

    The lateral distribution function (LDF) of radio emission from an extensive air shower is considered as the basic signature sensitive to the shower longitudinal development and, as a consequence, to the mass of a primary cosmic ray's particle that initiated a given shower. The peculiarities in the LDF's structure as well as their sensitivity to the height of shower maximum are investigated and explained

  19. Search for long-lived massive particles in extensive air showers

    Science.gov (United States)

    Kawamoto, M.; Inoue, N.; Misaki, Y.; Manabe, O.; Takeuchi, T.; Toyoda, Y.

    1985-01-01

    Air showers containing delayed sub-showers which may be produced by a long-lived massive particle have been investigated by using twelve detectors. Ten events have been selected out as the candidates. However, a definite conclusion cannot be reached at the present time.

  20. Detection of Extensive Cosmic Air Showers by Small Scintillation Detectors with Wavelength-Shifting Fibres

    Science.gov (United States)

    Aiola, Salvatore; La Rocca, Paola; Riggi, Francesco; Riggi, Simone

    2012-01-01

    A set of three small scintillation detectors was employed to measure correlated events due to the passage of cosmic muons originating from extensive air showers. The coincidence rate between (any) two detectors was extracted as a function of their relative distance. The difference between the arrival times in three non-aligned detectors was used…

  1. Radio emission from cosmic ray air showers : simulation results and parametrization

    NARCIS (Netherlands)

    Huege, T.; Falcke, H.D.E.

    2005-01-01

    We have developed a sophisticated model of the radio emission from extensive air showers in the scheme of coherent geosynchrotron radiation, providing a theoretical foundation for the interpretation of experimental data from current and future experiments. Having verified the model through compariso

  2. Prospects for radar detection of cosmic ray air showers with medium-frequency radio waves

    International Nuclear Information System (INIS)

    We show that the highly relativistic motion of an extensive air shower allows one to increase the wavelength of the radar signal above its transverse size without giving rise to signal scattering. This increases the efficiency of detection due to an increase in the reflection from the shower and a lower level of sky noise in the frequency range of the reflected signal. (paper)

  3. Influence of atmospheric electric fields on the radio emission from extensive air showers

    DEFF Research Database (Denmark)

    Trinh, T. N. G.; Scholten, O.; Buitink, S.;

    2016-01-01

    The atmospheric electric fields in thunderclouds have been shown to significantly modify the intensity and polarization patterns of the radio footprint of cosmic-ray-induced extensive air showers. Simulations indicated a very nonlinear dependence of the signal strength in the frequency window of ...

  4. Effects of massive photons from the dark sector on the muon content in extensive air showers

    Czech Academy of Sciences Publication Activity Database

    Ebr, Jan; Nečesal, Petr

    2013-01-01

    Roč. 725, 4-5 (2013), s. 185-189. ISSN 0370-2693 R&D Projects: GA MŠk(CZ) LA08016 Institutional support: RVO:68378271 Keywords : dark matter * bremsstrahlung * extensive air shower * muon production Subject RIV: BF - Elementary Particles and High Energy Physics Impact factor: 6.019, year: 2013

  5. Radio emission from Air Showers. Comparison of theoretical approaches

    CERN Document Server

    Belov, Konstantin

    2013-01-01

    While the fluorescence and the ground counter techniques for the detection of ultra-high energy cosmic rays (UHECR) were being developed for decades, the interest in the radio detection diminished after the initial experiments in the 1960s. As a result, the fluorescence and the surface array techniques are more mature today, providing more reliable measurements of the primary cosmic particle energy, chemical composition and the inelastic cross-section. The advantages of the radio technique are 100 percent duty cycle and lower deployment and operational costs. Thus, the radio technique can greatly complement the fluorescence and the ground array detection and can also work independently. With the ANITA balloon detector observing UHECRs and the success of LOPES, CODALEMA and other surface radio detectors, the radio technique received a significant boost in recent years. Reliable Monte Carlo (MC) simulations are needed in order to obtain the energy and other parameters of the primary cosmic ray particle from the...

  6. First results of the air shower experiment KASCADE

    International Nuclear Information System (INIS)

    The main goals of the KASCADE (KArlsruhe Shower Core and Array DEtector) experiment are the determination of the energy spectrum and elemental composition of the charged cosmic rays in the energy range around the knee at ∼ 5 PeV. Due to the large number of measured observables per single shower a variety of different approaches are applied to the data, preferably on an event-by-event basis. First results are presented and the influence of the high-energy interaction models underlying the analyses is discussed

  7. Studies of Cosmic Ray Composition and Air Shower Structure with the Pierre Auger Observatory

    Energy Technology Data Exchange (ETDEWEB)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Measurement of the average depth of shower maximum and its fluctuations with the Pierre Auger Observatory; (2) Study of the nuclear mass composition of UHECR with the surface detectors of the Pierre Auger Observatory; (3) Comparison of data from the Pierre Auger Observatory with predictions from air shower simulations: testing models of hadronic interactions; (4) A Monte Carlo exploration of methods to determine the UHECR composition with the Pierre Auger Observatory; (5) The delay of the start-time measured with the Pierre Auger Observatory for inclined showers and a comparison of its variance with models; (6) UHE neutrino signatures in the surface detector of the Pierre Auger Observatory; and (7) The electromagnetic component of inclined air showers at the Pierre Auger Observatory.

  8. Detection of Cherenkov light from air showers with Geiger-APDs

    CERN Document Server

    Otte, A N; Biland, A; Göbel, F; Lorenz, E; Pauss, F; Renker, D; Röser, U; Schweizer, T

    2007-01-01

    We have detected Cherenkov light from air showers with Geiger-mode APDs (G-APDs). G-APDs are novel semiconductor photon-detectors, which offer several advantages compared to conventional photomultiplier tubes in the field of ground-based gamma-ray astronomy. In a field test with the MAGIC telescope we have tested the efficiency of a G-APD / light catcher setup to detect Cherenkov light from air showers. We estimate a detection efficiency, which is 60% higher than the efficiency of a MAGIC camera pixel. Ambient temperature dark count rates of the tested G-APDs are below the rates of the night sky light background. According to these recent tests G-APDs promise a major progress in ground-based gamma-ray astronomy.

  9. Measurement of muon content in inclined air showers above 4 x 1018 eV

    International Nuclear Information System (INIS)

    The Pierre Auger Observatory in Malarguee, Argentina, is sensitive to air showers up to almost horizontal angles of incidence. Air showers with zenith angles between 60 and 80 degrees are suited to measure the muon component of the shower with the Auger Surface Detector since the primary electromagnetic component gets absorbed in the atmosphere before the shower reaches ground. Some of those events are also observed by the Fluorescence Detector which allows us to determine the total energy of the shower independent of the Surface Detector. Based on these hybrids events the size of muon component for a given cosmic ray energy is determined, which can then be compared to model predictions. We present an update of this analysis.

  10. Calculation of molecular bremsstrahlung radiation and air shower plasma conditions for CROME

    International Nuclear Information System (INIS)

    The possibility of the detection of extensive air showers by observation of isotropic microwave radiation due to molecular bremsstrahlung has been proposed in 2008. Ionization electrons, forming a short-lived, tenuous plasma in the wake of the shower, interact with atmospheric neutrals and produce bremsstrahlung. Concurrent with first measurements of microwave radiation by the CROME experiment in Karlsruhe, an independent, theory based model for emission of isotropic bremsstrahlung emission has been developed. In this talk, the assumptions of the model for bremsstrahlung emission and the findings concerning the state of the plasma in an air shower are discussed. The magnitude of the expected signal is calculated and compared to predictions made in the original proposal by Gorham et al. and to the observed GHz signals.

  11. Simulation of the charge ratio of cosmic ray muons in extensive air showers using CORSIKA

    International Nuclear Information System (INIS)

    The interaction of primary cosmic rays in the atmosphere produces, among other particles, pions and kaons. They decay to muons, which form an important component of extensive air showers. The ratio of positively to negatively charged muons, called the muon charge ratio, provides important information about the cosmic ray interactions in the atmosphere. In this study, the theoretical hadronic interaction models in the cosmic ray simulation code CORSIKA have been used to study the charge ratio of cosmic ray muons simulated in extensive air showers. An East - West effect on the charge ratio of simulated cosmic ray muons is observed. It is more pronounced for inclined and low-energy muons (momentum less than 100 GeV/c and zenith angle greater than 80 ). Experimental data from ''MINOS Near'' experiment gives similar results.

  12. Atmospheric Profiles at the Southern Pierre Auger Observatory and their Relevance to Air Shower Measurement

    CERN Document Server

    Keilhauer, B; Engel, R; Gora, D; Homola, P; Klages, H; Pekala, J; Risse, M; Unger, M; Wilczynska, B; Wilczynski, H

    2005-01-01

    The dependence of atmospheric conditions on altitude and time have to be known at the site of an air shower experiment for accurate reconstruction of extensive air showers and their simulations. The height-profile of atmospheric depth is of particular interest as it enters directly into the reconstruction of longitudinal shower development and of the primary energy and mass of cosmic rays. For the southern part of the Auger Observatory, the atmosphere has been investigated in a number of campaigns with meteorological radio soundings and with continuous measurements of ground-based weather stations. Focussing on atmospheric depth and temperature profiles, temporal variations are described and monthly profiles are developed. Uncertainties of the monthly atmospheres that are currently applied in the Auger reconstruction are discussed.

  13. The Roland Maze Project - school-based extensive air shower network

    International Nuclear Information System (INIS)

    We plan to construct the large area network of extensive air shower detectors placed on the roofs of high school buildings in the city of Lodz. Detection points will be connected by INTERNET to the central server and their work will be synchronized by GPS. The main scientific goal of the project are studies of ultra high energy cosmic rays. Using existing town infrastructure (INTERNET, power supply, etc.) will significantly reduce the cost of the experiment. Engaging high school students in the research program should significantly increase their knowledge of science and modern technologies, and can be a very efficient way of science popularisation. We performed simulations of the projected network capabilities of registering Extensive Air Showers and reconstructing energies of primary particles. Results of the simulations and the current status of project realisation will be presented

  14. The Auger Engineering Radio Array and multi-hybrid cosmic ray detection

    Science.gov (United States)

    Holt, E. M.; Pierre Auger Collaboration

    2016-05-01

    The Auger Engineering Radio Array (AERA) aims at the detection of air showers induced by high-energy cosmic rays. As an extension of the Pierre Auger Observatory, it measures complementary information to the particle detectors, fluorescence telescopes and to the muon scintillators of the Auger Muons and Infill for the Ground Array (AMIGA). AERA is sensitive to all fundamental parameters of an extensive air shower such as the arrival direction, energy and depth of shower maximum. Since the radio emission is induced purely by the electromagnetic component of the shower, in combination with the AMIGA muon counters, AERA is perfect for separate measurements of the electrons and muons in the shower, if combined with a muon counting detector like AMIGA. In addition to the depth of the shower maximum, the ratio of the electron and muon number serves as a measure of the primary particle mass.

  15. New method for the time calibration of an interferometric radio antenna array

    CERN Document Server

    Schröder, F G; Bähren, L; Blümer, J; Bozdog, H; Falcke, H; Haungs, A; Horneffer, A; Huege, T; Isar, P G; Krömer, O; Nehls, S; 10.1016/j.nima.2010.01.072

    2010-01-01

    Digital radio antenna arrays, like LOPES (LOFAR PrototypE Station), detect high-energy cosmic rays via the radio emission from atmospheric extensive air showers. LOPES is an array of dipole antennas placed within and triggered by the KASCADE-Grande experiment on site of the Karlsruhe Institute of Technology, Germany. The antennas are digitally combined to build a radio interferometer by forming a beam into the air shower arrival direction which allows measurements even at low signal-to-noise ratios in individual antennas. This technique requires a precise time calibration. A combination of several calibration steps is used to achieve the necessary timing accuracy of about 1 ns. The group delays of the setup are measured, the frequency dependence of these delays (dispersion) is corrected in the subsequent data analysis, and variations of the delays with time are monitored. We use a transmitting reference antenna, a beacon, which continuously emits sine waves at known frequencies. Variations of the relative del...

  16. Simulation of air shower image in fluorescence light based on energy deposits derived from CORSIKA

    OpenAIRE

    Gora, D.; Heck, D.; Homola, P.; Klages, H.; Pekala, J.; Risse, M.; Wilczynska, B.; Wilczynski, H.

    2004-01-01

    Spatial distributions of energy deposited by an extensive air shower in the atmosphere through ionization, as obtained from the CORSIKA simulation program, are used to find the fluorescence light distribution in the optical image of the shower. The shower image derived in this way is somewhat smaller than that obtained from the NKG lateral distribution of particles in the shower. The size of the image shows a small dependence on the primary particle type.

  17. Photon air showers at ultra-high energy and the photonuclear cross-section

    OpenAIRE

    Risse, M.; Homola, P.; Engel, R.; Gora, D.; Heck, D.; Pekala, J.; Wilczynska, B.; Wilczynski, H.

    2005-01-01

    Experimental conclusions from air shower observations on cosmic-ray photons above 10^19 eV are based on the comparison to detailed shower simulations. For the calculations, the photonuclear cross-section needs to be extrapolated over several orders of magnitude in energy. The uncertainty from the cross-section extrapolation translates into an uncertainty of the predicted shower features for primary photons and, thus, into uncertainties for a possible data interpretation. After briefly reviewi...

  18. Primary Particle Type of the Most Energetic Fly's Eye Air Shower

    OpenAIRE

    Risse, M.; Homola, P.; Gora, D.; Pekala, J.; Wilczynska, B.; Wilczynski, H.

    2004-01-01

    The longitudinal profile of the most energetic cosmic-ray air shower measured so far, the event recorded by the Fly's Eye detector with a reconstructed primary energy of about 320 EeV, is compared to simulated shower profiles. The calculations are performed with the CORSIKA code and include primary photons and different hadron primaries. For primary photons, preshower formation in the geomagnetic field is additionally treated in detail. For primary hadrons, the hadronic interaction models QGS...

  19. Constraints on hadronic models in extensive air showers with the Pierre Auger Observatory

    CERN Document Server

    ,

    2016-01-01

    Extensive air showers initiated by ultra-high energy cosmic rays are sensitive to the details of hadronic interactions models, so we present the main results obtained using the data of the Pierre Auger Observatory. The depth at which the maximum of the electromagnetic development takes place is the most sensitive parameter to infer the nature of the cosmic rays. However, the hadronic models cannot describe consistently the maximum and the muon measurements at energies higher than those reached at the LHC.

  20. Depth of maximum of air-shower profiles at the Pierre Auger Observatory. II. Composition implications

    Czech Academy of Sciences Publication Activity Database

    Aab, A.; Abreu, P.; Aglietta, M.; Boháčová, Martina; Chudoba, Jiří; Ebr, Jan; Mandát, Dušan; Nečesal, Petr; Palatka, Miroslav; Pech, Miroslav; Prouza, Michael; Řídký, Jan; Schovánek, Petr; Trávníček, Petr; Vícha, Jakub

    2014-01-01

    Roč. 90, č. 12 (2014), "122006-1"-"122006-12". ISSN 1550-7998 R&D Projects: GA MŠk(CZ) LG13007; GA MŠk(CZ) 7AMB14AR005; GA ČR(CZ) GA14-17501S Institutional support: RVO:68378271 Keywords : Pierre Auger Observatory * air-shower * fluorescence telescopes Subject RIV: BF - Elementary Particles and High Energy Physics Impact factor: 4.643, year: 2014

  1. Muons in air showers at the Pierre Auger Observatory: mean number in highly inclined events

    Czech Academy of Sciences Publication Activity Database

    Aab, A.; Abreu, P.; Aglietta, M.; Boháčová, Martina; Chudoba, Jiří; Ebr, Jan; Mandát, Dušan; Nečesal, Petr; Palatka, Miroslav; Pech, Miroslav; Prouza, Michael; Řídký, Jan; Schovánek, Petr; Trávníček, Petr; Vícha, Jakub

    2015-01-01

    Roč. 91, č. 3 (2015), , "032003-1"-"032003-12". ISSN 1550-7998 R&D Projects: GA MŠk(CZ) LG13007; GA MŠk(CZ) 7AMB14AR005; GA ČR(CZ) GA14-17501S Institutional support: RVO:68378271 Keywords : Pierre Auger Observatory * air showers * ultrahigh energies * cosmic rays * detector Subject RIV: BF - Elementary Particles and High Energy Physics Impact factor: 4.643, year: 2014

  2. Muons in air showers at the Pierre Auger Observatory: measurement of atmospheric production depth

    Czech Academy of Sciences Publication Activity Database

    Aab, A.; Abreu, P.; Aglietta, M.; Boháčová, Martina; Chudoba, Jiří; Ebr, Jan; Mandát, Dušan; Nečesal, Petr; Palatka, Miroslav; Pech, Miroslav; Prouza, Michael; Řídký, Jan; Schovánek, Petr; Trávníček, Petr; Vícha, Jakub

    2014-01-01

    Roč. 90, č. 1 (2014), "012012-1"-"012012-15". ISSN 1550-7998 R&D Projects: GA ČR(CZ) GA14-17501S; GA MŠk(CZ) 7AMB14AR005; GA MŠk(CZ) LG13007 Institutional support: RVO:68378271 Keywords : Pierre Auger Observatory * detector * cosmic rays * muon s * air showers Subject RIV: BF - Elementary Particles and High Energy Physics Impact factor: 4.643, year: 2014

  3. LOPES 3D - vectorial measurements of radio emission from cosmic ray induced air showers

    CERN Document Server

    Apel, W D; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Chiavassa, A; Daumiller, K; de Souza, V; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Fuchs, B; Fuhrmann, D; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmidt, A; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Zabierowski, J; Zensus, J A

    2013-01-01

    LOPES 3D is able to measure all three components of the electric field vector of the radio emission from air showers. This allows a better comparison with emission models. The measurement of the vertical component increases the sensitivity to inclined showers. By measuring all three components of the electric field vector LOPES 3D demonstrates by how much the reconstruction accuracy of primary cosmic ray parameters increases. Thus LOPES 3D evaluates the usefulness of vectorial measurements for large scale applications.

  4. Accelerator Measurements of Magnetically Induced Radio Emission from Particle Cascades with Applications to Cosmic-Ray Air Showers.

    Science.gov (United States)

    Belov, K; Mulrey, K; Romero-Wolf, A; Wissel, S A; Zilles, A; Bechtol, K; Borch, K; Chen, P; Clem, J; Gorham, P W; Hast, C; Huege, T; Hyneman, R; Jobe, K; Kuwatani, K; Lam, J; Liu, T C; Nam, J; Naudet, C; Nichol, R J; Rauch, B F; Rotter, B; Saltzberg, D; Schoorlemmer, H; Seckel, D; Strutt, B; Vieregg, A G; Williams, C

    2016-04-01

    For 50 years, cosmic-ray air showers have been detected by their radio emission. We present the first laboratory measurements that validate electrodynamics simulations used in air shower modeling. An experiment at SLAC provides a beam test of radio-frequency (rf) radiation from charged particle cascades in the presence of a magnetic field, a model system of a cosmic-ray air shower. This experiment provides a suite of controlled laboratory measurements to compare to particle-level simulations of rf emission, which are relied upon in ultrahigh-energy cosmic-ray air shower detection. We compare simulations to data for intensity, linearity with magnetic field, angular distribution, polarization, and spectral content. In particular, we confirm modern predictions that the magnetically induced emission in a dielectric forms a cone that peaks at the Cherenkov angle and show that the simulations reproduce the data within systematic uncertainties. PMID:27104694

  5. Accelerator Measurements of Magnetically Induced Radio Emission from Particle Cascades with Applications to Cosmic-Ray Air Showers

    Science.gov (United States)

    Belov, K.; Mulrey, K.; Romero-Wolf, A.; Wissel, S. A.; Zilles, A.; Bechtol, K.; Borch, K.; Chen, P.; Clem, J.; Gorham, P. W.; Hast, C.; Huege, T.; Hyneman, R.; Jobe, K.; Kuwatani, K.; Lam, J.; Liu, T. C.; Nam, J.; Naudet, C.; Nichol, R. J.; Rauch, B. F.; Rotter, B.; Saltzberg, D.; Schoorlemmer, H.; Seckel, D.; Strutt, B.; Vieregg, A. G.; Williams, C.; T-510 Collaboration

    2016-04-01

    For 50 years, cosmic-ray air showers have been detected by their radio emission. We present the first laboratory measurements that validate electrodynamics simulations used in air shower modeling. An experiment at SLAC provides a beam test of radio-frequency (rf) radiation from charged particle cascades in the presence of a magnetic field, a model system of a cosmic-ray air shower. This experiment provides a suite of controlled laboratory measurements to compare to particle-level simulations of rf emission, which are relied upon in ultrahigh-energy cosmic-ray air shower detection. We compare simulations to data for intensity, linearity with magnetic field, angular distribution, polarization, and spectral content. In particular, we confirm modern predictions that the magnetically induced emission in a dielectric forms a cone that peaks at the Cherenkov angle and show that the simulations reproduce the data within systematic uncertainties.

  6. Cosmic ray simulation and dependence of maximum air shower development (Hmax on mass and energy of primaries temperature

    Directory of Open Access Journals (Sweden)

    G. Rastgarzadeh

    2006-06-01

    Full Text Available   Monte Carlo simulation with CORSIKA code using QGSJET hadronic interaction model is applied on more than 5000 cosmic ray primaries to investigate dependence of maximum air shower development (Hmax on mass and energy of primaries.

  7. Radio detection of cosmic ray air showers in the digital era

    CERN Document Server

    Huege, T

    2016-01-01

    In 1965 it was discovered that cosmic ray air showers emit impulsive radio signals at frequencies below 100 MHz. After a period of intense research in the 1960s and 1970s, however, interest in the detection technique faded almost completely. With the availability of powerful digital signal processing techniques, new attempts at measuring cosmic ray air showers via their radio emission were started at the beginning of the new millennium. Starting with modest, small-scale digital prototype setups, the field has evolved, matured and grown very significantly in the past decade. Today's second-generation digital radio detection experiments consist of up to hundreds of radio antennas or cover areas of up to 17 km$^{2}$. We understand the physics of the radio emission in extensive air showers in detail and have developed analysis strategies to accurately derive from radio signals parameters which are related to the astrophysics of the primary cosmic ray particles, in particular their energy, arrival direction and es...

  8. Measurement of cosmic-ray air showers with the Tunka Radio Extension (Tunka-Rex)

    Science.gov (United States)

    Bezyazeekov, P. A.; Budnev, N. M.; Gress, O. A.; Haungs, A.; Hiller, R.; Huege, T.; Kazarina, Y.; Kleifges, M.; Konstantinov, E. N.; Korosteleva, E. E.; Kostunin, D.; Krömer, O.; Kuzmichev, L. A.; Levinson, E.; Lubsandorzhiev, N.; Mirgazov, R. R.; Monkhoev, R.; Pakhorukov, A.; Pankov, L.; Prosin, V. V.; Rubtsov, G. I.; Rühle, C.; Schröder, F. G.; Wischnewski, R.; Zagorodnikov, A.

    2015-12-01

    Tunka-Rex is a radio detector for cosmic-ray air showers in Siberia, triggered by Tunka-133, a co-located air-Cherenkov detector. The main goal of Tunka-Rex is the cross-calibration of the two detectors by measuring the air-Cherenkov light and the radio signal emitted by the same air showers. This way we can explore the precision of the radio-detection technique, especially for the reconstruction of the primary energy and the depth of the shower maximum. The latter is sensitive to the mass of the primary cosmic-ray particles. In this paper we describe the detector setup and explain how electronics and antennas have been calibrated. The analysis of data of the first season proves the detection of cosmic-ray air showers and therefore, the functionality of the detector. We confirm the expected dependence of the detection threshold on the geomagnetic angle and the correlation between the energy of the primary cosmic-ray particle and the radio amplitude. Furthermore, we compare reconstructed amplitudes of radio pulses with predictions from CoREAS simulations, finding agreement within the uncertainties.

  9. REAS3: A revised implementation of the geosynchrotron model for radio emission from air showers

    International Nuclear Information System (INIS)

    Over the past years, the freely available Monte Carlo-code REAS which simulates radio emission from air showers based on the geosynchrotron model, was used regularly for comparisons with data. However, it emerged that in the previous version of the code, emission due to the variation of the number of charged particles within an air shower was not taken into account. In the following article, we show the implementation of these emission contributions in REAS3 by the inclusion of “end-point contributions” and discuss the changes on the predictions of REAS obtained by this revision. The basis for describing radiation processes is an universal description which is gained by the use of the end-point formulation. Hence, not only pure geomagnetic radiation is simulated with REAS3 but also radiation due to the variation of the net charge excess in the air shower, independent of the Earth's magnetic field. Furthermore, we present a comparison of lateral distributions of LOPES data with REAS3-simulated distributions. The comparison shows a good agreement between both, data and REAS3 simulations.

  10. Method to calibrate the absolute energy scale of air showers with ultrahigh energy photons.

    Science.gov (United States)

    Homola, Piotr; Risse, Markus

    2014-04-18

    Calibrating the absolute energy scale of air showers initiated by ultrahigh energy (UHE) cosmic rays is an important experimental issue. Currently, the corresponding systematic uncertainty amounts to 14%-21% using the fluorescence technique. Here, we describe a new, independent method which can be applied if ultrahigh energy photons are observed. While such photon-initiated showers have not yet been identified, the capabilities of present and future cosmic-ray detectors may allow their discovery. The method makes use of the geomagnetic conversion of UHE photons (preshower effect), which significantly affects the subsequent longitudinal shower development. The conversion probability depends on photon energy and can be calculated accurately by QED. The comparison of the observed fraction of converted photon events to the expected one allows the determination of the absolute energy scale of the observed photon air showers and, thus, an energy calibration of the air shower experiment. We provide details of the method and estimate the accuracy that can be reached as a function of the number of observed photon showers. Already a very small number of UHE photons may help to test and fix the absolute energy scale. PMID:24785024

  11. Extensive Air Showers and Ultra High-Energy Cosmic Rays: A Historical Review

    CERN Document Server

    Kampert, Karl-Heinz

    2012-01-01

    The discovery of extensive air showers by Rossi, Schmeiser, Bothe, Kolh\\"orster and Auger at the end of the 1930s, facilitated by the coincidence technique of Bothe and Rossi, led to fundamental contributions in the field of cosmic ray physics and laid the foundation for high-energy particle physics. Soon after World War II a cosmic ray group at MIT in the USA pioneered detailed investigations of air shower phenomena and their experimental skill laid the foundation for many of the methods and much of the instrumentation used today. Soon interests focussed on the highest energies requiring much larger detectors to be operated. The first detection of air fluorescence light by Japanese and US groups in the early 1970s marked an important experimental breakthrough towards this end as it allowed huge volumes of atmosphere to be monitored by optical telescopes. Radio observations of air showers, pioneered in the 1960s, are presently experiencing a renaissance and may revolutionise the field again. In the last 7 dec...

  12. Monte Carlo simulations of geosynchrotron radio emission from CORSIKA-simulated air showers

    CERN Document Server

    Huege, T; Engel, R

    2006-01-01

    We present simulations performed with REAS2, a new Monte Carlo code for the calculation of geosynchrotron radio emission from extensive air showers. The code uses thoroughly tested time-domain radio emission routines in conjunction with a realistic air shower model based on per-shower multi-dimensional CORSIKA-generated histograms. We assess in detail how the transition from simpler, parametrised, to realistic, CORSIKA-based particle distributions affects the predicted radio emission from a typical 10^17 eV air shower. The effects of eliminating a previously needed free parameter and adopting realistic electron to positron ratios are also discussed. Compared with earlier calculations based on parametrised showers, REAS2 simulations predict slightly weaker and in some cases narrower pulses. In addition, a pronounced east-west versus north-south asymmetry arises in the emission pattern, and the radio pulses become generally unipolar. Finally, we demonstrate how REAS2 can be used to study radio pulse shapes and ...

  13. Radio detection of cosmic ray air showers in the digital era

    Science.gov (United States)

    Huege, Tim

    2016-03-01

    In 1965 it was discovered that cosmic ray air showers emit impulsive radio signals at frequencies below 100 MHz. After a period of intense research in the 1960s and 1970s, however, interest in the detection technique faded almost completely. With the availability of powerful digital signal processing techniques, new attempts at measuring cosmic ray air showers via their radio emission were started at the beginning of the new millennium. Starting with modest, small-scale digital prototype setups, the field has evolved, matured and grown very significantly in the past decade. Today's second-generation digital radio detection experiments consist of up to hundreds of radio antennas or cover areas of up to 17 km2. We understand the physics of the radio emission in extensive air showers in detail and have developed analysis strategies to accurately derive from radio signals parameters which are related to the astrophysics of the primary cosmic ray particles, in particular their energy, arrival direction and estimators for their mass. In parallel to these successes, limitations inherent in the physics of the radio signals have also become increasingly clear. In this article, we review the progress of the past decade and the current state of the field, discuss the current paradigm of the radio emission physics and present the experimental evidence supporting it. Finally, we discuss the potential for future applications of the radio detection technique to advance the field of cosmic ray physics.

  14. Measurement of cosmic-ray air showers with the Tunka Radio Extension (Tunka-Rex)

    CERN Document Server

    Bezyazeekov, P A; Gress, O A; Haungs, A; Hiller, R; Huege, T; Kazarina, Y; Kleifges, M; Konstantinov, E N; Korosteleva, E E; Kostunin, D; Krömer, O; Kuzmichev, L A; Levinson, E; Lubsandorzhiev, N; Mirgazov, R R; Monkhoev, R; Pakhorukov, A; Pankov, L; Prosin, V V; Rubtsov, G I; Rühle, C; Schröder, F G; Wischnewski, R; Zagorodnikov, A

    2015-01-01

    Tunka-Rex is a radio detector for cosmic-ray air showers in Siberia, triggered by Tunka-133, a co-located air-Cherenkov detector. The main goal of Tunka-Rex is the cross-calibration of the two detectors by measuring the air-Cherenkov light and the radio signal emitted by the same air showers. This way we can explore the precision of the radio-detection technique, especially for the reconstruction of the primary energy and the depth of the shower maximum. The latter is sensitive to the mass of the primary cosmic-ray particles. In this paper we describe the detector setup and explain how electronics and antennas have been calibrated. The analysis of data of the first season proves the detection of cosmic-ray air showers and therefore, the functionality of the detector. We confirm the expected dependence of the detection threshold on the geomagnetic angle and the correlation between the energy of the primary cosmic-ray particle and the radio amplitude. Furthermore, we compare reconstructed amplitudes of radio pu...

  15. Air fluorescence detection of large air showers below the horizon

    Science.gov (United States)

    Halverson, P.; Bowen, T.

    1985-01-01

    In the interest of exploring the cosmic ray spectrum at energies greater than 10 to the 18th power eV, where flux rates at the Earth's surface drop below 100 yr(-1) km(-2) sr(-1), cosmic ray physicists have been forced to construct ever larger detectors in order to collect useful amounts of data in reasonable lengths of time. At present, the ultimate example of this trend is the Fly's Eye system in Utah, which uses the atmosphere around an array of skyward-looking photomultiplier tubes. The air acts as a scintillator to give detecting areas as large as 5000 square kilometers sr (for highest energy events). This experiment has revealed structure (and a possible cutoff) in the ultra-high energy region above 10 o the 19th power eV. The success of the Fly's Eye experiment provides impetus for continuing the development of larger detectors to make accessible even higher energies. However, due to the rapidly falling flux, a tenfold increase in observable energy would call for a hundredfold increase in the detecting area. But, the cost of expanding the Fly's Eye detecting area will approximately scale linearly with area. It is for these reasons that the authors have proposed a new approach to using the atmosphere as a scintillator; one which will require fewer photomultipliers, less hardware (thus being less extensive), yet will provide position and shower size information.

  16. Radio detection of high-energy cosmic rays with the Auger Engineering Radio Array

    Science.gov (United States)

    Schröder, Frank G.

    2016-07-01

    The Auger Engineering Radio Array (AERA) is an enhancement of the Pierre Auger Observatory in Argentina. Covering about 17km2, AERA is the world-largest antenna array for cosmic-ray observation. It consists of more than 150 antenna stations detecting the radio signal emitted by air showers, i.e., cascades of secondary particles caused by primary cosmic rays hitting the atmosphere. At the beginning, technical goals had been in focus: first of all, the successful demonstration that a large-scale antenna array consisting of autonomous stations is feasible. Moreover, techniques for calibration of the antennas and time calibration of the array have been developed, as well as special software for the data analysis. Meanwhile physics goals come into focus. At the Pierre Auger Observatory air showers are simultaneously detected by several detector systems, in particular water-Cherenkov detectors at the surface, underground muon detectors, and fluorescence telescopes, which enables cross-calibration of different detection techniques. For the direction and energy of air showers, the precision achieved by AERA is already competitive; for the type of primary particle, several methods are tested and optimized. By combining AERA with the particle detectors we aim for a better understanding of cosmic rays in the energy range from approximately 0.3 to 10 EeV, i.e., significantly higher energies than preceding radio arrays.

  17. Radio measurements of the energy and the depth of the shower maximum of cosmic-ray air showers by Tunka-Rex

    Science.gov (United States)

    Bezyazeekov, P. A.; Budnev, N. M.; Gress, O. A.; Haungs, A.; Hiller, R.; Huege, T.; Kazarina, Y.; Kleifges, M.; Konstantinov, E. N.; Korosteleva, E. E.; Kostunin, D.; Krömer, O.; Kuzmichev, L. A.; Lubsandorzhiev, N.; Mirgazov, R. R.; Monkhoev, R.; Pakhorukov, A.; Pankov, L.; Prosin, V. V.; Rubtsov, G. I.; Schröder, F. G.; Wischnewski, R.; Zagorodnikov, A.

    2016-01-01

    We reconstructed the energy and the position of the shower maximum of air showers with energies E gtrsim 100 PeV applying a method using radio measurements performed with Tunka-Rex. An event-to-event comparison to air-Cherenkov measurements of the same air showers with the Tunka-133 photomultiplier array confirms that the radio reconstruction works reliably. The Tunka-Rex reconstruction methods and absolute scales have been tuned on CoREAS simulations and yield energy and Xmax values consistent with the Tunka-133 measurements. The results of two independent measurement seasons agree within statistical uncertainties, which gives additional confidence in the radio reconstruction. The energy precision of Tunka-Rex is comparable to the Tunka-133 precision of 15%, and exhibits a 20% uncertainty on the absolute scale dominated by the amplitude calibration of the antennas. For Xmax, this is the first direct experimental correlation of radio measurements with a different, established method. At the moment, the Xmax resolution of Tunka-Rex is approximately 40 g/cm2. This resolution can probably be improved by deploying additional antennas and by further development of the reconstruction methods, since the present analysis does not yet reveal any principle limitations.

  18. Characteristics of air showers produced by extremely high energy gamma-rays

    International Nuclear Information System (INIS)

    The technique of adjoint cascade equations has been applied to calculate the properties of air showers produced by extremely high energy (EHE) γ-rays in the energy range 1018-1022 eV. The high intrinsic accuracy, combined with very modest (compared with the traditional Monte Carlo codes) computational time requirements, make this method as an effective tool for the detailed study of development of EHE showers in the Earth's atmosphere. In this paper a wide range of parameters of γ-ray-induced showers are analysed taking into account two independent effects which become crucial for the cascade development in the EHE regime - the Landau-Pomeranchuk-Migdal (LPM) effect and the interaction of primary γ-rays with the geomagnetic field (GMF). Although the LPM effect leads to dramatic modifications of shower characteristics, especially at primary energies exceeding 1019 eV, the GMF effect, which starts to 'work' at approximately the same energies, prevents, to a large extent, the LPM effect by converting the primary γ-ray into a bunch of synchrotron γ-ray photons with energies effectively below the threshold of the LPM effect. This bunch of secondary photons hits the atmosphere and creates a large number of simultaneous showers. The superposition of these independent showers mimics a single shower with energy E=ΣEi≅E0, but without the signatures of the LPM effect. This makes the longitudinal profile of such a composite electromagnetic shower quite similar to the longitudinal profile of hadronic showers. At the same time, the number of muons as well as their lateral distribution differ significantly from the corresponding parameters of proton-induced showers. In the 'gamma-ray bunch' regime, the total number of muons is less, by a factor of 5-10, than the number of muons in hadronic showers. Also, compared with the hadronic showers, the electromagnetic showers are characterized by a significantly narrower lateral distribution of muons. Even so, for inclined EHE

  19. Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

    CERN Document Server

    Apel, W D; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Chiavassa, A; Daumiller, K; de Souza, V; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Fuchs, B; Fuhrmann, D; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmidt, A; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Zabierowski, J; Zensus, J A

    2013-01-01

    Cosmic ray air showers emit radio pulses at MHz frequencies, which can be measured with radio antenna arrays - like LOPES at the Karlsruhe Institute of Technology in Germany. To improve the understanding of the radio emission, we test theoretical descriptions with measured data. The observables used for these tests are the absolute amplitude of the radio signal, and the shape of the radio lateral distribution. We compare lateral distributions of more than 500 LOPES events with two recent and public Monte Carlo simulation codes, REAS 3.11 and CoREAS (v 1.0). The absolute radio amplitudes predicted by REAS 3.11 are in good agreement with the LOPES measurements. The amplitudes predicted by CoREAS are lower by a factor of two, and marginally compatible with the LOPES measurements within the systematic scale uncertainties. In contrast to any previous versions of REAS, REAS 3.11 and CoREAS now reproduce the shape of the measured lateral distributions correctly. This reflects a remarkable progress compared to the si...

  20. Afterpulses and decay times of fast scintillation counters for extensive air shower experiments

    International Nuclear Information System (INIS)

    A fast scintillation counter system to observe the arrival time distribution of relativistic particles in extensive air showers has been developed. The generation rate of afterpulses observed by a ternary plastic scintillation counter of a fast-time-response photomultiplier were studied in detail. It was found that the effect of afterpulses generated in the photomultiplier and scintillation process was negligibly small compared with that of afterpulses produced by delayed particles in the shower. It was also found that long decay components in the scintillator output can be explained as being due to afterpulses. (orig.)

  1. Ultrahigh energy cosmic ray composition from surface air shower and underground muon measurements at Soudan 2

    International Nuclear Information System (INIS)

    The Soudan 2 experiment has performed time-coincident cosmic ray air shower and underground muon measurements. Comparisons to Monte Carlo predictions show that such measurements can make statistically significant tests of the primary composition in the knee region of the cosmic ray spectrum. The results do not support any significant increase in the average primary mass with energy in the range of ∼104 TeV per nucleus. Some systematic uncertainties remain, however, particularly in the Monte Carlo modeling of the cosmic ray shower

  2. Measuring the muon content of air showers with IceTop

    Directory of Open Access Journals (Sweden)

    Gonzalez Javier G.

    2015-01-01

    Full Text Available IceTop, the surface component of the IceCube detector, has been used to measure the energy spectrum of cosmic ray primaries in the range between 1.58 PeV and 1.26 EeV. It can also be used to study the low energy muons in air showers by looking at large distances (> 300 m from the shower axis. We will show the muon lateral distribution function at large lateral distances as measured with IceTop and discuss the implications of this measurement. We will also discuss the prospects for low energy muon studies with IceTop.

  3. Atmospheric effects and sidereal-diurnal variations in extended air showers

    Science.gov (United States)

    Efimov, N. N.; Krasilnikov, D. D.; Nikolskiy, S. N.; Shamsutdinova, F. K.

    1975-01-01

    Observations are presented on the variations of extended air shower intensity with an average power of 1.4 x 10,000 and 1.4 x 100,000 particles at sea level. The effect of disintegrating particles and the essential role of cascades formed above the lower third of the atmosphere are examined. However, the authors failed to discover anisotropy of initial particles with an energy of 10 to the 14th power to 10 to the 15th power eV with an accuracy of up to 0.1%.

  4. The cosmic-ray air-shower signal in Askaryan radio detectors

    Science.gov (United States)

    de Vries, Krijn D.; Buitink, Stijn; van Eijndhoven, Nick; Meures, Thomas; Ó Murchadha, Aongus; Scholten, Olaf

    2016-02-01

    We discuss the radio emission from high-energy cosmic-ray induced air showers hitting Earth's surface before the cascade has died out in the atmosphere. The induced emission gives rise to a radio signal which should be detectable in the currently operating Askaryan radio detectors built to search for the GZK neutrino flux in ice. The in-air emission, the in-ice emission, as well as a new component, the coherent transition radiation when the particle bunch crosses the air-ice boundary, are included in the calculations.

  5. Study of extensive air showers with the EAS-BARS pilot setup

    International Nuclear Information System (INIS)

    To investigate into spectrum of the extensive air showers (EAS) within its breakdown region one designed and constructed BARS-EAS pilot setup. It consists of eight scintillation counters. Two central counters are placed on the case of a liquid-argon spectrometer. Total recording area of the BARS-EAS setup is equal to 104 m2. Conditions to select events are as follows: 6-fold coincidences, excess of the total energy release in 50 GeV value spectrometer. Besides, distance from shower axis up to spectrometer centre should be maximum 10 m. One estimated accuracy of restoration of EAS parameters

  6. The Air Microwave Yield (AMY experiment to measure the GHz emission from air shower plasmas

    Directory of Open Access Journals (Sweden)

    Smida R.

    2013-06-01

    Full Text Available The AMY experiment aims to measure the Microwave Bremsstrahlung Radiation (MBR emitted by air-showers secondary electrons accelerating in collisions with neutral molecules of the atmosphere. The measurements are performed at the Beam Test Facility (BTF of Frascati INFN National Laboratories and the final purpose is to characterize the process to be used in a next generation detectors of ultra-high energy cosmic rays (up to 1020eV. We describe the experimental set-up and the first test measurement performed in November 2011.

  7. Electron lateral distribution in air showers: scaling formalism and its implications

    International Nuclear Information System (INIS)

    Theoretical results representing further development of scaling formalism for the lateral distribution of electrons in atmospheric cascade showers are reported in this paper. A detailed study of the root mean square radius of extensive air shower electrons - the basic parameter of the lateral distribution function (LDF) - has been carried out. Comparisons of our predictions with CORSIKA simulation results and also KASCADE and AGASA experimental data are presented. A new method for cosmic ray primary composition deduction from the shape of electron LDF, applicable in wide primary energy range with weak sensitivity to hadronic interaction model, is introduced. (author)

  8. Photoelectron multipliers in photodetector of orbital fluorescence detector of extensive air showers

    International Nuclear Information System (INIS)

    The choice of a photoelectron multiplier (FEM) for photoreceiver of the fluorescent detector used for observation of extensive air showers from near-Earth orbit under varying conditions of the night sky is discussed. Special attention is paid to the problem of the FEM amplification factor control. The characteristics of two photomultipliers with uviol input glass and multialkaline cathode, i.e. FEU-184UM and R1463U, are compared. It is suggested that the FEM are grouped in cluster with a common power supply and information recording system to solve the problem of power supply and FEM amplification factor control

  9. QGSJET-II: physics, recent improvements, and results for air showers

    Directory of Open Access Journals (Sweden)

    Ostapchenko S.

    2013-06-01

    Full Text Available Modeling of high energy hadronic and nuclear interactions by the QGSJET-II generator is discussed. Recent updates related to the treatment of nonlinear effects inthe interaction dynamics and to the model calibration with new LHC data are described. A special attention is devoted to the predictions of the new model version forcharacteristics of extensive air showers initiated by high energy cosmic rays. In particular, an improved description of charge exchange processes in pion collisionsis discussed and the respective enhancement of the shower muon content is analyzed.

  10. Investigation of extensive air shower muon and electron components on a MGU device

    Energy Technology Data Exchange (ETDEWEB)

    Grishina, N.V.; Kalmykov, N.N.; Kulikov, G.V.; Rozhdestvenskii, S.M.; Solov' eva, V.I.; Fomin, Yu.A.; Khrenov, B.A.; Khristiansen, G.B. (Moskovskij Gosudarstvennyj Univ. (USSR). Nauchno-Issledovatel' skij Inst. Yadernoj Fiziki)

    1981-07-01

    The muon and electron component of extensive air showers (EAS) with the number of particles of 10/sup 5/-10/sup 6/ is investigated. The functions of electron and muon spatial distribution and muon energetic spectra on different distances from the EAS axis are presented. It is shown that muon component characteristics (muon current and the energetic composition) in the distance range of r<8 m depends slightly on EAS age. Widths of spatial muon distribution change noticeably with age. Calculations of EAS development according to the scaling model do not agree with the data of the experiment.

  11. Measurements of the muon component of extensive air showers at 320 m.w.e. underground

    Energy Technology Data Exchange (ETDEWEB)

    Grupen, C.; Kurt, M.T.; Mailov, A. E-mail: mailov@aleph.physik.uni-siegen.de; Mueller, A.S.; Putzer, A.; Rensch, B.; Sander, H.G.; Schmeling, S.; Schmelling, M.; Wachsmuth, H.; Ziegler, T.; Zuber, K

    2003-09-01

    The ALEPH detector at LEP has been supplemented with five scintillator telescopes to measure the muon component of cosmic ray air showers underground. The emphasis of the present analysis of a new data set is to measure coincidences over distances up to about 1 km which are sensitive to the forward production of hadronic interactions and the chemical composition of primary cosmic rays in the energy range around 10{sup 15} eV. First results indicate that the observed decoherence curve of muons is compatible with a light primary composition and the arrival directions of muons show no obvious clustering in galactic coordinates.

  12. Measurements of the muon component of extensive air showers at 320 mwe underground

    CERN Document Server

    Grupen, C; Mailov, A; Müller, A S; Putzer, A; Rensch, B; Sander, H G; Schmeling, S; Schmelling, M; Wachsmuth, H W; Ziegler, T; Zuber, K

    2003-01-01

    The ALEPH detector at LEP has been supplemented with five scintillator telescopes to measure the muon component of cosmic ray air showers underground. The emphasis of the present analysis of a new data set is to measure coincidences over distances up to about 1km which are sensitive to the forward production of hadronic interactions and the chemical composition of primary cosmic rays in the energy range around 10**1**5eV. First results indicate that the observed decoherence curve of muons is compatible with a light primary composition and the arrival directions of muons show no obvious clustering in galactic coordinates.

  13. Cloud-chamber search for multiple-cores and high transverse-momenta in cosmic ray air showers

    International Nuclear Information System (INIS)

    In this experiment, the Leeds 2.87 m2 cloud-chamber is located at the center of a 7.2 m x 7.2 m array of ten scintillators that trigger the chamber on showers of approximately equal to 105 particles whose cores fall within approximately equal to 5 m of the center of the array. Model calculations indicate that even if every nuclearactive collision in an air shower creates a product hadron with high transverse momentum - and thus a sub-core, only one such sub-core would be detected per month by the Leeds apparatus. Visual examination of the cloud-chamber photographs of the 3285 events recorded during six months' operation reveals 89 shower-core candidates. For most of these candidates, the separation between the shower-axis located by the scintillator data and the axis seen in the cloud-chamber obeys a two-dimensional Gaussian distribution. For 7 events, however, the separation is greater than or equal to 4 sigma, and these candidates are either sub-cores or products of local interactions. One of these 7 contains almost 90 charged particles within a radius of 0.2 m and may be a genuine sub-core indicating a transverse momentum of 15 GeV/c. Observing a single sub-core in the cloud-chamber implies that about 1/3 of the 105-particle showers that trigger the chamber have sub-cores. Model calculations show that interactions of shower hadrons in the roof should cause about 0.2 dense regions of the size observed in the cloud-chamber. Model calculations show that the roofing above the Kiel detectors is probably not sufficient to develop all of the dense regions that they observe

  14. The MIDAS Experiment: A New Technique for the Detection of Extensive Air Showers

    CERN Document Server

    Williams, C; Berlin, A; Bohacova, M; Facal, P; Genat, J F; Mills, E; Monasor, M; Privitera, P; Reyes, L C; d'Orfeuil, B Rouille; Wayne, S; Alekotte, I; Bertou, X; Bonifazi, C; Neto, J R T de Mello; Santos, E M; Alvarez-Muñiz, J; Carvalho, W; Zas, E

    2010-01-01

    Recent measurements suggest free electrons created in ultra-high energy cosmic ray extensive air showers (EAS) can interact with neutral air molecules producing Bremsstrahlung radiation in the microwave regime. The microwave radiation produced is expected to scale with the number of free electrons in the shower, which itself is a function of the energy of the primary particle and atmospheric depth. Using these properties a calorimetric measurement of the EAS is possible. This technique is analogous to fluorescence detection with the added benefit of a nearly 100% duty cycle and practically no atmospheric attenuation. The Microwave Detection of Air Showers (MIDAS) prototype is currently being developed at the University of Chicago. MIDAS consists of a 53 feed receiver operating in the 3.4 to 4.2 GHz band. The camera is deployed on a 4.5 meter parabolic reflector and is instrumented with high speed power detectors and autonomous FPGA trigger electronics. We present the current status of the MIDAS instrument and...

  15. Reconstruction of extensive air showers using the MIDAS molecular Bremsstrahlung detector

    Energy Technology Data Exchange (ETDEWEB)

    Castro, Andre Ramos de [Universidade Federal do Rio de Janeiro (UFRJ), RJ (Brazil). Escola Politecnica; Bonifazi, Carla; Santos, Edivaldo Moura; Soares, Elvis do Amaral; Mello Neto, Joao Ramos Torres de [Universidade Federal do Rio de Janeiro (UFRJ), RJ (Brazil). Inst. de Fisica; Almeida, Rogerio Menezes de [Universidade Federal Fluminense (EEIMVR/UFF), Volta Redonda, RJ (Brazil). Escola de Engenharia Industrial Metalurgica de Volta Redonda

    2011-07-01

    Full text: The weakly ionized plasma created in the atmosphere after the passage of an Extensive Air Shower (EAS) gives rise to the emission of continuous radiation known as Molecular Bremsstrahlung Radiation (MBR) as free electrons scatter off neutral nitrogen (and less frequently oxygen) molecules. The isotropic and unpolarized nature of MBR rises the possibility of an EAS detection similar to that using fluorescence telescopes to capture the ultraviolet light emitted by the ionized nitrogen molecules. The MBR emission, however, falls into the centimeter wavelength range, requiring the use of radio/microwave antennas instead of optical telescopes. In order to test the feasibility of the technique, the MIDAS (Microwave Detection of Air Showers) Collaboration has built a prototype detector where a parabolical reflector illuminates a multi-pixel camera of commercial TV satellite C-band (3.4-4.2 GHz) feeds. This work addresses the geometrical reconstruction of EAS induced by Ultra High Energy Cosmic Rays (UHECR) using the MIDAS detector. The reconstruction chain is similar to that currently applied to the Auger Fluorescence detector events. We have simulated the shower MBR emission assuming two different scenarios: coherent and incoherent emission, i.e., radiation intensity scaling quadratically and linearly with the energy of the primary particle. The MIDAS prototype detector's response is then simulated. Finally, given the simulated events in real data format, we reconstruct the shower's arrival direction, including direction uncertainties and estimate the expected rate of observed events. (author)

  16. Study of muon bundles from extensive air showers with the ALICE detector at CERN LHC

    Science.gov (United States)

    Shtejer, K.

    2016-05-01

    ALICE is one of four large experiments at the CERN Large Hadron Collider, specially designed to study particle production in ultra-relativistic heavy-ion collisions. Located 52 meters underground with 28 meters of overburden rock, it has also been used to detect muons produced by cosmic-ray interactions in the upper atmosphere. The large size and excellent tracking capability of the ALICE Time Projection Chamber are exploited to study the muonic component of extensive air showers. We present the multiplicity distribution of these atmospheric muons and its comparison with Monte Carlo simulations. The latest version of the QGSJET hadronic interaction model was used to simulate the development of the resulting air showers. High multiplicity events containing more than 100 reconstructed muons were also studied. Similar events have been studied in previous underground experiments such as ALEPH and DELPHI at LEP without satisfactory explanations for the frequency of the highest multiplicity events. We demonstrate that the high muon-multiplicity events observed in ALICE stem from primary cosmic rays with energies above 1016 eV and that the frequency of these events can be successfully described by assuming a heavy mass composition of primary cosmic rays in this energy range.

  17. Interpretation of measurements of the number of muons in extensive air shower experiments

    CERN Document Server

    Prado, Raul Ribeiro; Pimenta, Mário; de Souza, Vitor

    2016-01-01

    In this paper we analyze the energy evolution of the muon content of air showers between $10^{18.4}$ and $10^{19.6}$ eV to be able to determine the most likely mass composition scenario from future number of muons measurements. The energy and primary mass evolution of the number of muons is studied based on the Heitler-Matthews model and Monte Carlo simulation of the air shower. A simple model to describe the evolution of the first and second moments of number of muons distributions is proposed and validated. An analysis approach based on the comparison between this model's predictions and data to discriminate among a set of composition scenarios is presented and tested with simulations. It is shown that the composition scenarios can be potentially discriminated under the conditions imposed by the method. The discrimination power of the proposed analysis is stable under systematic changes of the absolute number of muons from model predictions and on the scale of the reconstructed energy.

  18. Discriminating between electron and gamma air showers using direct Cherenkov light

    International Nuclear Information System (INIS)

    Imaging Atmospheric Cherenkov Telescopes (IACTs) detect VHE gamma rays from galactic and extragalactic sources in order to probe the acceleration mechanisms involved in the most energetic and exotic sources. The reconstruction techniques currently used can distinguish most of the background of hadrons entering the atmosphere as they produce very different air showers. Showers initiated by electrons on the other hand are much harder to separate, as they also produce electromagnetic cascades. A new technique making use of direct Cherenkov (DC) light could provide a way to finally distinguish between the two. Cherenkov light emitted directly from the primary particle before it interacts results in a signal at the start of the extensive air shower image in the IACT camera. Probing the characteristics of DC light could allow direct identification of electrons and other charged primaries. This would lead to the increased sensitivity of H.E.S.S. and CTA, confirmation of the electron background contamination level and could also provide a measurement of the diffuse extragalactic background light.

  19. Reconstruction of extensive air showers using the MIDAS molecular Bremsstrahlung detector

    International Nuclear Information System (INIS)

    Full text: The weakly ionized plasma created in the atmosphere after the passage of an Extensive Air Shower (EAS) gives rise to the emission of continuous radiation known as Molecular Bremsstrahlung Radiation (MBR) as free electrons scatter off neutral nitrogen (and less frequently oxygen) molecules. The isotropic and unpolarized nature of MBR rises the possibility of an EAS detection similar to that using fluorescence telescopes to capture the ultraviolet light emitted by the ionized nitrogen molecules. The MBR emission, however, falls into the centimeter wavelength range, requiring the use of radio/microwave antennas instead of optical telescopes. In order to test the feasibility of the technique, the MIDAS (Microwave Detection of Air Showers) Collaboration has built a prototype detector where a parabolical reflector illuminates a multi-pixel camera of commercial TV satellite C-band (3.4-4.2 GHz) feeds. This work addresses the geometrical reconstruction of EAS induced by Ultra High Energy Cosmic Rays (UHECR) using the MIDAS detector. The reconstruction chain is similar to that currently applied to the Auger Fluorescence detector events. We have simulated the shower MBR emission assuming two different scenarios: coherent and incoherent emission, i.e., radiation intensity scaling quadratically and linearly with the energy of the primary particle. The MIDAS prototype detector's response is then simulated. Finally, given the simulated events in real data format, we reconstruct the shower's arrival direction, including direction uncertainties and estimate the expected rate of observed events. (author)

  20. Simulation of radio emission from air showers in atmospheric electric fields

    CERN Document Server

    Buitink, S; Falcke, H; Kuijpers, J

    2010-01-01

    We study the effect of atmospheric electric fields on the radio pulse emitted by cosmic ray air showers. Under fair weather conditions the dominant part of the radio emission is driven by the geomagnetic field. When the shower charges are accelerated and deflected in an electric field additional radiation is emitted. We simulate this effect with the Monte Carlo code REAS2, using CORSIKA-simulated showers as input. In both codes a routine has been implemented that treats the effect of the electric field on the shower particles. We find that the radio pulse is significantly altered in background fields of the order of ~100 V/cm and higher. Practically, this means that air showers passing through thunderstorms emit radio pulses that are not a reliable measure for the shower energy. Under other weather circumstances significant electric field effects are expected to occur rarely, but nimbostratus clouds can harbor fields that are large enough. In general, the contribution of the electric field to the radio pulse ...

  1. A new way of air shower detection: measuring the properties of cosmic rays with LOFAR

    Science.gov (United States)

    Nelles, A.; Buitink, S.; Corstanje, A.; Enriquez, J. E.; Falcke, H.; Hörandel, J. R.; Rachen, J. P.; Schellart, P.; Scholten, O.; ter Veen, S.; Thoudam, S.; Trinh, T. N. G.

    2015-08-01

    High-energy cosmic rays impinging onto the atmosphere of the Earth initiate cascades of secondary particles: extensive air showers. Many of the particles in a shower are electrons and positrons. During the development of the air shower and by interacting with the geomagnetic field, the electromagnetic cascade creates radiation, which we detect at frequencies of tens of MHz with the LOFAR radio telescope in the Netherlands. After many years of struggling to understand the emission mechanisms, the radio community has achieved the breakthrough. We are now able to determine direction, energy, and type of the shower- inducing primary particle from the radio measurements. The large number of antennas at LOFAR allows us to have a high precision and very detailed measurements. We will elaborate on the shower reconstruction, a precise description of the intensity of the radio signal at ground level (at frequencies from 10 to 240 MHz), a precise measurement of the shape of the radio wavefront, and on the reconstruction of the shower energy.

  2. Full Monte Carlo simulations of radio emission from extensive air showers with CoREAS

    CERN Document Server

    Huege, Tim

    2013-01-01

    CoREAS is a Monte Carlo simulation code for the calculation of radio emission from extensive air showers. It is based on the "endpoint formalism" for radiation from moving charges implemented directly in CORSIKA. Consequently, the full complexity of the air-shower physics is taken into account without the need for approximations or assumptions on the emission mechanism. We present results of simulations for an unthinned shower performed with CoREAS for both MHz and GHz frequencies. At MHz frequencies, the simulations predict the well-known mixture of geomagnetic and charge excess radiation. At GHz frequencies, the emission is strongly influenced by Cherenkov effects arising from the varying refractive index in the atmosphere. In addition, a qualitative difference in the symmetry of the GHz radiation pattern is observed when compared to the ones at lower frequencies. We also discuss the strong increase in the ground area subtended by the radio emission when going from near-vertical to very inclined geometries,...

  3. Cosmic ray energy reconstruction from the S(500) observable recorded in the KASCADE-Grande air shower experiment

    Science.gov (United States)

    Apel, W. D.; Arteaga-Velázquez, J. C.; Bekk, K.; Bertaina, M.; Blümer, J.; Bozdog, H.; Brancus, I. M.; Cantoni, E.; Chiavassa, A.; Cossavella, F.; Daumiller, K.; de Souza, V.; Di Pierro, F.; Doll, P.; Engel, R.; Fuhrmann, D.; Gherghel-Lascu, A.; Gils, H. J.; Glasstetter, R.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J. R.; Huber, D.; Huege, T.; Kampert, K.-H.; Kang, D.; Klages, H. O.; Link, K.; Łuczak, P.; Mathes, H. J.; Mayer, H. J.; Milke, J.; Mitrica, B.; Morello, C.; Oehlschläger, J.; Ostapchenko, S.; Palmieri, N.; Petcu, M.; Pierog, T.; Rebel, H.; Roth, M.; Schieler, H.; Schoo, S.; Schröder, F. G.; Sima, O.; Toma, G.; Trinchero, G. C.; Ulrich, H.; Weindl, A.; Wochele, J.; Zabierowski, J.

    2016-04-01

    The energy reconstruction at KASCADE-Grande is based on a combination of the shower size and the total muon number, which are both estimated for each individual air shower event. We present investigations where we employed a second method to reconstruct the primary energy using S(500), which are the charged particle densities inferred with the KASCADE-Grande detector at a distance of 500 m from the shower axis. We considered the attenuation of inclined showers by applying the "Constant Intensity Cut" method and we employed a simulation-derived calibration to convert the recorded S(500) into primary energy. We observed a systematic shift in the S(500)-derived energy compared with previously reported results obtained using the standard reconstruction technique. However, a comparison of the two methods based on simulated and measured data showed that this shift only appeared in the measured data. Our investigations showed that this shift was caused mainly by the inadequate description of the shape of the lateral density distribution in the simulations.

  4. An investigation of mass composition of ultra-high energy cosmic rays with energies above 1019 eV via the study of extensive air showers

    Directory of Open Access Journals (Sweden)

    Doostmohammadi S.

    2012-01-01

    Full Text Available The electron and muon components of extensive air shower (EAS with energies above 1019 eV are analyzed via various giant EAS arrays. A varying property of showers is observed for two energy ranges; higher and lower than (3 − 4 x 1019 eV. The age parameter, zenith angle, shower size dependence on muon size and shower size dependence on primary energy show an increment of mass composition (MC above (3−4x 1019eV. Comparison of the observed EAS results with the simulations of Capdevielle et al. (2000 and Shinozaki et al. (2005 gives at most 20% photon fraction for primary energies above 1019 eV. The arrival directions of showers above 4x1019 eV indicate an increasing concentration towards the super galactic plane.

  5. Ultra-high energy cosmic rays: analysis of extensive air showers and their associated electromagnetic signal in the MHz domain

    International Nuclear Information System (INIS)

    In this HDR (accreditation to supervise research) report, the author proposes a review of the present results in the field of ultra-high energy cosmic rays. After a presentation of some results about the Fermi mechanism to accelerate cosmic rays, the author more particularly addresses the reconstruction of air showers, and the search for sources. He also addresses the radio signal emitted by air shower secondary positrons and electrons. He proposes an overview of the present knowledge on the basis of present experiments. Data show that the electric field is mainly due to the influence of the Earth magnetic field which acts on electrons and positrons, but more recently, the contribution due to electrons in excess seems to appear in data. The author reports the last advances in the field of simulation of the electric field, with notably the prediction of new signal produced by the disappearance of the air shower during its absorption by the soil

  6. Lateral distribution of high energy hadrons and gamma ray in air shower cores observed with emulsion chambers

    Science.gov (United States)

    Matano, T.; Machida, M.; Kawasumi, N.; Tsushima, I.; Honda, K.; Hashimoto, K.; Navia, C. E.; Matinic, N.; Aquirre, C.

    1985-01-01

    A high energy event of a bundle of electrons, gamma rays and hadronic gamma rays in an air shower core were observed. The bundles were detected with an emulsion chamber with thickness of 15 cm lead. This air shower is estimated to be initiated with a proton with energy around 10 to the 17th power to 10 to the 18th power eV at an altitude of around 100 gmc/2. Lateral distributions of the electromagnetic component with energy above 2 TeV and also the hadronic component of energy above 6 TeV of this air shower core were determined. Particles in the bundle are produced with process of the development of the nuclear cascade, the primary energy of each interaction in the cascade which produces these particles is unknown. To know the primary energy dependence of transverse momentum, the average products of energy and distance for various average energies of secondary particles are studied.

  7. A Measurement of Time-Averaged Aerosol Optical Depth using Air-Showers Observed in Stereo by HiRes

    CERN Document Server

    Abbasi, R U; Amann, J F; Archbold, G; Atkins, R; Belov, K; Belz, J W; Ben Zvi, S; Bergman, D R; Boyer, J H; Cannon, C T; Cao, Z; Connolly, B M; Fedorova, Y; Finley, C B; Hanlon, W F; Hoffman, C M; Holzscheiter, M H; Hughes, G A; Hüntemeyer, P; Jui, C C H; Kirn, M A; Knapp, B C; Loh, E C; Manago, N; Mannel, E J; Martens, K; Matthews, J A J; Matthews, J N; O'Neill, A; Reil, K; Roberts, M D; Schnetzer, S R; Seman, M; Sinnis, G; Smith, J D; Sokolsky, P; Song, C; Springer, R W; Stokes, B T; Thomas, S B; Thomson, G B; Tupa, D; Westerhoff, S; Wiencke, L R

    2006-01-01

    Air fluorescence measurements of cosmic ray energy must be corrected for attenuation of the atmosphere. In this paper we show that the air-showers themselves can yield a measurement of the aerosol attenuation in terms of optical depth, time-averaged over extended periods. Although the technique lacks statistical power to make the critical hourly measurements that only specialized active instruments can achieve, we note the technique does not depend on absolute calibration of the detector hardware, and requires no additional equipment beyond the fluorescence detectors that observe the air showers. This paper describes the technique, and presents results based on analysis of 1258 air-showers observed in stereo by the High Resolution Fly's Eye over a four year span.

  8. Construction of a Medium-Sized Schwarzschild-Couder Telescope for the Cherenkov Telescope Array: Implementation of the Cherenkov-Camera Data Acquisition System

    OpenAIRE

    Santander, M.; Buckley, J.; Humensky, B.; Mukherjee, R.; Consortium, for the CTA

    2015-01-01

    A medium-sized Schwarzchild-Couder Telescope (SCT) is being developed as a possible extension for the Cherenkov Telescope Array (CTA). The Cherenkov camera of the telescope is designed to have 11328 silicon photomultiplier pixels capable of capturing high-resolution images of air showers in the atmosphere. The combination of the large number of pixels and the high trigger rate (> 5 kHz) expected for this telescope results in a multi-Gbps data throughput. This sets challenging requirements on ...

  9. Failures in power-combining arrays

    OpenAIRE

    Rutledge, David B.; Cheng, Nai-Shuo; York, Robert A.; Weikle, Robert M., II; De Lisio, Michael P.

    1999-01-01

    We derive a simple formula for the change in output when a device fails in a power-combining structure with identical matched devices. The loss is written in terms of the scattering coefficient of the failed device and reflection coefficient of an input port in the combining network. We apply this formula to several power combiners, including arrays in free space and enclosed waveguide structures. Our simulations indicate the output power degrades gracefully as devices fail, which is in agree...

  10. Longitudinal EAS-Development Studies in the Air-Shower Experiment KASCADE-Grande

    CERN Document Server

    Doll, P; Arteaga-Velázquez, J C; Bekk, K; Bertaina, M; Blümer, J; Bozdog, H; Brancus, I M; Buchholz, P; Cantoni, E; Chiavassa, A; Cossavella, F; Daumiller, K; de Souza, V; di Pierro, F; Engel, R; Engler, J; Finger, M; Fuhrmann, D; Ghia, P L; Gils, H J; Glasstetter, R; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Kickelbick, D; Klages, H O; Link, K; Łuczak, P; Ludwig, M; Mathes, H J; Mayer, H J; Melissas, M; Milke, J; Mitrica, B; Morello, C; Navarra, G; Nehls, S; Oehlschläger, J; Ostapchenko, S; Over, S; Palmieria, N; Petcu, M; Pierog, T; Rebel, H; Roth, M; Schieler, H; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Ulrich, H; Weindl, A; Wochele, J; Wommer, M; Zabierowski, J

    2010-01-01

    A large area (128 m^2) Muon Tracking Detector (MTD), located within the KASCADE experiment, has been built with the aim to identify muons (E_mu > 0.8 GeV) and their directions in extensive air showers by track measurements under more than 18 r.l. shielding. The orientation of the muon track with respect to the shower axis is expressed in terms of the radial- and tangential angles. By means of triangulation the muon production height H_mu is determined. By means of H_mu, a transition from light to heavy cosmic ray primary particle with increasing shower energy Eo from 1-10 PeV is observed. Muon pseudorapidity distributions for the first interactions above 15 km are studied and compared to Monte Carlo simulations.

  11. Measurement of the Depth of Maximum of Extensive Air Showers above 1018 eV

    International Nuclear Information System (INIS)

    We describe the measurement of the depth of maximum, Xmax, of the longitudinal development of air showers induced by cosmic rays. Almost 4000 events above 1018 eV observed by the fluorescence detector of the Pierre Auger Observatory in coincidence with at least one surface detector station are selected for the analysis. The average shower maximum was found to evolve with energy at a rate of (106-21+35) g/cm2/decade below 1018.24±0.05 eV, and (24±3) g/cm2/decade above this energy. The measured shower-to-shower fluctuations decrease from about 55 to 26 g/cm2. The interpretation of these results in terms of the cosmic ray mass composition is briefly discussed.

  12. What tell us extensive air shower observations about hadronic interactions at ultrahigh energies?

    International Nuclear Information System (INIS)

    The interpretation of extensive air shower (EAS) observations needs a sufficiently accurate knowledge of the interactions driving the cascade development in the atmosphere. While the electromagnetic and weak interaction parts do not provide principal problems, the hadronic interaction is a subject of uncertainties and debates, especially in the ultrahigh energy region extending the energy limits of man made accelerators and experimental knowledge from collider experiments. Since the EAS development is dominantly governed by soft processes, which are presently not accessible to a perturbative QCD treatment, one has to rely on QCD inspired phenomenological interaction models, in particular on string-models based on the Gribow-Regge theory like QGSJET, VENUS and SYBILL. Recent results of the EAS experiments KASCADE are scrutinized in terms of such models used as generators in the Monte Carlo EAS simulation code CORSIKA. (orig.)

  13. Energy dependent fractal dimension in lateral electron distribution of extensive air showers

    Directory of Open Access Journals (Sweden)

    D. Purmohammad

    2008-12-01

    Full Text Available   Secondary electrons at ground level of simulated extensive air showers have been analyzed using a wavelet transform based technique, in order to investigate the variation of fractal dimensions of the lateral distribution of the electrons with shower energy and primary particle mass number. The fractal dimension is shown to increase with shower energy and seems to saturate to constant values near the core of the shower at higher energies. Using the fractal dimension properties at different core distances, a multi-parameter separation technique is then applied to the data. It has been shown that the technique has good accuracy at high energy, provided the energy of the shower is obtained independently.

  14. Cosmogenic neutrinos and signals of TeV gravity in air showers and neutrino telescopes.

    Science.gov (United States)

    Illana, J I; Masip, M; Meloni, D

    2004-10-01

    The existence of extra dimensions allows the possibility that the fundamental scale of gravity is at the TeV. If that is the case, gravity could dominate the interactions of ultrahigh energy cosmic rays. In particular, the production of microscopic black holes by cosmogenic neutrinos has been estimated in a number of papers. We consider here gravity-mediated interactions at larger distances, where they can be calculated in the eikonal approximation. We show that for the expected flux of cosmogenic neutrinos these elastic processes give a stronger signal than black hole production in neutrino telescopes. Taking the bounds on the higher-dimensional Planck mass M(D) (D=4 + n) from current air shower experiments, for n=2(6) elastic collisions could produce up to 118 (34) events per year at IceCube. On the other hand, the absence of any signal would imply a bound of M(D) > or approximately 5 TeV. PMID:15524863

  15. A study of depth of shower maximum of simulated air shower longitudinal profile using statistical methods

    International Nuclear Information System (INIS)

    The study of primary mass composition is important in revealing the vital information about the origin, acceleration and propagation mechanisms of high energy cosmic rays as it is difficult to analyse those properties directly. Several parameters may be considered for analysis of mass composition which carry information regarding the identity of the primary particle. The mass composition can be inferred from the study of depth of shower maximum (Xmax), shower maximum fluctuations (ΔXmax) and elongation rate (dXmax/dE). A new statistical analysis using higher moments of simulated air shower longitudinal profile using CORSIKA code within energy range 1015-1019eV for different primary induced shower is presented here.

  16. Testing of Large Diameter Fresnel Optics for Space Based Observations of Extensive Air Showers

    Science.gov (United States)

    Adams, James H.; Christl, Mark J.; Young, Roy M.

    2011-01-01

    The JEM-EUSO mission will detect extensive air showers produced by extreme energy cosmic rays. It operates from the ISS looking down on Earth's night time atmosphere to detect the nitrogen fluorescence and Cherenkov produce by the charged particles in the EAS. The JEM-EUSO science objectives require a large field of view, sensitivity to energies below 50 EeV, and must fit within available ISS resources. The JEM-EUSO optic module uses three large diameter, thin plastic lenses with Fresnel surfaces to meet the instrument requirements. A bread-board model of the optic has been manufactured and has undergone preliminary tests. We report the results of optical performance tests and evaluate the present capability to manufacture these optical elements.

  17. Proton-air and proton-proton cross sections from air shower data

    Science.gov (United States)

    Linsley, J.

    1985-01-01

    Data on the fluctuations in depth of maximum development of cosmic ray air showers, corrected for the effects of mixed primary composition and shower development fluctuations, yield values of the inelastic proton-air cross section for laboratory energies in the range 10 to the 8th power to 10 to the 10th power GeV. From these values of proton-air cross section, corresponding values of the proton-proton total cross section are derived by means of Glauber theory and geometrical scaling. The resulting values of proton-proton cross section are inconsistent with a well known 1n(2)s extrapolation of ISR data which is consistent with SPS data; they indicate a less rapid rate of increase in the interval 540 sq root of s 100000 GeV.

  18. Experimental study of the time structure of the muon component of Extensive Air Showers

    International Nuclear Information System (INIS)

    By using the Triggerlayer and the Multiwire Proportional Chambers of the Central Detector of the KASCADE experiment muons with an energy threshold of 2.4 GeV are measured in Extensive Air Showers. The arrival times of these muons measured with the Triggerlayer are examined whether they can give information about the shower development and the shower inducing primary. Detailed simulation studies are prepared, and special attention is put on the understanding of the detector response. By use of the arrival time of the first registered muon as a reference time, a strong dependency of the measured arrival times on the multiplicity of the muons is reviled. A procedure for the correction of this dependency is presented and checked for its usefulness. Altogether a very good agreement of the simulations with the measured data is observed. (orig.)

  19. Results of fractal analysis of the Kiel extensive air shower data

    International Nuclear Information System (INIS)

    For years there has been a problem in cosmic ray studies of how to distinguish individual extensive air showers (EAS) originating from primary protons, heavy nuclei or primary photons. In this paper results of experimental data obtained from the fractal analysis of particle density distributions in individual EAS detected in the range of shower sizes Ne between 1.4x105-5x106 by the old Kiel experiment are presented. The Lipschitz-Hoelder exponent distributions of EAS detected by the Kiel experiment are discussed. The examples of EAS most probably originating from primary protons, heavy nuclei and high-energy gamma-rays are presented. The lateral distributions of charged particle densities at small distances, angular and size spectra and the mass composition of primary cosmic ray particles around the 'knee' of the energy spectrum are discussed. The Monte Carlo simulation data illustrating the problem of interest are also shown. (author)

  20. The center of lateral iso-density contours for inclined cosmic air showers

    Science.gov (United States)

    Montanus, J. M. C.

    2016-02-01

    The horizontal lateral density of a cosmic air shower with a non-zero zenith angle is asymmetric. The asymmetry consist of a stretching of the iso-density contours to ellipses and to a shift of the center of the elliptic contours with respect to the core of the shower. The shift is caused by atmospheric attenuation. The modeling of the attenuation results in an equation for the shift as a function of zenith angle and the size of the iso-density contours. A more accurate equation is obtained by investigating the shift in lateral densities of simulated showers. It is shown how the shift can be incorporated in an elliptic lateral density function. A linear approximation for the shift allows for an analytical solution for the shifted elliptic density. Its predictions for the polar variations of the density are compared with data of simulated showers.

  1. Primary Particle Type of the Most Energetic Fly's Eye Air Shower

    CERN Document Server

    Risse, M; Gora, D; Pekala, J; Wilczynska, B; Wilczynski, H

    2004-01-01

    The longitudinal profile of the most energetic cosmic-ray air shower measured so far, the event recorded by the Fly's Eye detector with a reconstructed primary energy of about 320 EeV, is compared to simulated shower profiles. The calculations are performed with the CORSIKA code and include primary photons and different hadron primaries. For primary photons, preshower formation in the geomagnetic field is additionally treated in detail. For primary hadrons, the hadronic interaction models QGSJET01 and SIBYLL2.1 have been employed. The predicted longitudinal profiles are compared to the observation. A method for testing the hypothesis of a specific primary particle type against the measured profile is described which naturally takes shower fluctuations into account. The Fly's Eye event is compatible with any assumption of a hadron primary between proton and iron nuclei in both interaction models, although differences between QGSJET01 and SIBYLL2.1 in the predicted profiles of lighter nuclei exist. The primary ...

  2. CORSIKA implementation of heavy quark production and propagation in extensive air showers

    Science.gov (United States)

    Bueno, A.; Gascón, A.

    2014-02-01

    Heavy quarks are commonly produced in current accelerator experiments. Hence it is natural to think that they should be likewise created in collisions with larger center of mass energies like the ones involving ultra-high energy cosmic rays and atmospheric nuclei. Despite this fact, a detailed treatment of heavy hadrons is missing in Monte Carlo generators of Extensive Air Showers (EAS). It is a must to improve the description of how heavy flavors appear and evolve in atmospheric showers. With this goal in mind, we study two different models for heavy quark production in proton-air collisions. We also analyze a dedicated treatment of heavy hadrons interactions with atmospheric nuclei. This paper shows how those models have been implemented as new options available in CORSIKA, one of the most used EAS simulators. This new computational tool allows us to analyze the effects that the propagation of heavy hadrons has in the EAS development.

  3. The center of lateral iso-density contours for inclined cosmic air showers

    CERN Document Server

    Montanus, J M C

    2015-01-01

    The lateral density of a cosmic air shower with a non-zero zenith angle is azimuthally asymmetric. The azimuthal asymmetry consist of a stretching of the iso-density contours to ellipses and to a shift of the center of the elliptic contours with respect to the core of the shower. The aim of the paper is to investigate the shift of the center of the elliptic iso-density contours for different zenith angles . On the basis of a model a qualitative equation is derived for the iso-density contours of inclined showers including the shift. to obtain a quantitative equation MC densities are investigated. The shift can be incorporated in an analytic expression of the azimuthal asymmetry of the lateral density as a function of the polar coordinates and parameterized by the zenith angle. Its predictions for asymmetric lateral densities are compared with densities obtained with MC simulations.

  4. Atmospheric effects on extensive air showers observed with the Surface Detector of the Pierre Auger Observatory

    Czech Academy of Sciences Publication Activity Database

    Abraham, J.; Abreu, M.; Aglietta, M.; Boháčová, Martina; Chudoba, Jiří; Halenka, V.; Hrabovský, Miroslav; Kárová, Tatiana; Mandát, Dušan; Nečesal, Petr; Nožka, Libor; Nyklíček, M.; Palatka, Miroslav; Pech, Miroslav; Prouza, Michael; Rössler, T.; Řídký, Jan; Schovancová, Jaroslava; Schovánek, Petr; Šmída, Radomír; Trávníček, Petr

    2009-01-01

    Roč. 32, č. 2 (2009), s. 89-99. ISSN 0927-6505 R&D Projects: GA AV ČR KJB100100904; GA AV ČR KJB300100801; GA MŠk(CZ) LA08016; GA MŠk(CZ) 1M06002 Institutional research plan: CEZ:AV0Z10100502; CEZ:AV0Z10100522 Keywords : extensive air showers * UHECR * atmosphere * weather Subject RIV: BF - Elementary Particles and High Energy Physics Impact factor: 4.136, year: 2009 http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6TJ1-4WNRK08-1&_user=625012&_coverDate=09%2F30%2F2009&_rdoc=2&_fmt=high&_orig=browse&_srch=d

  5. Investigations of the fluctuations of the muon component of extensive air showers at mountain altitudes

    International Nuclear Information System (INIS)

    We present results of fluctuations of the muon component (muon threshold energy Esub(μ) >= 5 GeV) of extensive air showers (EAS) for a fixed size Nsub(e) in an interval 105 6 at a mean distance of 38 m from the shower axis and at a depth in the atmosphere of 690 g cm-2. The data were collected by the Tien-Shan EAS arrangement (altitude 3,340 m a.s.l). The standard deviations of the 'development' fluctuations have been estimated by subtraction of the 'observed' and 'reception' fluctuations assuming a GAMMA-distribution of the muon density spectrum using a maximun-likelihood method. The results show that the 'development' fluctuations remain almost unchanged and have a standard deviation of about 0.3. (orig.)

  6. Air shower simulation for background estimation in muon tomography of volcanoes

    Directory of Open Access Journals (Sweden)

    S. Béné

    2012-08-01

    Full Text Available One of the main sources of background for the radiography of volcanoes with atmospheric muons comes from the accidental coincidences produced in the muon telescopes by the air showers. In order to quantify this background, Monte-Carlo simulations of the showers and of the detector are developed by the Tomuvol collaboration. As a first step, the atmospheric showers were simulated and investigated using two Monte-Carlo packages, CORSIKA and GEANT4. We compared the results provided by the two programs for the muonic component of vertical proton-induced showers at three energies: 1, 10 and 100 TeV. We found that the spatial distribution and energy spectrum of the muons were in good agreement for the two codes, while significant differences were observed for the arrival time of the muons.

  7. Air shower simulation for background estimation in muon tomography of volcanoes

    Directory of Open Access Journals (Sweden)

    S. Béné

    2013-01-01

    Full Text Available One of the main sources of background for the radiography of volcanoes using atmospheric muons comes from the accidental coincidences produced in the muon telescopes by charged particles belonging to the air shower generated by the primary cosmic ray. In order to quantify this background effect, Monte Carlo simulations of the showers and of the detector are developed by the TOMUVOL collaboration. As a first step, the atmospheric showers were simulated and investigated using two Monte Carlo packages, CORSIKA and GEANT4. We compared the results provided by the two programs for the muonic component of vertical proton-induced showers at three energies: 1, 10 and 100 TeV. We found that the spatial distribution and energy spectrum of the muons were in good agreement for the two codes.

  8. Quantum Black Holes Effects on the Shape of Extensive Air Showers

    CERN Document Server

    Arsene, Nicusor; Denton, Peter B; Micu, Octavian

    2013-01-01

    We investigate the possibility to find a characteristic TeV scale quantum black holes decay signature in the data recorded by cosmic rays experiments. TeV black holes can be produced via the collisions of ultra high energetic protons (E > $10^18$ eV) with nucleons the from atmosphere. We focus on the case when the black holes decay into two particles moving in the forward direction in the Earth reference frame (back-to-back in the center of mass reference frame) and induce two overlapping showers. When reconstructing both the energy and the shape of the resultant air shower, there is a significant difference between showers induced only via standard model interactions and showers produced via the back-to-back decay of black holes as intermediate states.

  9. Implementing the De-thinning Method for High Energy Cosmic Rays Extensive Air Shower Simulations

    CERN Document Server

    Estupiñán, A; Núñez, L A

    2015-01-01

    To simulate the interaction of cosmic rays with the Earth atmosphere requires highly complex computational resources and several statistical techniques have been developed to simplify those calculations. It is common to implement the thinning algorithms to reduce the number of secondary particles by assigning weights to representative particles in the evolution of the cascade. However, since this is a compression method with information loss, it is required to recover the original flux of secondary particles without introduce artificial biases. In this work we present the preliminary results of our version of the de-thinning algorithm for the reconstruction of thinned simulations of extensive air showers initiated by cosmic rays and photons in the energy range $10^{15} < E/\\mathrm{eV} < 10^{17}$.

  10. What do we learn about hadronic interactions at ultrahigh energies from extensive air shower observations?

    International Nuclear Information System (INIS)

    The interpretation of extensive air shower (EAS) observations needs a sufficiently accurate knowledge of the interactions driving the cascade development in the atmosphere. While the electromagnetic and weak interaction parts do not provide principal problems, the hadronic interaction is a subject of uncertainties and debates, especially in the ultrahigh energy region extending the energy limits of man made accelerators and experimental knowledge from collider experiments. Since the EAS development is dominantly governed by soft processes, which are presently not accessible to a perturbative QCD treatment, one has to rely on QCD inspired phenomenological interaction models, in particular on string-models based on the Gribov-Regge theory like QGSJET, VENUS and SYBILL. Recent results of the EAS experiments KASCADE are scrutinized in terms of such models used as generators in the Monte Carlo EAS simulation code CORSIKA. (author)

  11. Changes in extensive air showers from isotropic Lorentz violation in the photon sector

    CERN Document Server

    Diaz, J S; Risse, M

    2016-01-01

    We consider a theory with isotropic nonbirefringent Lorentz violation in the photon sector and explore the effects on the development of the electromagnetic component of extensive air showers in the Earth atmosphere. Specifically, we consider the case of a "fast" photon with a phase velocity larger than the maximum attainable velocity of a massive Dirac fermion (this case corresponds to a negative Lorentz-violating parameter $\\kappa$ in the action). The production of photons with energies above the threshold for photon decay prevents the conventional production of electron-positron pairs, which gets replaced by the prompt decay of photons into electron-positron pairs. This rapid production of charged leptons accelerates the shower development, decreasing the atmospheric depth of the shower maximum ($X_\\text{max}$) by an amount which could be measured by cosmic-ray observatories. Precise measurements of $X_\\text{max}$ could then improve existing limits on the negative Lorentz-violating parameter $\\kappa$ by se...

  12. On some peculiarities of extensive air showers initiated by gamma-rays of extremely high energies

    International Nuclear Information System (INIS)

    The number of low-energy muons (Eμ ≤ 1 GeV) in extensive air showers (EAS) initiated by primary gamma-rays of extremely high energies is calculated. It is shown that at large depths (z ≥ 1000 g/cm2) the number of low-energy muons in EAS from gamma-rays with energy E0 ≥ 1018 eV is of the same order as in the proton-induced shower, as opposed to the energy range E0 ∼ 1015 eV, where the gamma-showers are muon-poor. The influence of the Landau-Pomeranchuk-Migdal effect and of the interaction of the primary photon with the geomagnetic field on the development of an electromagnetic shower in the Earth atmosphere at energies E0 ≥ 1019 eV is investigated. 22 refs.; 6 figs

  13. Time structure of extensive air shower at a distance of 100-800 m from axis

    International Nuclear Information System (INIS)

    Temporal structure of extensive air shower is investigated. Particle arrival time distributions at a distance of 100-800 m from the shower axis are analysed. Time distributions, corresponding to the passage through the detectors of both single f1(t) particles and a certain number of fn(t) particles (fn(t)-the first particle delay distribution at the n particle passage) are obtained. fn(t) distribution may as well be obtained from f1(t) distribution by simulating n particle passage, given that each particle passage does not depend on the passage of the other ones. The data available show, that there are no indications of experimental distribution deviations from the calculated ones

  14. Study on the muon component of extensive air showers by means of the underground magnetic spectrometer

    Energy Technology Data Exchange (ETDEWEB)

    Kulikov, G.V.; Rozhdestvenskij, S.M.; Solov' eva, V.I.; Khrenov, B.A.; Khristiansen, G.B.; Vdovchik, E.; Olejnichak, Ya. (Lodz Univ. (Poland). Inst. Fizyki; Moskovskij Gosudarstvennyj Univ. (USSR). Nauchno-Issledovatel' skij Inst. Yadernoj Fiziki)

    1980-01-01

    Muon component of extensive air-showers (EAS) was measured by means of a magnetic spectrometer placed at a depth of 40 m w.e. in the center of the MSU complex facility. Given are data on the density of the muon component with different threshold energy in EAS with the particle quantity N=2x10/sup 5/, muon energy spectrum as a whole in EAS as well as the most interesting space-energy characteristics of the muon component. Experimental data are most close to theoretical obtained from the calculation according to the model of high multiplicity in the case of the standard composition of primary radiation. Tendency to the increase in the steepness of the energy spectrum with the growth of muon energy is noted. In the energy range E=100-500 ueV the index of energy spectrum ..gamma..=1.8+-0.15.

  15. Study on the muon component of extensive air showers by means of the underground magnetic spectrometer

    International Nuclear Information System (INIS)

    Muon component of extensive air-showers (EAS) was measured by means of a magnetic spectrometer placed at a depth of 40 m w.e. in the center of the MSU complex facility. Given are data on the density of the muon component with different threshold energy in EAS with the particle quantity N=2x105, muon energy spectrum as a whole in EAS as well as the most interesting space-energy characteristics of the muon component. Experimental data are most close to theoretical obtained from the calculation according to the model of high nultiplicity in the case of the standard composition of primary radiation. Tendency to the increase in the steepness of the energy spectrum with the growth of muon energy is noted. In the energy range E=100-500 ueV the index of energy spectrum ν=1.8+-0.15

  16. On the Possibility of Radar Detection of Ultra-high Energy Cosmic Ray- and Neutrino-induced Air Showers

    Science.gov (United States)

    Gorham, P.

    1999-01-01

    We show that cosmic rays air showers resulting from primaries with energies above 10(sup 19) eV should be straightforward to detect with radar ranging techniques, where the radar echoes are produced by scattering from the column of ionized air produced by the shower.

  17. Electrons, muons and hadrons in extensive air showers and how do they depend on nuclear interaction model, part 1

    Science.gov (United States)

    Wrotniak, J. A.; Yodh, G. B.

    1985-01-01

    Monte Carlo simulations of extensive air showers were performed using a couple of different nuclear interaction models and obtaining a variety of shower characteristics. The discussion of these shows that the sensitivity of observables to the primary mass spectrum is significantly stronger than to the interaction model, the latter being quite weak.

  18. Status of the Whipple Observatory Cerenkov air shower imaging telescope array

    Science.gov (United States)

    Akerlof, C. W.; Cawley, M. F.; Fegan, D. J.; Fennell, S.; Freeman, S.; Frishman, D.; Harris, K.; Hillas, A. M.; Jennings, D.; Lamb, R. C.

    1992-01-01

    Recently the power of the Cerenkov imaging technique in Very High Energy gamma-ray astronomy was demonstrated by the detection of the Crab nebula at high statistical significance. In order to further develop this technique to allow the detection of weaker or more distant sources a second 10 m class reflector was constructed about 120 m from the original instrument. The addition of the second reflector will allow both a reduction in the energy threshold and an improvement in the rejection of the hadronic background. The design and construction of the second reflector, Gamma Ray Astrophysics New Imaging TElescope (GRANITE) is described.

  19. Nuclear composition of 1- to 20-PeV primary cosmic rays according to lateral features of the electron-photon component of all extensive air showers and of extensive air showers accompanying high-energy gamma rays and hadrons in X-ray emulsion chambers at the Tien Shan level

    International Nuclear Information System (INIS)

    Data from the Tien Shan array Adron on the dependence of the lateral distributions of the electron-photon component (age parameter S) in extensive air showers of cosmic rays on the number of electrons, Ne, which is a quantity that characterizes the primary-nucleus energy E0, are subjected to a comparative analysis. The distributions in question are given both for all showers and for showers accompanying high-energy gamma rays and hadrons in x-ray emulsion chambers. According to calculations, events associated with the latter are generated predominantly by primary protons, and this makes it possible to assess their role at various values of E0. The distributions with respect to S suggest a significant fraction of light nuclei, predominantly protons, in the region after the knee in the spectrum for Ne > 106, at least up to Ne = 5.6 x 106 (E0 ∼ 10 PeV)

  20. Accelerator measurements of magnetically-induced radio emission from particle cascades with applications to cosmic-ray air showers

    CERN Document Server

    Belov, K; Romero-Wolf, A; Wissel, S A; Zilles, A; Bechtol, K; Borch, K; Chen, P; Clem, J; Gorham, P W; Hast, C; Huege, T; Hyneman, R; Jobe, K; Kuwatani, K; Lam, J; Liu, T; Nam, J; Naudet, C; Nichol, R; Rauch, B F; Rotter, B; Saltzberg, D; Schoorlemmer, H; Seckel, D; Strutt, B; Vieregg, A G; Williams, C

    2015-01-01

    An experiment at SLAC provides the first beam test of radio-frequency (RF) radiation from a charged particle cascade in the presence of a magnetic field (up to $\\sim$1~kG), a model system for RF emission from a cosmic-ray air shower. This experiment provides a suite of controlled laboratory measurements to compare to particle-level simulations of RF emission, which are relied upon in ultra-high-energy cosmic-ray air shower detection. We compare simulations to data for intensity, linearity with magnetic field, angular distribution, polarization, and spectral content. In particular, we confirm recent predictions that the magnetically induced emission forms a beam that peaks at the Cherenkov angle and show that the simulations reproduce the data within systematic uncertainties.

  1. Measurement of the lateral distribution function of radio emission from ultra high energy cosmic ray induced air showers

    International Nuclear Information System (INIS)

    The Radio Detector of the Pierre Auger Observatory recorded 492 air shower events in coincidence with the Auger Surface Detector from April 2007 till May 2008. We investigate the lateral distribution function (LDF) which describes the variation of the radio signal with different positions of the observer and the shower axis. As observable we choose the relative difference of the radio signal intensity observed in single air shower events with the two logarithmic-periodic dipole antennas of the setup. We find that this observable is sensitive to the LDF when observed as a function of distance D between the antennas and the shower axis. Using Monte-Carlo techniques to estimate the impact of experimental uncertainties on our measurements we find that a purely exponential shape of the LDF is unlikely to explain the measurements. We observe that a better agreement can be achieved with an LDF model that exhibits a lateral falloff ∝1/Dk with k ∼1.2.

  2. Measurements in the Forward Phase-Space with the CMS Experiment and their Impact on Physics of Extensive Air Showers

    CERN Document Server

    AUTHOR|(CDS)2083313; Quast, Günter; Ulrich, Ralf

    2015-11-18

    The astrophysical interpretation of ultra-high energy cosmic rays is based on detection of extensive air showers in indirect measurements. Hadronic interaction models that are needed for such analyses require parameters to be adjusted to collider data since soft particle production cannot be calculated from first principles. Within this work, the program CRMC was developed that unifies all air shower hadronic interaction models and supports the output formats used by collider experiments. Almost all LHC experiments have adopted the use these hadronic interaction models thanks to CRMC. The program can even be used in detector simulations to make direct comparison to reconstructed quantities from which the cosmic ray and the particle physics communities benefit immensely. Furthermore, nuclear effects were studied with the CMS experiments at the LHC. The production cross section was derived in recent proton-lead collision data at sqrt(s(NN)) = 5.02 TeV in order to study nuclear effects. The measurement constrain...

  3. Low-frequency radio emission caused by coherent magnetic Bremsstrahlung of charged particles of extensive air showers

    International Nuclear Information System (INIS)

    The possibility of detecting the high-energy cosmic rays by the magnetobremsstrahlung coherent low-frequency radiation of the extensive air shower is studied. It is shown that the field intensity for such a radio emission constitutes approximately 200 μkV/m MHz at the distance of 100 km for the particle with the initial energy of 1021 eV. The high intensity of the field, caused by this radiation mechanism, makes it possible to consider that it is the cause of the earlier determined high intensity of the shower radio emission on the low frequencies. The possibility of radio detection of the cosmic rays with the energy above 1021 eV is considered. The studies on the radio pulses accompanying the extensive air shower (EAS), are carried out by means of high-speed electronics. The EAS signal duration is evaluated as 10-20 μs

  4. Measurements of the Depth of Maximum of Air-Shower Profiles at the Pierre Auger Observatory and their Composition Implications

    Science.gov (United States)

    de Souza, V.

    We describe how the analysis of air showers detected by the Pierre Auger Observatory leads to an accurate determination of the depth of maximum (Xmax). First, the analysis of the air-shower which leads to the reconstruction of Xmax is discussed. The properties of the detector and its measurement biases are treated and carefully taken into consideration. The Xmax results are interpreted in terms of composition, where the interpretation depends mainly on the hadronic interaction models. A global fit of the Xmax distribution yields an estimate of the abundance of four primaries species. The analysis represents the most statistically significant composition information ever obtained for energies above 1017.8 eV. The scenario that emerges shows no support for a strong flux of iron nuclei and a strong energy dependence of the proton fraction.

  5. IceVeto. An extension of IceTop to veto air showers for neutrino astronomy with IceCube

    International Nuclear Information System (INIS)

    IceCube is the world's largest high-energy neutrino observatory, built at the geographic South Pole. For neutrino astronomy, a large background-free sample of well-reconstructed astrophysical neutrinos is essential. The main background for this signal are muons and neutrinos which are produced in cosmic-ray air showers in the Earth's atmosphere. The coincident detection of these air showers by the surface detector IceTop has been proven to be a powerful veto for atmospheric neutrinos and muons in the field of view of the southern hemisphere. This motivates a significant extension of IceTop. First estimates indicate that such a veto detector will more than double the discovery potential of current point source analyses. Here, we present the motivation and capabilities of different technologies based on simulations and measurements.

  6. Results from Pion-Carbon Interactions Measured by NA61/SHINE for Improved Understanding of Extensive Air Showers

    CERN Document Server

    Hervé, Alexander E

    2015-01-01

    The interpretation of extensive air shower measurements, produced by ultra-high energy cosmic rays, relies on the correct modeling of the hadron-air interactions that occur during the shower development. The majority of hadronic particles are produced at equivalent beam energies below the TeV range. NA61/SHINE is a fixed target experiment using secondary beams produced at CERN at the SPS. Hadron-hadron interactions have been recorded at beam momenta between 13 and 350 GeV/c with a wide-acceptance spectrometer. In this contribution we present measurements of the spectra of charged pions and the $\\rho^0$ production in pion-carbon interactions, which are essential for modeling of air showers.

  7. Measuring a Cherenkov ring in the radio emission from air showers at 110-190 MHz with LOFAR

    CERN Document Server

    Nelles, A; Buitink, S; Corstanje, A; de Vries, K D; Enriquez, J E; Falcke, H; Frieswijk, W; Hörandel, J R; Scholten, O; ter Veen, S; Thoudam, S; Akker, M van den; Anderson, J; Asgekar, A; Bell, M E; Bentum, M J; Bernardi, G; Best, P; Bregman, J; Breitling, F; Broderick, J; Brouw, W N; Brüggen, M; Butcher, H R; Ciardi, B; Deller, A; Duscha, S; Eislöffel, J; Fallows, R A; Garrett, M A; Gunst, A W; Hassall, T E; Heald, G; Horneffer, A; Iacobelli, M; Juette, E; Karastergiou, A; Kondratiev, V I; Kramer, M; Kuniyoshi, M; Kuper, G; Maat, P; Mann, G; Mevius, M; Norden, M J; Paas, H; Pandey-Pommier, M; Pietka, G; Pizzo, R; Polatidis, A G; Reich, W; Röttgering, H; Scaife, A M M; Schwarz, D; Smirnov, O; Stapper, B W; Steinmetz, M; Stewart, A; Tagger, M; Tang, Y; Tasse, C; Vermeulen, R; Vocks, C; van Weeren, R J; Wijnholds, S J; Wucknitz, O; Yatawatta, S; Zarka, P

    2014-01-01

    Measuring radio emission from air showers offers a novel way to determine properties of the primary cosmic rays such as their mass and energy. Theory predicts that relativistic time compression effects lead to a ring of amplified emission which starts to dominate the emission pattern for frequencies above ~100 MHz. In this article we present the first detailed measurements of this structure. Ring structures in the radio emission of air showers are measured with the LOFAR radio telescope in the frequency range of 110 - 190 MHz. These data are well described by CoREAS simulations. They clearly confirm the importance of including the index of refraction of air as a function of height. Furthermore, the presence of the Cherenkov ring offers the possibility for a geometrical measurement of the depth of shower maximum, which in turn depends on the mass of the primary particle.

  8. IceVeto. An extension of IceTop to veto air showers for neutrino astronomy with IceCube

    Energy Technology Data Exchange (ETDEWEB)

    Auffenberg, Jan; Kemp, Julian; Raedel, Leif; Rongen, Martin; Schaufel, Merlin; Stahlberg, Martin; Hansmann, Bengt; Wiebusch, Christopher [RWTH Aachen University, Physikalische Institut III b (Germany); Collaboration: IceCube-Collaboration

    2015-07-01

    IceCube is the world's largest high-energy neutrino observatory, built at the geographic South Pole. For neutrino astronomy, a large background-free sample of well-reconstructed astrophysical neutrinos is essential. The main background for this signal are muons and neutrinos which are produced in cosmic-ray air showers in the Earth's atmosphere. The coincident detection of these air showers by the surface detector IceTop has been proven to be a powerful veto for atmospheric neutrinos and muons in the field of view of the southern hemisphere. This motivates a significant extension of IceTop. First estimates indicate that such a veto detector will more than double the discovery potential of current point source analyses. Here, we present the motivation and capabilities of different technologies based on simulations and measurements.

  9. Longitudinal profile of Nµ/Ne in extensive air showers: Implications for cosmic rays mass composition study

    Directory of Open Access Journals (Sweden)

    D Purmohammad

    2013-10-01

    Full Text Available Nµ/Ne, muon to electron population ratio in extensive air showers at high altitudes has been shown to be a suitable estimator of primary cosmic rays mass composition. This study is based on simulated extensive air showers. The Nµ/Ne ratio has been obtained in 100 depths from the top of the atmosphere to the sea level for different primary particle masses and energies. An empirical relation between cosmic ray atomic mass and Nµ/Ne has been obtained. The relation has then been used for estimation of atomic masses of progenitors of another set of simulated showers. Although the estimated masses are rough, the accuracy of the estimation improves with observation altitude.

  10. Minimal prospects for radio detection of extensive air showers in the atmosphere of Jupiter

    CERN Document Server

    Bray, J D

    2016-01-01

    One possible approach for detecting ultra-high-energy cosmic rays and neutrinos is to search for radio emission from extensive air showers created when they interact in the atmosphere of Jupiter, effectively utilizing Jupiter as a particle detector. We investigate the potential of this approach. For searches with current or planned radio telescopes we find that the effective area for detection of cosmic rays is substantial (~3*10^7 km^2), but the acceptance angle is so small that the typical geometric aperture (~10^3 km^2 sr) is less than that of existing terrestrial detectors, and cosmic rays also cannot be detected below an extremely high threshold energy (~10^23 eV). The geometric aperture for neutrinos is slightly larger, and greater sensitivity can be achieved with a radio detector on a Jupiter-orbiting satellite, but in neither case is this sufficient to constitute a practical detection technique. Exploitation of the large surface area of Jupiter for detecting ultra-high-energy particles remains a long-...

  11. Minimal Prospects for Radio Detection of Extensive Air Showers in the Atmosphere of Jupiter

    Science.gov (United States)

    Bray, J. D.; Nelles, A.

    2016-07-01

    One possible approach for detecting ultra-high-energy cosmic rays and neutrinos is to search for radio emission from extensive air showers created when they interact in the atmosphere of Jupiter, effectively utilizing Jupiter as a particle detector. We investigate the potential of this approach. For searches with current or planned radio telescopes we find that the effective area for detection of cosmic rays is substantial (∼3 × 107 km2), but the acceptance angle is so small that the typical geometric aperture (∼103 km2 sr) is less than that of existing terrestrial detectors, and cosmic rays also cannot be detected below an extremely high threshold energy (∼1023 eV). The geometric aperture for neutrinos is slightly larger, and greater sensitivity can be achieved with a radio detector on a Jupiter-orbiting satellite, but in neither case is this sufficient to constitute a practical detection technique. Exploitation of the large surface area of Jupiter for detecting ultra-high-energy particles remains a long-term prospect that will require a different technique, such as orbital fluorescence detection.

  12. Muon content of UHE air showers: discrimination method between electromagnetic and hadronic cascades

    International Nuclear Information System (INIS)

    Results from a detailed Monte Carlo simulation for the muon component of EAS, at mountain altitude (800 g cm-2), generated by vertical γ-rays, protons, oxygen and iron primary cosmic rays, in the energy range 1012-1016 eV, are provided for muon threshold energies from 0.1 to 100 GeV. In the simulation of the different components of the shower (μ±, e±, γ...), the CORSIKA (cosmic ray simulator for cascade) code has been used to allow for both, electromagnetic and hadronic interactions. Results on the variation and fluctuation of the total muon number with shower size and primary energy are obtained, as well as longitudinal developments, lateral distributions of low-energy muons in air showers and muon energy spectra. Moreover, analytical expressions are fitted to the muon lateral developments, and muon energy spectra have been parametrized to a log-normal distribution. Apart from their value as new results, they may be used for the design of current studies at mountain altitudes. We also seek to provide relations to interpret the experimental data, for those who do not have detailed simulation calculations available. (author)

  13. Photon air showers at ultra-high energy and the photonuclear cross-section

    CERN Document Server

    Risse, M; Engel, R; Gora, D; Heck, D; Pekala, J; Wilczynska, B; Wilczynski, H

    2006-01-01

    Experimental conclusions from air shower observations on cosmic-ray photons above 10^19 eV are based on the comparison to detailed shower simulations. For the calculations, the photonuclear cross-section needs to be extrapolated over several orders of magnitude in energy. The uncertainty from the cross-section extrapolation translates into an uncertainty of the predicted shower features for primary photons and, thus, into uncertainties for a possible data interpretation. After briefly reviewing the current status of ultra-high energy photon studies, the impact of the uncertainty of the photonuclear cross-section for shower calculations is investigated. Estimates for the uncertainties in the main shower observables are provided. Photon discrimination is shown to be possible even for rapidly rising cross-sections. When photon-initiated showers are identified, it is argued that the sensitivity of photon shower observables to the photonuclear cross-section can in turn be exploited to constrain the cross-section a...

  14. Reinterpreting the development of extensive air showers initiated by nuclei and photons

    CERN Document Server

    De Domenico, Manlio; Riggi, Simone; Bertin, Eric

    2013-01-01

    Ultra-high energy cosmic rays (UHECRs) interacting with the atmosphere generate extensive air showers (EAS) of secondary particles. The depth corresponding to the maximum development of the shower, $\\Xmax$, is a well-known observable for determining the nature of the primary cosmic ray which initiated the cascade process. In this paper, we present an empirical model to describe the distribution of $\\Xmax$ for EAS initiated by nuclei and photons in the energy range from $10^{17}$ eV up to $10^{21}$ eV. Our model adopts the generalized Gumbel distribution motivated by the relationship between the generalized Gumbel statistics and the distribution of the sum of non-identically distributed variables in dissipative stochastic systems. We provide an analytical expression for describing the $\\Xmax$ distribution for photons and for nuclei. The impact of the hadronic interaction model is investigated in detail, even in the case of the most up-to-date models accounting for LHC observations. We also briefly discuss the ...

  15. Updated Event Rate for Horizontal and Upward Tau Air Showers in EUSO

    CERN Document Server

    Fargion, D; De Santis, M

    2003-01-01

    There is more and more expectation on EUSO outcoming project. This experiment, while monitoring at dark, downward to the Earth, a wide atmosphere layers, may discover, among common downward Ultra High Energy Cosmic Rays, UHECR showers, also first High Energy Neutrino-Induced Showers. These events are either originated in Air (EUSO Field of View) or within a widest Earth Crust ring crown leading to ultra high energy Tau whose decay in flight produce up-ward and horizontal showers. Most of those vertical downward neutrinos induced Shower in air, are drown in the dominant noise of downward UHECR showers. We showed and refine here the signature of Upward and Horizontal Upward and Horizontal Tau Air-Showers, UPTAUS and HORTAUs (or also named Earth skimming neutrinos), born within widest Earth Crust Crown (Sea or Rock) Areas surrounding EUSO field of view. These UPTAUs and HORTAUs effective masses and the consequent EUSO event Number are estimated by an unified exact analytical formula. The effective target Masses ...

  16. $$ Uncertainty from Extrapolation of Cosmic Ray Air Shower Parameters

    CERN Document Server

    Abbasi, R U

    2016-01-01

    Recent measurements at the LHC of the p-p total cross section have reduced the uncertainty in simulations of cosmic ray air showers. In particular of the depth of shower maximum, called $X_{max}$. However, uncertainties of other important parameters, in particular the multiplicity and elasticity of high energy interactions, have not improved, and there is a remaining uncertainty due to the total cross section. Uncertainties due to extrapolations from accelerator data, at a maximum energy of $\\sim$ one TeV in the p-p center of mass, to 250 TeV ($3\\times10^{19}$ eV in a cosmic ray proton's lab frame) introduce significant uncertainties in predictions of $$. In this paper we estimate a lower limit on these uncertainties. The result is that the uncertainty in $$ is larger than the difference among the modern models being used in the field. At the full energy of the LHC, which is equivalent to $\\sim 1\\times10^{17}$ eV in the cosmic ray lab frame, the extrapolation is not as extreme, and the uncertainty is approxim...

  17. What do we learn about hadronic interactions at very high energies from extensive air shower observations?

    International Nuclear Information System (INIS)

    The development of Extensive Air Showers (EAS) is driven by the hadronic interactions of the primary and secondary particles with the atmospheric nuclei. Hence a careful analysis of the EAS appearance, in particular of the hadronic component, provides valuable information on features of the hadronic interaction. Especially, in ultrahigh energy regions extending the energy limits of man-made accelerators and the experimental knowledge from collider experiments, the hadronic interaction is subject of uncertainties and debates. Since the EAS development is dominantly governed by soft processes, which are not accessible to a perturbative QCD treatment, the interpretation of EAS observations has to rely on QCD inspired phenomenological interaction models, in particular on string models based on the Gribov-Regge theory, like VENUS, QGSJET and SIBYLL. The basic features of such models are sketched from point of view of a practical use as generators for EAS Monte Carlo simulations and analyses of experimental results. Applications are illustrated with various examples of EAS observations, scrutinised as source of information on very-high energy hadronic interaction features. (author)

  18. Measurements of the muon content of air showers at the Pierre Auger Observatory

    Science.gov (United States)

    Valiño, I.; Pierre Auger Collaboration

    2015-08-01

    The Pierre Auger Observatory offers a unique window to study cosmic rays and particle physics at energies above 3 EeV (corresponding to a centre-of-mass energy of 75 TeV in proton-proton collisions) inaccessible to accelerator experiments. We discuss the different methods of estimating the number of muons in showers recorded at the Pierre Auger Observatory, which is an observable sensitive to primary mass composition and to properties of the hadronic interactions in the shower. The muon content, derived from data with these methods, is presented and compared to predictions from the post-LHC hadronic interaction models for different primary composition. We find that models do not reproduce well the Auger observations, displaying a deficit of muons at the ground. In the light of these results, a better understanding of ultra-high energy extensive air showers and hadronic interactions is crucial to determine the composition of ultra-high energy cosmic rays. We report on the upgrade plans of the Pierre Auger Observatory to achieve this science goal.

  19. Test of hadronic interaction models by investigation of the hadronic component of extensive air showers

    International Nuclear Information System (INIS)

    At energies larger than 100 TeV the flux of cosmic rays becomes so small that direct measurements above the atmosphere are currently not possible. At higher energies ground based detector stations are used to measure the extensive air showers (EAS) induced by the primary cosmic rays. The interpretation of these measurements is based on the comparison with EAS simulations. The hadronic interactions are described by models which have to extrapolate to kinematical and energy ranges beyond the limits of present accelerator experiments. This extrapolation causes uncertainties in the simulations and in the interpretation of EAS measurements. For testing the hadronic interaction models DPMJET II.5, NEXUS 2, and QGSJET 98 in the EAS simulation program CORSIKA several hadronic observables as well as their correlations with the number of muons and electrons of EAS are investigated. The comparison of measurements of the EAS experiment KASCADE with simulations of primary protons and iron nuclei shows a good agreement between measurement and simulation in case of QGSJET. NEXUS shows problems in the correlation of the hadronic and the electromagnetic EAS components. For a fixed electron number the hadronic component is underestimated. DPMJET predicts a too late shower development in the atmosphere. This results in an overestimation of the hadronic and electromagnetic components at a fixed number of muons. (orig.)

  20. Simulation studies of the information content of muon arrival time observations of high energy extensive air showers

    International Nuclear Information System (INIS)

    By extensive Monte Carlo calculations, using the air shower simulation code CORSIKA, EAS muon arrival time distributions and EAS time profiles up to 320 m distances from the shower centre have been generated, for proton, oxygen and iron induced showers using different hadronic interaction models as Monte Carlo generators. The model dependence and mass discriminating features have been scrutinised for three energies ranges, (1.0-1.78) 1015 eV, (1.0-1.78) 1016 eV and (1.78-3.16) 1016 eV. The present studies have been focussed to the exploration of the information carried by EAS time observables and their correlations in view of features discriminating the mass of the cosmic primary and different hadronic interaction models. Advanced non-parametric statistical methods based on Bayesian decision rules have been applied to scrutinise the EAS observables and to specify quantitatively the results. A first inspection allows some tentative conclusions: 1. The correlations of the local muon arrival time variables with the local muon density improves the true classification rate and discrimination features. It turns out that the correlation can be replaced by a single parameter: Δτq/ρμ. The classification gets improved by correlating the muon arrival times with the shower age, the shower size Ne and Nμtr; 2. Correlating the observation of Δτq/ρμ for two radial distances, the mass discrimination of the primaries get only slightly improved, different from our previous results analysing the (global) arrival times of the foremost muon correlated at two different radial distances; 3. Comparing the classification rates for different muon arrival time quantities: the first quartile, the median and the third quartile, by both considered models QGSJET and VENUS similar results have been obtained.The analysis of the median Δτ0.50 and of the slow component of the arrival time distribution, represented by Δτ0.75, improves the true-classification rate of the oxygen component

  1. Impact of LHC data on the interpretation of Λ{sub η} measured from air-shower fluctuations

    Energy Technology Data Exchange (ETDEWEB)

    Kuotb Awad, Alaa; Baur, Sebastian; Akbiyik, Melike; Baus, Colin; Katkov, Igor; Ulrich, Ralf; Woehrmann, Hauke [KIT, Karlsruhe (Germany); Collaboration: Pierre Auger-Collaboration

    2015-07-01

    It is demonstrated how LHC data is used to improve interaction models. The impact on the interpretation of air-showers measurements is shown. An updated version of the conversion factor from Λ{sub η} to σ{sub p-air} is determined. The model-related uncertainties are reduced with the new interaction models, which results in more precise proton-air cross section measurements obtained from UHECR data.

  2. Impact of LHC data on the interpretation of Λη measured from air-shower fluctuations

    International Nuclear Information System (INIS)

    It is demonstrated how LHC data is used to improve interaction models. The impact on the interpretation of air-showers measurements is shown. An updated version of the conversion factor from Λη to σp-air is determined. The model-related uncertainties are reduced with the new interaction models, which results in more precise proton-air cross section measurements obtained from UHECR data.

  3. Weather induced effects on extensive air showers observed with the surface detector of the Pierre Auger Observatory

    CERN Document Server

    Bleve, Carla

    2007-01-01

    The rate of events measured with the surface detector of the Pierre Auger Observatory is found to be modulated by the weather conditions. This effect is due to the increasing amount of matter traversed by the shower as the ground pressure increases and to the inverse proportionality of the Moliere radius to the air density near ground. Air-shower simulations with different realistic profiles of the atmosphere support this interpretation of the observed effects.

  4. A method for high precision reconstruction of air shower Xmax using two-dimensional radio intensity profiles

    CERN Document Server

    Buitink, S; Enriquez, J E; Halcke, H; Hörandel, J R; Huege, T; Nelles, A; Rachen, J P; Schellart, P; Scholten, O; ter Veen, S; Thoudam, S; Trinh, T N G

    2014-01-01

    The mass composition of cosmic rays contains important clues about their origin. Accurate measurements are needed to resolve long-standing issues such as the transition from Galactic to extragalactic origin, and the nature of the cutoff observed at the highest energies. Composition can be studied by measuring the atmospheric depth of the shower maximum Xmax of air showers generated by high-energy cosmic rays hitting the Earth's atmosphere. We present a new method to reconstruct Xmax based on radio measurements. The radio emission mechanism of air showers is a complex process that creates an asymmetric intensity pattern on the ground. The shape of this pattern strongly depends on the longitudinal development of the shower. We reconstruct Xmax by fitting two-dimensional intensity profiles, simulated with CoREAS, to data from the LOFAR radio telescope. In the dense LOFAR core, air showers are detected by hundreds of antennas simultaneously. The simulations fit the data very well, indicating that the radiation me...

  5. The primary composition beyond 10 to the 5th power GeV as deduced from high energy hadrons and muons in air showers

    Science.gov (United States)

    Grieder, P. K. F.

    1985-01-01

    Data obtained from a large set of air shower simulation calculations with use of highly refined hadronic interaction and shower simulation model are presented, in an attempt to solve the problem of primary chemical composition beyond 100,000 GeV total energy. It is rated that high energy hadrons in air showers offer a rather unique primary mass signature and show that the interpretation of high energy muon data is much more ambiguous. Predictions are compared with experimental data.

  6. Large-Area, UV-Optimized, Back-Illuminated Silicon Photomultiplier Arrays Project

    Data.gov (United States)

    National Aeronautics and Space Administration — Large-area (3m2), UV-sensitive focal plane arrays are needed for observation of air showers from ultra-high energy cosmic rays (JEM-EUSO) as well as for...

  7. Measurement of arrival time of particles in extensive air showers using TDC32

    Science.gov (United States)

    Gupta, S. K.; Christiansen, J.; Hayashi, Y.; Jain, A.; Mohanty, P. K.; Ravindran, K. C.; Satyanarayana, B.

    2013-04-01

    Arrival time of particles in an extensive air shower (EAS) is a key physical parameter to determine its direction. EAS direction is useful for studies of anisotropy and composition of cosmic rays, and search for multi-TeV γ-rays sources. Accurate timing may be used to search exotic phenomena such as production of new particles at extremely high energies available during early stages of development of EAS and also for detecting sub-relativistic hadrons in EAS. Time to digital converters (TDCs) are used to perform this task. Traditional TDCs operate in the START-STOP mode with limited dynamic range and single-hit capability. With the advent of high luminosity collider LHC, need for TDCs with large dynamic range, multi-hit capability and TRIGGERED mode of operation became necessary. A 32 channel TDC was designed for the GRAPES-3 experiment on a CAMAC platform around TDC32, an ASIC developed by micro-electronics group at CERN, Geneva. Four modules were operated in the GRAPES-3 experiment. Here, we present details of the circuit design and their performance over several years. The multi-hit feature of this device was used to study the time structure of particles in the EAS on time scale of ~1 μs. The distribution of time intervals in the multi-hit data shows an exponential profile with a time constant of ~370 ns. These delayed particles are likely to be neutrons produced in the EAS core that were recorded in the scintillator detectors following the relativistic EAS front.

  8. Core structure of extensive air showers at primary energies around the knee by a multifractal moments analysis

    International Nuclear Information System (INIS)

    Patterns of particle distributions in the core of extensive air showers, measured by multiwire proportional chambers installed below the central detector of the KASCADE experiment are analysed in terms of multifractal moments. Correlating the obtained mass sensitive parameters with the shower size and the number of reconstructed muons in the core region, an artificial neural net analysis leads to probability distributions for associating single showers to particular primary masses. The resulting chemical composition in the energy region of the knee tends to a heavier composition after the knee. The knee position seems to be shifted to higher energies in case of heavy primary cosmic rays

  9. Electrons, muons and hadrons in extensive air showers and how do they depend on nuclear interaction model, part 2

    Science.gov (United States)

    Wrotniak, J. A.; Yodh, G. B.

    1985-01-01

    Some of the results of Monte Carlo simulations of extensive air showers for nuclear interactions models are presented. The most significant part of scaling violation effect is generated by the inclusion of rising cross-section. Among the models considered the lowest value for Eo/N(max) is obtained when rapidly rising cross-section and charge exchange are both included (model R-F01). The value is still 1.38 GeV/electron. Except at the highest energies, the sensitivity to atomic mass of the primary is greater than to specific assumptions about multiple production.

  10. Weather induced effects on extensive air showers observed with the surface detector of the Pierre Auger Observatory

    Science.gov (United States)

    Bleve, Carla

    The rate of events measured with the surface detector (SD) of the Pierre Auger Observatory is found to be modulated by the weather conditions. This effect, observed in different ranges of S(1000), the signal measured at 1000 m from the shower core, is due to the increasing amount of matter traversed by a shower as the ground pressure increases and to the inverse proportionality of the Moliere radius to the air density near ground. The latter effect results in a modulation of the lateral spread of the shower with T and P. Air- shower simulations with different realistic profiles of the atmosphere support this interpretation of the observed effects.

  11. Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

    CERN Document Server

    Homola, Piotr; Wilczyński, Henryk

    2014-01-01

    The angular distribution of Cherenkov light in an air shower is closely linked to that of the shower electrons and positrons. As charged particles in extensive air showers are deflected by the magnetic field of the Earth, a deformation of the angular distribution of the Cherenkov light, that would be approximately symmetric about the shower axis if no magnetic field were present, is expected. In this work we study the variation of the Cherenkov light distribution as a function of the azimuth angle in the plane perpendicular to shower axis. It is found that the asymmetry induced by the geomagnetic field is most significant for early stages of shower evolution and for showers arriving almost perpendicular to the vector of the local geomagnetic field. Furthermore, it is shown that ignoring the azimuthal asymmetry of Cherenkov light might lead to a significant under- or overestimation of the Cherenkov light signal especially at sites where the local geomagnetic field is strong. Based on CORSIKA simulations, the a...

  12. Search for very high-energy neutrinos by SHALON (Cherenkov radiation of extensive air showers observed at large zenith angles)

    Energy Technology Data Exchange (ETDEWEB)

    Sinitsyna, V.G. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation); Arsov, T.P. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation); Borisov, S.S. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation); Musin, F.I. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation); Nikolsky, S.I. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation); Malyshko, A.A. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation); Sinitsyna, V.Y. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation); Platonov, G.F. [P.N.Lebedev Physical Institute, Leninsky pr.53, Moscow (Russian Federation)

    2006-01-15

    The detection of extraterrestrial very high energy neutrinos by the atmospheric Cherenkov telescopic system SHALON is discussed. The analysis of results of observation of extensive air showers at 3338 m above sea level by means of the gamma-telescope SHALON at zenith angles 72{sup o}, 76{sup o}, 84{sup o}, 96{sup o} are presented. The observed results are compared with the data of of shower according to zenith angle. The observation has been carried out at Tien-Shan station with SHALON gamma-telescope. The SHALON telescopic system has mirror with area of 11.2m{sup 2} and 144 PMT matrix with 0.2{sup o} angular resolution, and has the largest angular acceptance in the world - > 8{sup o}. It allows to continuously control the background of cosmic ray particle emission and the atmospheric transparency with observation thus increasing observation efficiency. It is the telescope characteristics that permit to start searching for local neutrino sources with energy 10{sup 13}-10{sup 15} eV on EAS generated in mountain-range located at some 5 and more kilometers from the gamma-telescope (in Russian the SHALON abbreviation means - the Extensive Air Showers from Neutrino)

  13. Reconstructing energy and Xmax of cosmic ray air showers using the radio lateral distribution measured with LOPES

    CERN Document Server

    Apel, W D; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Chiavassa, A; Daumiller, K; de Souza, V; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Fuchs, B; Fuhrmann, D; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Łuczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmid, A; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Wommer, M; Zabierowski, J; Zensus, J A

    2013-01-01

    The LOPES experiment, a digital radio interferometer located at KIT (Karlsruhe Institute of Technology), obtained remarkable results for the detection of radio emission from extensive air showers at MHz frequencies. Features of the radio lateral distribution function (LDF) measured by LOPES are explored in this work for a precise reconstruction of two fundamental air shower parameters: the primary energy and the shower Xmax. The method presented here has been developed on (REAS3-)simulations, and is applied to LOPES measurements. Despite the high human-made noise at the LOPES site, it is possible to reconstruct both the energy and Xmax for individual events. On the one hand, the energy resolution is promising and comparable to the one of the co-located KASCADE-Grande experiment. On the other hand, Xmax values are reconstructed with the LOPES measurements with a resolution of 90 g/cm2 . A precision on Xmax better than 30 g/cm2 is predicted and achievable in a region with a lower human-made noise level.

  14. Progress report on a new search for free e/3 quarks in the cores of 10(15) - 10(16) eV air showers

    Science.gov (United States)

    Hodson, A. L.; Bull, R. M.; Taylor, R. S.; Belford, C. H.

    1985-01-01

    The Leeds 3 sq m Wilson cloud chamber is being used in a new search for free e/3 quarks close to the axes of 10 to the 15th power - 10 to the 16th power eV air showers. A ratio trigger circuit is used to detect the incidence of air shower cores; the position of the shower center and the axis direction are determined from photographs of current-limited spark chambers. It is thus possible, for the first time, to know where we have looked for quarks in air showers and to select for scanning only those cloud chamber photographs where we have good evidence that the shower axis was close to the chamber. 250 g/sq cm of lead/concrete absorber above the cloud chamber serve to reduce particle densities and make a quark search possible very close to the shower axes. The current status of the search is given.

  15. Muon components detected by EAS array and Okayama muon telescope experiments

    International Nuclear Information System (INIS)

    The Okayama muon telescope and the extensive air shower (EAS) array in Large Area Air Shower (LAAS) experiments were used to measure both muon and electron components in EAS events. The average ratio of the number of muon tracks to electron tracks 0.01 ± 0.005 was derived from this analysis, which is consistent with the typical core distance of EAS from the telescope in PeV energies derived from EAS simulation results

  16. Results and Perspectives of the Auger Engineering Radio Array

    CERN Document Server

    ,

    2016-01-01

    The Auger Engineering Radio Array (AERA) is an extension of the Pierre Auger Cosmic-Ray Observatory. It is used to detect radio emission from extensive air showers with energies beyond $10^{17}~$eV in the $30 - 80~$MHz frequency band. After three phases of deployment, AERA now consists of more than 150 autonomous radio stations with different spacings, covering an area of about $17~$km$^2$. It is located at the same site as other Auger low-energy detector extensions enabling combinations with various other measurement techniques. The radio array allows different technical schemes to be explored as well as cross-calibration of our measurements with the established baseline detectors of the Auger Observatory. We report on the most recent technological developments and give an overview of the experimental results obtained with AERA. In particular, we will present the measurement of the radiation energy, i.e., the amount of energy that is emitted by the air shower in the form of radio emission, and its dependence...

  17. Muons (≥1 GeV) in large extensive air showers of energies between 1016.5 eV and 1019.5 eV observed at Akeno

    International Nuclear Information System (INIS)

    The properties of muons (≥1 GeV) in giant air showers between 1016.5 eV and 1019.5 eV are measured by the Akeno 1 km2, 20 km2 and 100 km2 air shower arrays. The lateral distribution of muons is well fitted by the formula given by Greisen (1960) with parameters β=2.52±0.02 and log(R0)=(0.58±0.04) (sec θ -1)+(2.39±0.05) between 1016.5 eV and 1019.0 eV within 800 m of the air shower axis, where theta is the zenith angle of the shower arrival direction. The relation between the total number of muons (Nμ) and the total number of electrons (Ne) derived using these parameters is expressed on average as Nμ (2:6±1.3)x105.0+ α (Ne/107)b where α=(1.07±0.13) (sec θ -1) and b=(0.77±0.02)-(0.17±0.02) (sec θ -1). The lateral distribution of muons becomes steeper than expected from extrapolation of the above formula for core distances >800 m and is expressed as ρ μ = Nμ (C'μ/R02)r-0.75 (1+r)-β (1+(R/800 m)3)-δ (r=R/R0, where R is a core distance). No deviation from this formula has been observed for sec θ 19.0 eV. The relation between the muon density (S(600)) and the charged-particle density on the ground at 600 m from the core (S(600)) is studied between 1016.5 eV and 1019.0 eV. A systematic change in the chemical composition of cosmic rays from a predominantly heavy to a predominantly light composition above 1017.5 eV claimed by the Fly's Eye group has not been detected beyond the present experimental uncertainties. The present experiment suggests a much smaller rate of change of composition between 1017.5 eV and 1018.5 eV than that from the Fly's Eye experiment. (author)

  18. Array size scaling of passive coherent beam combination in fiber laser array

    Institute of Scientific and Technical Information of China (English)

    Yuhao Xue; Bing He; Jun Zhou; Jinchong Xue; Zhen Li; Houkang Liu; Qihong Lou

    2012-01-01

    Array size scaling of passive coherent beam combination is explored theoretically.The Strehl ratio variation with wavelength is simulated in 4-,9-,16-,and 25-channel fiber arrays.The average Strehl ratio and phase error are calculated.The Strehl ratio is found to be near 100% for arrays with less than 5 fibers,but decreases significantly for larger arrays.These results are in good agreement with the recent experimental results.

  19. Measurement of the Depth of Maximum of Extensive Air Showers above 10^18 eV

    Energy Technology Data Exchange (ETDEWEB)

    Abraham, J.; /Buenos Aires, CONICET; Abreu, P.; /Lisbon, IST; Aglietta, M.; /Turin U. /INFN, Turin; Ahn, E.J.; /Fermilab; Allard, D.; /APC, Paris; Allekotte, I.; /Centro Atomico Bariloche /Buenos Aires, CONICET; Allen, J.; /New York U.; Alvarez-Muniz, J.; /Santiago de Compostela U.; Ambrosio, M.; /Naples U.; Anchordoqui, L.; /Wisconsin U., Milwaukee; Andringa, S.; /Lisbon, IST /Boskovic Inst., Zagreb

    2010-02-01

    We describe the measurement of the depth of maximum, X{sub max}, of the longitudinal development of air showers induced by cosmic rays. Almost 4000 events above 10{sup 18} eV observed by the fluorescence detector of the Pierre Auger Observatory in coincidence with at least one surface detector station are selected for the analysis. The average shower maximum was found to evolve with energy at a rate of (106{sub -21}{sup +35}) g/cm{sup 2}/decade below 10{sup 18.24 {+-} 0.05}eV, and (24 {+-} 3) g/cm{sup 2}/decade above this energy. The measured shower-to-shower fluctuations decrease from about 55 to 26 g/cm{sup 2}. The interpretation of these results in terms of the cosmic ray mass composition is briefly discussed.

  20. Measurement of the depth of maximum of extensive air showers above 10{18} eV.

    Science.gov (United States)

    Abraham, J; Abreu, P; Aglietta, M; Ahn, E J; Allard, D; Allekotte, I; Allen, J; Alvarez-Muñiz, J; Ambrosio, M; Anchordoqui, L; Andringa, S; Anticić, T; Anzalone, A; Aramo, C; Arganda, E; Arisaka, K; Arqueros, F; Asorey, H; Assis, P; Aublin, J; Ave, M; Avila, G; Bäcker, T; Badagnani, D; Balzer, M; Barber, K B; Barbosa, A F; Barroso, S L C; Baughman, B; Bauleo, P; Beatty, J J; Becker, B R; Becker, K H; Bellétoile, A; Bellido, J A; Benzvi, S; Berat, C; Bergmann, T; Bertou, X; Biermann, P L; Billoir, P; Blanch-Bigas, O; Blanco, F; Blanco, M; Bleve, C; Blümer, H; Bohácová, M; Boncioli, D; Bonifazi, C; Bonino, R; Borodai, N; Brack, J; Brogueira, P; Brown, W C; Bruijn, R; Buchholz, P; Bueno, A; Burton, R E; Busca, N G; Caballero-Mora, K S; Caramete, L; Caruso, R; Castellina, A; Catalano, O; Cataldi, G; Cazon, L; Cester, R; Chauvin, J; Chiavassa, A; Chinellato, J A; Chou, A; Chudoba, J; Clay, R W; Colombo, E; Coluccia, M R; Conceição, R; Contreras, F; Cook, H; Cooper, M J; Coppens, J; Cordier, A; Cotti, U; Coutu, S; Covault, C E; Creusot, A; Criss, A; Cronin, J; Curutiu, A; Dagoret-Campagne, S; Dallier, R; Daumiller, K; Dawson, B R; de Almeida, R M; De Domenico, M; De Donato, C; de Jong, S J; De La Vega, G; de Mello Junior, W J M; de Mello Neto, J R T; De Mitri, I; de Souza, V; de Vries, K D; Decerprit, G; Del Peral, L; Deligny, O; Della Selva, A; Delle Fratte, C; Dembinski, H; Di Giulio, C; Diaz, J C; Díaz Castro, M L; Diep, P N; Dobrigkeit, C; D'Olivo, J C; Dong, P N; Dorofeev, A; Dos Anjos, J C; Dova, M T; D'Urso, D; Dutan, I; Duvernois, M A; Ebr, J; Engel, R; Erdmann, M; Escobar, C O; Etchegoyen, A; Facal San Luis, P; Falcke, H; Farrar, G; Fauth, A C; Fazzini, N; Ferrero, A; Fick, B; Filevich, A; Filipcic, A; Fleck, I; Fliescher, S; Fracchiolla, C E; Fraenkel, E D; Fröhlich, U; Fulgione, W; Gamarra, R F; Gambetta, S; García, B; García Gámez, D; Garcia-Pinto, D; Garrido, X; Gelmini, G; Gemmeke, H; Ghia, P L; Giaccari, U; Giller, M; Glass, H; Goggin, L M; Gold, M S; Golup, G; Gomez Albarracin, F; Gómez Berisso, M; Gonçalves, P; Gonzalez, D; Gonzalez, J G; Góra, D; Gorgi, A; Gouffon, P; Gozzini, S R; Grashorn, E; Grebe, S; Grigat, M; Grillo, A F; Guardincerri, Y; Guarino, F; Guedes, G P; Hague, J D; Halenka, V; Hansen, P; Harari, D; Harmsma, S; Harton, J L; Haungs, A; Hebbeker, T; Heck, D; Herve, A E; Hojvat, C; Holmes, V C; Homola, P; Hörandel, J R; Horneffer, A; Hrabovský, M; Huege, T; Hussain, M; Iarlori, M; Insolia, A; Ionita, F; Italiano, A; Jiraskova, S; Kadija, K; Kaducak, M; Kampert, K H; Karova, T; Kasper, P; Kégl, B; Keilhauer, B; Keivani, A; Kelley, J; Kemp, E; Kieckhafer, R M; Klages, H O; Kleifges, M; Kleinfeller, J; Knapik, R; Knapp, J; Koang, D-H; Krieger, A; Krömer, O; Kruppke-Hansen, D; Kuehn, F; Kuempel, D; Kulbartz, K; Kunka, N; Kusenko, A; La Rosa, G; Lachaud, C; Lago, B L; Lautridou, P; Leão, M S A B; Lebrun, D; Lebrun, P; Lee, J; Leigui de Oliveira, M A; Lemiere, A; Letessier-Selvon, A; Lhenry-Yvon, I; López, R; Lopez Agüera, A; Louedec, K; Lozano Bahilo, J; Lucero, A; Ludwig, M; Lyberis, H; Maccarone, M C; Macolino, C; Maldera, S; Mandat, D; Mantsch, P; Mariazzi, A G; Marin, V; Maris, I C; Marquez Falcon, H R; Marsella, G; Martello, D; Martínez Bravo, O; Mathes, H J; Matthews, J; Matthews, J A J; Matthiae, G; Maurizio, D; Mazur, P O; McEwen, M; Medina-Tanco, G; Melissas, M; Melo, D; Menichetti, E; Menshikov, A; Meurer, C; Micanović, S; Micheletti, M I; Miller, W; Miramonti, L; Mollerach, S; Monasor, M; Monnier Ragaigne, D; Montanet, F; Morales, B; Morello, C; Moreno, E; Moreno, J C; Morris, C; Mostafá, M; Mueller, S; Muller, M A; Mussa, R; Navarra, G; Navarro, J L; Navas, S; Necesal, P; Nellen, L; Nhung, P T; Nierstenhoefer, N; Nitz, D; Nosek, D; Nozka, L; Nyklicek, M; Oehlschläger, J; Olinto, A; Oliva, P; Olmos-Gilbaja, V M; Ortiz, M; Pacheco, N; Pakk Selmi-Dei, D; Palatka, M; Pallotta, J; Palmieri, N; Parente, G; Parizot, E; Parlati, S; Parra, A; Parrisius, J; Parsons, R D; Pastor, S; Paul, T; Pavlidou, V; Payet, K; Pech, M; Pekala, J; Pelayo, R; Pepe, I M; Perrone, L; Pesce, R; Petermann, E; Petrera, S; Petrinca, P; Petrolini, A; Petrov, Y; Petrovic, J; Pfendner, C; Piegaia, R; Pierog, T; Pimenta, M; Pirronello, V; Platino, M; Ponce, V H; Pontz, M; Privitera, P; Prouza, M; Quel, E J; Rautenberg, J; Ravel, O; Ravignani, D; Redondo, A; Revenu, B; Rezende, F A S; Ridky, J; Riggi, S; Risse, M; Ristori, P; Rivière, C; Rizi, V; Robledo, C; Rodriguez, G; Rodriguez Martino, J; Rodriguez Rojo, J; Rodriguez-Cabo, I; Rodríguez-Frías, M D; Ros, G; Rosado, J; Rossler, T; Roth, M; Rouillé-d'Orfeuil, B; Roulet, E; Rovero, A C; Salamida, F; Salazar, H; Salina, G; Sánchez, F; Santander, M; Santo, C E; Santos, E; Santos, E M; Sarazin, F; Sarkar, S; Sato, R; Scharf, N; Scherini, V; Schieler, H; Schiffer, P; Schmidt, A; Schmidt, F; Schmidt, T; Scholten, O; Schoorlemmer, H; Schovancova, J; Schovánek, P; Schroeder, F; Schulte, S; Schüssler, F; Schuster, D; Sciutto, S J; Scuderi, M; Segreto, A; Semikoz, D; Settimo, M; Shadkam, A; Shellard, R C; Sidelnik, I; Siffert, B B; Sigl, G; Smiałkowski, A; Smída, R; Snow, G R; Sommers, P; Sorokin, J; Spinka, H; Squartini, R; Stasielak, J; Stephan, M; Strazzeri, E; Stutz, A; Suarez, F; Suomijärvi, T; Supanitsky, A D; Susa, T; Sutherland, M S; Swain, J; Szadkowski, Z; Tamashiro, A; Tamburro, A; Tapia, A; Tarutina, T; Taşcău, O; Tcaciuc, R; Tcherniakhovski, D; Tegolo, D; Thao, N T; Thomas, D; Tiffenberg, J; Timmermans, C; Tkaczyk, W; Todero Peixoto, C J; Tomé, B; Tonachini, A; Travnicek, P; Tridapalli, D B; Tristram, G; Trovato, E; Tueros, M; Ulrich, R; Unger, M; Urban, M; Valdés Galicia, J F; Valiño, I; Valore, L; van den Berg, A M; Vázquez, J R; Vázquez, R A; Veberic, D; Venters, T; Verzi, V; Videla, M; Villaseñor, L; Vorobiov, S; Voyvodic, L; Wahlberg, H; Wahrlich, P; Wainberg, O; Warner, D; Watson, A A; Westerhoff, S; Whelan, B J; Wieczorek, G; Wiencke, L; Wilczyńska, B; Wilczyński, H; Williams, C; Winchen, T; Winnick, M G; Wundheiler, B; Yamamoto, T; Younk, P; Yuan, G; Yushkov, A; Zas, E; Zavrtanik, D; Zavrtanik, M; Zaw, I; Zepeda, A; Ziolkowski, M

    2010-03-01

    We describe the measurement of the depth of maximum, X{max}, of the longitudinal development of air showers induced by cosmic rays. Almost 4000 events above 10;{18} eV observed by the fluorescence detector of the Pierre Auger Observatory in coincidence with at least one surface detector station are selected for the analysis. The average shower maximum was found to evolve with energy at a rate of (106{-21}{+35}) g/cm{2}/decade below 10{18.24+/-0.05} eV, and (24+/-3) g/cm{2}/decade above this energy. The measured shower-to-shower fluctuations decrease from about 55 to 26 g/cm{2}. The interpretation of these results in terms of the cosmic ray mass composition is briefly discussed. PMID:20366976

  1. Examination of Lorentz invariance by means of watching of extensive air showers development at super high energies

    International Nuclear Information System (INIS)

    The idea about possible violation of the Lorentz invariance stated by Coleman and Glashow to solve the astrophysics problems of air showers with E > 1020 eV giant energy values may be tested on the basis of the experimental data for these showers. Comparing the calculation results for longitudinal propagation of showers and for distribution of their maximum depths conducted in terms of a model of quark-gluon strings with regard to the Landau-Pomeranchuk-Migdal effect and with regard to interactions of neutral pions under superhigh energy values with the available experimental data one derived new restrictions for possible difference of the speeds of photons and neutral pions |cγ - cπ0| 20 and if one increased the observed depth of shower maximum by the upper evaluation of the error, then |cγ - cπ0| 22

  2. Composition of primary cosmic rays near the bend from a study of hadrons in air showers at sea level

    Science.gov (United States)

    Mincer, A. I.; Freudenreich, H. T.; Goodman, J. A.; Tonwar, S. C.; Yodh, G. B.; Ellsworth, R. W.; Berley, D.

    1985-01-01

    Data on hadrons in air showers arriving at sea level were studied to find sensitivity to primary cosmic ray composition. The rate of showers which satisfy minimum shower density and hadron energy requirements as well as the rate of showers containing hadrons delayed with respect to the electron shower front are compared to Monte Carlo simulations. The data on the rate of total triggers and delayed hadrons are compared to predicted rates for two models of primary composition. The data are consistent with models which require an increasing heavy nuclei fraction near 10 to the 15th power eV. The spectra which are consistent with the observed rate are also compared to the observed shower size spectrum at sea level and mountain level.

  3. Spatial and frequency characteristics of ratio emission caused by interaction of extensive air shower with Earth surface

    International Nuclear Information System (INIS)

    The spatial characteristic of the radioemission direction, caused by interaction of superplus electrons of the extensive air shower with the Earth surface is determined in the approximation of the ideal soil conductivity. The analysis of the obtained results determined the frequency range (∼ 0.2-1 MHz), for which the shower emission by such a irradiation mechanism is at its maximum. Besides, it proved possible to explain the determined earlier absence of direct dependence between the shower energy, and the radiosignal amplitude. Realization of the sharply-direction radiation diagrams within the range of 0.2-3 MHz for a wide interval of the axis inclination is the basic cause of this phenomenon

  4. Reconstruction of the energy and depth of maximum of cosmic-ray air showers from LOPES radio measurements

    Science.gov (United States)

    Apel, W. D.; Arteaga-Velazquez, J. C.; Bähren, L.; Bekk, K.; Bertaina, M.; Biermann, P. L.; Blümer, J.; Bozdog, H.; Brancus, I. M.; Cantoni, E.; Chiavassa, A.; Daumiller, K.; de Souza, V.; di Pierro, F.; Doll, P.; Engel, R.; Falcke, H.; Fuchs, B.; Fuhrmann, D.; Gemmeke, H.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J. R.; Horneffer, A.; Huber, D.; Huege, T.; Isar, P. G.; Kampert, K.-H.; Kang, D.; Krömer, O.; Kuijpers, J.; Link, K.; Łuczak, P.; Ludwig, M.; Mathes, H. J.; Melissas, M.; Morello, C.; Oehlschläger, J.; Palmieri, N.; Pierog, T.; Rautenberg, J.; Rebel, H.; Roth, M.; Rühle, C.; Saftoiu, A.; Schieler, H.; Schmidt, A.; Schröder, F. G.; Sima, O.; Toma, G.; Trinchero, G. C.; Weindl, A.; Wochele, J.; Zabierowski, J.; Zensus, J. A.; Lopes Collaboration

    2014-09-01

    LOPES is a digital radio interferometer located at Karlsruhe Institute of Technology (KIT), Germany, that measures radio emission from extensive air showers at MHz frequencies in coincidence with KASCADE-Grande. In this article, we explore a method (slope method) that leverages the slope of the measured radio lateral distribution to reconstruct crucial attributes of primary cosmic rays. First, we present an investigation of the method on the basis of pure simulations. Second, we directly apply the slope method to LOPES measurements. Applying the slope method to simulations, we obtain uncertainties on the reconstruction of energy and depth of shower maximum (Xmax) of 13% and 50 g /cm2, respectively. Applying it to LOPES measurements, we are able to reconstruct energy and Xmax of individual events with upper limits on the precision of 20%-25% for the primary energy and 95 g /cm2 for Xmax, despite strong human-made noise at the LOPES site.

  5. Reconstruction of the energy and depth of maximum of cosmic-ray air-showers from LOPES radio measurements

    CERN Document Server

    Apel, W D; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Cantoni, E; Chiavassa, A; Daumiller, K; de Souza, V; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Fuchs, B; Fuhrmann, D; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Łuczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmidt, A; Schröder, F G; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Zabierowski, J; Zensus, J A

    2014-01-01

    LOPES is a digital radio interferometer located at Karlsruhe Institute of Technology (KIT), Germany, which measures radio emission from extensive air showers at MHz frequencies in coincidence with KASCADE-Grande. In this article, we explore a method (slope method) which leverages the slope of the measured radio lateral distribution to reconstruct crucial attributes of primary cosmic rays. First, we present an investigation of the method on the basis of pure simulations. Second, we directly apply the slope method to LOPES measurements. Applying the slope method to simulations, we obtain uncertainties on the reconstruction of energy and depth of shower maximum Xmax of 13% and 50 g/cm^2, respectively. Applying it to LOPES measurements, we are able to reconstruct energy and Xmax of individual events with upper limits on the precision of 20-25% for the primary energy and 95 g/cm^2 for Xmax, despite strong human-made noise at the LOPES site.

  6. Anomalous time structure of extensive air shower particle flows in the knee region of primary cosmic ray spectrum

    International Nuclear Information System (INIS)

    We observe the new phenomenon of anomalous prolonged time distributions of neutron intensity using the 18NM64-type neutron monitor operating together with the shower installation of the Tian-Shan mountain cosmic ray station. We observe anomalous events in the core region of extensive air showers (EAS) with the size Ne>106. The threshold of their generation coincides with the 'knee' in the energy spectrum of primary cosmic rays (about 3x1015 eV). The prolonged neutron events are accompanied by the flows of EAS electrons and γ-quanta having time distributions similar to those of the neutrons. The discovered phenomenon may be a reason to make a principal change in the usual procedure of EAS exploration. (author)

  7. Cosmic ray air shower characteristics in the framework of the parton-based Gribov-Regge model nexus

    Energy Technology Data Exchange (ETDEWEB)

    Bossard, G.; Drescher, H.J.; Ostapchenko, S.; Pierog, T.; Werner, K. [SUBATECH, Nantes Univ., IN2P3/CNRS, Ecole des Mines, 44 (France); Kalmykov, N.N.; Pavlov, A.I.; Vishnevskaya, E.A. [Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow (Russian Federation)

    2000-08-01

    The purpose of this paper is twofold: first we want to introduce a new type of hadronic interaction model (NEXUS), which has a much more solid theoretical basis as, for example, presently used models like QGSJET and VENUS, and ensures therefore a much more reliable extrapolation towards high energies. Secondly, we want to promote an extensive air shower (EAS) calcination scheme, based on cascade equations rather than explicit Monte Carlo simulations, which is very accurate in calcination of main EAS characteristics and extremely fast concerning computing time. We employ the NEXUS model to provide the necessary data on particle production in hadron-air collisions and present the average EAS characteristics for energies 10{sup 14} - 10{sup 17} eV. The experimental data of the CASA-BLANKA group are analyzed in the framework of the new model. (authors)

  8. Study of Cherenkov Light Lateral Distribution Function around the Knee Region in Extensive Air Showers

    CERN Document Server

    Al-Rubaiee, A A; M., Marwah; Al-Douri, Y

    2015-01-01

    The Cherenkov light lateral distribution function (LDF) was simulated with the CORSIKA code, in the energy range (10^13-10^16) eV. This simulation was performed for conditions and configurations of the Tunka EAS Cherenkov array for two primary particles (p and Fe). Basing on the simulated results, many approximated functions are structured for two primary particles and different zenith angles. This allowed us to reconstruct the EAS events, which is, to determine the type and energy of the primary particles that produced showers from signal amplitudes of Cherenkov radiation which measured with Tunka Cherenkov array experiment. Comparison of the calculated LDF of Cherenkov radiation with that measured at the Tunka EAS array shows the ability for identifying of the primary particle that initiated the EAS cascades determining of its primary energy around the knee region of the cosmic ray spectrum.

  9. Reconstruction of extensive air showers and measurement of the cosmic ray energy spectrum in the range of 1 - 80 PeV at the South Pole

    Energy Technology Data Exchange (ETDEWEB)

    Klepser, Stefan

    2008-06-24

    IceTop is a km{sup 2} scale detector array for highly energetic cosmic radiation. It is a part of the IceCube Observatory that is presently being built at the geographic South Pole. It aims for the detection of huge particle cascades induced by PeV cosmic rays in the atmosphere. These extensive air showers are detected by cylindrical ice tanks that collect the Cherenkov light produced by penetrating particles. The main goal of IceTop is the investigation of the energy distribution and chemical composition of PeV to EeV cosmic rays. This thesis presents the first analysis of highly energetic cosmic ray data taken with IceTop. First, the light response of the IceTop tanks is parametrised as a function of energy and particle type. An expectation function for the distribution of shower signals in the detector plane is developed. The likelihood fit based on that can reconstruct the recorded shower events with resolutions of 1.5 in direction, 9m in location of the shower center, and 12% in energy. This is well competitive with other experiments. The resulting energy response of the array is studied to set up response matrices for different primary nuclei and inclinations. These allow for a deconvolution of the distribution of reconstructed energies to derive the real energy spectrum. Two unfolding algorithms are implemented and studied, and response matrices are modeled for four different composition assumptions. With each assumption, energy spectra are unfolded for three different bins in inclination, using a data sample with an exposure of 3.86.10{sup 11} m{sup 2} s sr, taken in August 2007. The range of the spectrum is 1-80 PeV. Finally, a new analysis method is developed that uses the fact that cosmic rays in the PeV range are expected to be isotropic. It is shown that this requirement can be used for a likelihood estimation that is sensitive to composition without using additional information from other detector components. The analysis shows a clear preference of

  10. Reconstruction of extensive air showers and measurement of the cosmic ray energy spectrum in the range of 1 - 80 PeV at the South Pole

    International Nuclear Information System (INIS)

    IceTop is a km2 scale detector array for highly energetic cosmic radiation. It is a part of the IceCube Observatory that is presently being built at the geographic South Pole. It aims for the detection of huge particle cascades induced by PeV cosmic rays in the atmosphere. These extensive air showers are detected by cylindrical ice tanks that collect the Cherenkov light produced by penetrating particles. The main goal of IceTop is the investigation of the energy distribution and chemical composition of PeV to EeV cosmic rays. This thesis presents the first analysis of highly energetic cosmic ray data taken with IceTop. First, the light response of the IceTop tanks is parametrised as a function of energy and particle type. An expectation function for the distribution of shower signals in the detector plane is developed. The likelihood fit based on that can reconstruct the recorded shower events with resolutions of 1.5 in direction, 9m in location of the shower center, and 12% in energy. This is well competitive with other experiments. The resulting energy response of the array is studied to set up response matrices for different primary nuclei and inclinations. These allow for a deconvolution of the distribution of reconstructed energies to derive the real energy spectrum. Two unfolding algorithms are implemented and studied, and response matrices are modeled for four different composition assumptions. With each assumption, energy spectra are unfolded for three different bins in inclination, using a data sample with an exposure of 3.86.1011 m2 s sr, taken in August 2007. The range of the spectrum is 1-80 PeV. Finally, a new analysis method is developed that uses the fact that cosmic rays in the PeV range are expected to be isotropic. It is shown that this requirement can be used for a likelihood estimation that is sensitive to composition without using additional information from other detector components. The analysis shows a clear preference of the mixed

  11. Anisotropy of the arrival direction of extensive air showers observed at Akeno

    International Nuclear Information System (INIS)

    The anisotropy of the arrival direction of the primary cosmic ray of energy 1015 to 1018 eV is studied using approximately 300 000 showers observed in 1981 and 1982 at the EAS array at Akeno. The anisotropy of the second harmonics appears to be (1.1=-0.4)% in the region 1016 to 1017 eV. The showers with rich muon content seem to come preferentially from a direction of about 2300 in the right ascension. No statistically meaningful anisotropy is found for muon-poor showers. (author)

  12. Atmospheric multiple scattering of fluorescence light from extensive air showers and effect of the aerosol size on the reconstruction of energy and depth of maximum

    CERN Document Server

    Louedec, K

    2013-01-01

    The reconstruction of the energy and the depth of maximum Xmax of an extensive air shower depends on the multiple scattering of fluorescence photons in the atmosphere. In this work, we explain how atmospheric aerosols, and especially their size, scatter the fluorescence photons during their propagation. Using a Monte Carlo simulation for the scattering of light, the dependence on the aerosol conditions of the multiple scattered light contribution to the recorded signal is fully parameterised. A clear dependence on the aerosol size is proposed for the first time. Finally, using this new parameterisation, the effect of atmospheric aerosols on the energy and on the Xmax reconstructions is presented for a typical extensive air shower observed by a ground-based detector: a systematic over-estimation of these two quantities is observed if aerosols of large size are neglected in the estimation of the multiple scattered fraction.

  13. Lateral distribution of Cherenkov light in extensive air showers at high mountain altitude produced by different primary particles in wide energy range

    CERN Document Server

    Mishev, A

    2005-01-01

    The general aim of this work is to obtain the lateral distribution of atmospheric Cherenkov light in extensive air showers produced by different primary particles precisely by. protons, Helium, Iron, Oxygen, Carbon, Nitrogen, Calcium, Silicon and gamma quanta in wide energy range at high mountain observation level of Chacaltaya cosmic ray station. The simulations are divided generally in two energy ranges 10GeV-10 TeV and 10 TeV-10 PeV. One large detector has been used for simulations, the aim being to reduce the statistical fluctuations of the obtained characteristics. The shape of the obtained lateral distributions of Cherenkov light in extensive air showers is discussed and the scientific potential for solution of different problems as well.

  14. ALTAI: computational code for the simulations of TeV air showers as observed with the ground-based imaging atmospheric Cherenkov telescopes

    International Nuclear Information System (INIS)

    Ground-based atmospheric Cherenkov telescopes are proven to be effective instruments for observations of very high-energy (VHE) γ-radiation from celestial objects. For effective use of such technique one needs detailed Monte Carlo simulations of γ-ray- and proton/nuclei-induced air showers in the Earth atmosphere. Here we discuss in detail the algorithms used in the numerical code ALTAI developed particularly for the simulations of Cherenkov light emission from air showers of energy below 50 TeV. The specific scheme of sampling the charged particle transport in the atmosphere allows the performance of very fast and accurate simulations used for interpretation of the VHE γ-ray observations

  15. Depth of maximum of extensive air showers and cosmic ray composition above 1017eV in the geometrical multichain model of nuclei interactions

    International Nuclear Information System (INIS)

    The depth of maximum for extensive air showers measured by Fly's Eye and Yakutsk experiments is analysed. The analysis depends on the hadronic interaction model that determines cascade development. The novel feature found in the cascading process for nucleus-nucleus collisions at high energies leads to a fast increase of the inelasticity in heavy nuclei interactions without changing the hadron-hadron interaction properties. This effects the development of the extensive air showers initiated by heavy primaries. The detailed calculations were performed using the recently developed geometrical multichain model and the CORSIKA simulation code. The agreement with data on average depth of shower maxima, the falling slope of the maxima distribution, and these distribution widths are found for the very heavy cosmic ray mass spectrum (slightly heavier than expected in the diffusion model at about 3x1017eV and similar to the Fly's Eye composition at this energy). (author)

  16. Measurement of the Radiation Energy in the Radio Signal of Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy

    CERN Document Server

    Aab, Alexander; Aglietta, Marco; Ahn, Eun-Joo; Samarai, Imen Al; Albuquerque, Ivone; Allekotte, Ingomar; Allison, Patrick; Almela, Alejandro; Castillo, Jesus Alvarez; Alvarez-Muñiz, Jaime; Batista, Rafael Alves; Ambrosio, Michelangelo; Aminaei, Amin; Anastasi, Gioacchino Alex; Anchordoqui, Luis; Andringa, Sofia; Aramo, Carla; Arqueros, Fernando; Arsene, Nicusor; Asorey, Hernán Gonzalo; Assis, Pedro; Aublin, Julien; Avila, Gualberto; Awal, Nafiun; Badescu, Alina Mihaela; Baus, Colin; Beatty, Jim; Becker, Karl Heinz; Bellido, Jose A; Berat, Corinne; Bertaina, Mario Edoardo; Bertou, Xavier; Biermann, Peter; Billoir, Pierre; Blaess, Simon G; Blanco, Alberto; Blanco, Miguel; Blazek, Jiri; Bleve, Carla; Blümer, Hans; Boháčová, Martina; Boncioli, Denise; Bonifazi, Carla; Borodai, Nataliia; Brack, Jeffrey; Brancus, Iliana; Bretz, Thomas; Bridgeman, Ariel; Brogueira, Pedro; Buchholz, Peter; Bueno, Antonio; Buitink, Stijn; Buscemi, Mario; Caballero-Mora, Karen S; Caccianiga, Barbara; Caccianiga, Lorenzo; Candusso, Marina; Caramete, Laurentiu; Caruso, Rossella; Castellina, Antonella; Cataldi, Gabriella; Cazon, Lorenzo; Cester, Rosanna; Chavez, Alan G; Chiavassa, Andrea; Chinellato, Jose Augusto; Chudoba, Jiri; Cilmo, Marco; Clay, Roger W; Cocciolo, Giuseppe; Colalillo, Roberta; Coleman, Alan; Collica, Laura; Coluccia, Maria Rita; Conceição, Ruben; Contreras, Fernando; Cooper, Mathew J; Cordier, Alain; Coutu, Stephane; Covault, Corbin; Cronin, James; Dallier, Richard; Daniel, Bruno; Dasso, Sergio; Daumiller, Kai; Dawson, Bruce R; de Almeida, Rogerio M; de Jong, Sijbrand J; De Mauro, Giuseppe; Neto, Joao de Mello; De Mitri, Ivan; de Oliveira, Jaime; de Souza, Vitor; del Peral, Luis; Deligny, Olivier; Dhital, Niraj; Di Giulio, Claudio; Di Matteo, Armando; Diaz, Johana Chirinos; Castro, Mary Lucia Díaz; Diogo, Francisco; Dobrigkeit, Carola; Docters, Wendy; D'Olivo, Juan Carlos; Dorofeev, Alexei; Hasankiadeh, Qader Dorosti; Anjos, Rita dos; Dova, Maria Teresa; Ebr, Jan; Engel, Ralph; Erdmann, Martin; Erfani, Mona; Escobar, Carlos O; Espadanal, Joao; Etchegoyen, Alberto; Falcke, Heino; Fang, Ke; Farrar, Glennys; Fauth, Anderson; Fazzini, Norberto; Ferguson, Andrew P; Fick, Brian; Figueira, Juan Manuel; Filevich, Alberto; Filipčič, Andrej; Fratu, Octavian; Freire, Martín Miguel; Fujii, Toshihiro; García, Beatriz; Garcia-Gamez, Diego; Garcia-Pinto, Diego; Gate, Florian; Gemmeke, Hartmut; Gherghel-Lascu, Alexandru; Ghia, Piera Luisa; Giaccari, Ugo; Giammarchi, Marco; Giller, Maria; Głas, Dariusz; Glaser, Christian; Glass, Henry; Golup, Geraldina; Berisso, Mariano Gómez; Vitale, Primo F Gómez; González, Nicolás; Gookin, Ben; Gordon, Jacob; Gorgi, Alessio; Gorham, Peter; Gouffon, Philippe; Griffith, Nathan; Grillo, Aurelio; Grubb, Trent D; Guarino, Fausto; Guedes, Germano; Hampel, Matías Rolf; Hansen, Patricia; Harari, Diego; Harrison, Thomas A; Hartmann, Sebastian; Harton, John; Haungs, Andreas; Hebbeker, Thomas; Heck, Dieter; Heimann, Philipp; Herve, Alexander E; Hill, Gary C; Hojvat, Carlos; Hollon, Nicholas; Holt, Ewa; Homola, Piotr; Hörandel, Jörg; Horvath, Pavel; Hrabovský, Miroslav; Huber, Daniel; Huege, Tim; Insolia, Antonio; Isar, Paula Gina; Jandt, Ingolf; Jansen, Stefan; Jarne, Cecilia; Johnsen, Jeffrey A; Josebachuili, Mariela; Kääpä, Alex; Kambeitz, Olga; Kampert, Karl Heinz; Kasper, Peter; Katkov, Igor; Keilhauer, Bianca; Kemp, Ernesto; Kieckhafer, Roger; Klages, Hans; Kleifges, Matthias; Kleinfeller, Jonny; Krause, Raphael; Krohm, Nicole; Kuempel, Daniel; Mezek, Gasper Kukec; Kunka, Norbert; Awad, Alaa Metwaly Kuotb; LaHurd, Danielle; Latronico, Luca; Lauer, Robert; Lauscher, Markus; Lautridou, Pascal; Coz, Sandra Le; Lebrun, Didier; Lebrun, Paul; de Oliveira, Marcelo Augusto Leigui; Letessier-Selvon, Antoine; Lhenry-Yvon, Isabelle; Link, Katrin; Lopes, Luis; López, Rebeca; Casado, Aida López; Louedec, Karim; Lucero, Agustin; Malacari, Max; Mallamaci, Manuela; Maller, Jennifer; Mandat, Dusan; Mantsch, Paul; Mariazzi, Analisa; Marin, Vincent; Mariş, Ioana; Marsella, Giovanni; Martello, Daniele; Martinez, Humberto; Bravo, Oscar Martínez; Martraire, Diane; Meza, Jimmy Masías; Mathes, Hermann-Josef; Mathys, Sebastian; Matthews, James; Matthews, John; Matthiae, Giorgio; Maurizio, Daniela; Mayotte, Eric; Mazur, Peter; Medina, Carlos; Medina-Tanco, Gustavo; Meissner, Rebecca; Mello, Victor; Melo, Diego; Menshikov, Alexander; Messina, Stefano; Micheletti, Maria Isabel; Middendorf, Lukas; Minaya, Ignacio A; Miramonti, Lino; Mitrica, Bogdan; Molina-Bueno, Laura; Mollerach, Silvia; Montanet, François

    2016-01-01

    We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 \\pm 0.7 (stat) \\pm 6.7 (sys) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cosmic-ray energy. A comparison with predictions from state-of-the-art first-principle calculations shows agreement with our measurement. The radiation energy provides direct access to the calorimetric energy in the electromagnetic cascade of extensive air showers. Comparison with our result thus allows the direct calibration of any cosmic-ray radio detector against the well-established energy scale of the Pierre Auger Observatory.

  17. Results from hadroproduction in p+C collisions at the CERN SPS for understanding of extensive air showers

    International Nuclear Information System (INIS)

    Analysing extensive air showers resulting from interaction of cosmic particles with the Earth's atmosphere is a major experimental technique of studying high-energy cosmic rays, whose cross-sections are too low for efficient direct detection. Unfortunately, the modeling of many important observables of such showers strongly depends on the applied model of low-energy hadronic interactions, with significant differences between them. It has been shown that many constraints to be applied to these models can be obtained by studying identified-particle spectra from accelerator collisions - in particular at the CERN Super Proton Synchrotron, whose energy range matches well that of final hadroproduction in high-energy EAS observed by such experiments as KASCADE, KASCADE-Grande and Pierre Auger Observatory. Here we present soon-to-be-published measurements of the pion production cross-section obtained by the NA61/SHINE experiment at the SPS, in proton-carbon collisions at the beam energy of 31 GeV from the year 2007. Further analyses of identified-particle yields in SHINE, in particular with a pion beam, are in preparation.

  18. Analysis of the space-time microstructure of cosmic ray air showers using the HADES RPC TOF wall

    International Nuclear Information System (INIS)

    Cosmic rays have been studied, since they were discovered one century ago, with a very broad spectrum of detectors and techniques. However, never the properties of the extended air showers (EAS) induced by high energy primary cosmic rays had been analysed at the Earth surface with a high granularity detector and a time resolution at the 0.1 ns scale. The commissioning of the timing RPC (Resistive Plate Chambers) time of flight wall of the HADES spectrometer with cosmic rays, at the GSI (Darmstadt, Germany), opened up that opportunity. During the last months of 2009, more than 500 millions of cosmic ray events were recorded by a stack of two RPC modules, of about 1.25 m2 each, able to measure swarms of up to ∼ 100 particles with a time resolution better than 100 ps. In this document it is demonstrated how such a relative small two-plane, high-granularity timing RPC setup may provide significant information about the properties of the shower and hence about the primary cosmic ray properties.

  19. Simulation studies of the information content of muon arrival time observations of high energy extensive air showers

    International Nuclear Information System (INIS)

    By extensive Monte Carlo calculations, using the air shower simulation code CORSIKA, EAS muon arrival time distributions and EAS time profiles up to 320 m distances from the shower centre have been generated, for proton, oxygen and iron induced showers using different hadronic interaction models as Monte Carlo generators. The model dependence and mass discriminating features have been scrutinized for three energy ranges, (1-1.7783) 1015 eV, (1.-1.78) 1016 eV and (1.78-3.16) 1016 eV, by use of non-parametric statistical inference method applied to multidimensional distributions, correlating the EAS time quantities with different other EAS observables. The correlations of local muon arrival times with the local muon density and the shower age indicate a good mass separation quality at larger shower distances. The best discrimination was obtained by adding the correlation with Nμtr quantity. The comparison between 'local times', with reference to the first registered muon and 'global times' with reference to the arrival time of the shower core, indicates a slightly better mass discrimination in the case of muon 'global' time distributions. (authors)

  20. Use of small extensive air showers with Nsub(e) >= 104 at mountains for the calibration of an interaction model

    International Nuclear Information System (INIS)

    A possibility of the usage of small extensive air showers (EAS) with a number of electrons of Nsub(e) >= 104. On mountains for the interaction model calibration is discussed. Calculations are carried out within the 4x1012-1.5x1015 eV energy range for two models: the model with scaling retain in the fragmentation region and the model with scaling violation. Spatial distributions of charged particle flux density and energy flux of the EAS electron-phonon component on the mountain level are presented. These characteristics were calculated for two mentioned models and two groups of showers with a mean density of rho=5-10 m-2 and 56-100 m-2. Both models give almost the same result. Presented theoretical data on spatial distributions of electrons and also of muons and hadrons satisfactorily describe experimental results. A conclusion is drawn that small EAS with Nsub(e) >= 104 may be used on mountains for the interaction model calibration

  1. Numerical simulations of compact intracloud discharges as the Relativistic Runaway Electron Avalanche-Extensive Air Shower process

    Science.gov (United States)

    Arabshahi, S.; Dwyer, J. R.; Nag, A.; Rakov, V. A.; Rassoul, H. K.

    2014-01-01

    Compact intracloud discharges (CIDs) are sources of the powerful, often isolated radio pulses emitted by thunderstorms. The VLF-LF radio pulses are called narrow bipolar pulses (NBPs). It is still not clear how CIDs are produced, but two categories of theoretical models that have previously been considered are the Transmission Line (TL) model and the Relativistic Runaway Electron Avalanche-Extensive Air Showers (RREA-EAS) model. In this paper, we perform numerical calculations of RREA-EASs for various electric field configurations inside thunderstorms. The results of these calculations are compared to results from the other models and to the experimental data. Our analysis shows that different theoretical models predict different fundamental characteristics for CIDs. Therefore, many previously published properties of CIDs are highly model dependent. This is because of the fact that measurements of the radiation field usually provide information about the current moment of the source, and different physical models with different discharge currents could have the same current moment. We have also found that although the RREA-EAS model could explain the current moments of CIDs, the required electric fields in the thundercloud are rather large and may not be realistic. Furthermore, the production of NBPs from RREA-EAS requires very energetic primary cosmic ray particles, not observed in nature. If such ultrahigh-energy particles were responsible for NBPs, then they should be far less frequent than is actually observed.

  2. Investigation of the radio wavefront of air showers with LOPES measurements and CoREAS simulations (ARENA 2014)

    CERN Document Server

    Schröder, F G; Arteaga-Velazquez, J C; Bähren, L; Bekk, K; Bertaina, M; Biermann, P L; Blümer, J; Bozdog, H; Brancus, I M; Cantoni, E; Chiavassa, A; Daumiller, K; de Souza, V; Di Pierro, F; Doll, P; Engel, R; Falcke, H; Fuchs, B; Fuhrmann, D; Gemmeke, H; Grupen, C; Haungs, A; Heck, D; Hörandel, J R; Horneffer, A; Huber, D; Huege, T; Isar, P G; Kampert, K -H; Kang, D; Krömer, O; Kuijpers, J; Link, K; Luczak, P; Ludwig, M; Mathes, H J; Melissas, M; Morello, C; Oehlschläger, J; Palmieri, N; Pierog, T; Rautenberg, J; Rebel, H; Roth, M; Rühle, C; Saftoiu, A; Schieler, H; Schmidt, A; Schoo, S; Sima, O; Toma, G; Trinchero, G C; Weindl, A; Wochele, J; Zabierowski, J; Zensus, J A

    2015-01-01

    We investigated the radio wavefront of cosmic-ray air showers with LOPES measurements and CoREAS simulations: the wavefront is of approximately hyperbolic shape and its steepness is sensitive to the shower maximum. For this study we used 316 events with an energy above 0.1 EeV and zenith angles below $45^\\circ$ measured by the LOPES experiment. LOPES was a digital radio interferometer consisting of up to 30 antennas on an area of approximately 200 m x 200 m at an altitude of 110 m above sea level. Triggered by KASCADE-Grande, LOPES measured the radio emission between 43 and 74 MHz, and our analysis might strictly hold only for such conditions. Moreover, we used CoREAS simulations made for each event, which show much clearer results than the measurements suffering from high background. A detailed description of our result is available in our recent paper published in JCAP09(2014)025. The present proceeding contains a summary and focuses on some additional aspects, e.g., the asymmetry of the wavefront: Accordin...

  3. Angular deviation of secondary charge particles in 1014-1016 eV extensive air showers: Constrains on application of hodoscopes

    Directory of Open Access Journals (Sweden)

    D Purmohammad

    2012-12-01

    Full Text Available   Deviation angles of secondary electrons and muons in simulated extensive air showers were studied. The angles have wide distribution, whose width depends on energy cuts imposed on shower particles. In this work, variation of deviation angles with the energy of secondary particles, shower energy, primary direction, and core distance was investigated. The results put limitations on application of hodoscopic devices in cosmic ray and gamma ray observations.

  4. The longitudinal development of muons in cosmic ray air showers at energies 10(15) - 10(17) eV

    Science.gov (United States)

    1985-01-01

    The relationship between longitudinal development of muons and conventional equi-intensity cuts is carefully investigated. The development of muons in Extensive Air Showers (EAS) has been calculated using simulation with a scaling violation model at the highest energies and mixed primary composition. Profiles of equi-intensity cuts expected at observation altitudes of 550, 690 and 930/sq cm can fit the observed data very well.

  5. Cosmic ray composition between 10 to the 15th power - 10 to the 17th power eV obtained by air shower experiments

    Science.gov (United States)

    Muraki, Y.

    1985-01-01

    Based on the air shower data, the chemical composition of the primary cosmic rays in the energy range 10 to the 15th power - 10 to the 17th power eV was obtained. The method is based on a well known N sub e-N sub mu and N sub e-N sub gamma. The simulation is calibrated by the CERN SPS pp collider results.

  6. Possibility of Using a Satellite-Based Detector for Recording Cherenkov Light from Ultrahigh-Energy Extensive Air Showers Penetrating into the Ocean Water

    CERN Document Server

    Shustova, O P; Khrenov, B A

    2011-01-01

    We have estimated the reflected component of Cherenkov radiation, which arises in developing of an extensive air shower with primary energy of 10^20 eV over the ocean surface. It has been shown that, under conditions of the TUS experiment, a flash of the reflected Cherenkov photons at the end of the fluorescence track can be identified in showers with zenith angles up to 20 degrees.

  7. Reconstruction of air shower muon densities using segmented counters with time resolution

    CERN Document Server

    Ravignani, D; Melo, D

    2016-01-01

    Despite the significant experimental effort made in the last decades, the origin of the ultra-high energy cosmic rays is still largely unknown. Key astrophysical information to identify where these energetic particles come from is provided by their chemical composition. It is well known that a very sensitive tracer of the primary particle type is the muon content of the showers generated by the interaction of the cosmic rays with air molecules. We introduce a likelihood function to reconstruct particle densities using segmented detectors with time resolution. As an example of this general method, we fit the muon distribution at ground level using an array of counters like AMIGA, one of the Pierre Auger Observatory detectors. For this particular case we compare the reconstruction performance against a previous method. With the new technique, more events can be reconstructed than before. In addition the statistical uncertainty of the measured number of muons is reduced, allowing for a better discrimination of t...

  8. The relation between the lateral profile of giant extensive air showers and the age parameter

    Science.gov (United States)

    Capdevielle, Jean-Noël; Cohen, Fabrice

    2005-05-01

    After performing extensive simulations with the code CoRSiKa, we have obtained an analytical description fitting with surprising accuracy the numerical densities up to distances larger than 5 km from the shower axis. This was achieved by using the hypergeometric formalism in place of the traditional NKG approach. The difficulty of cascade theory (validity limited to 3.5 Moliere radii), underlined with reason by the particle data group, is solved here, after overcoming the constraints of approximation B, to show that the distribution of lateral profiles at large distances is also correlated with the age parameter. This is an important step for a coherent interpretation of hybrid events recorded with both surface array and fluorescence telescopes, even with other information coming from Cerenkov or radio emission. A set of hypergeometric Gaussian functions, with a consistent relation between age parameter and total size, is proposed in the ultra-high-energy range (above 1 EeV) for electrons, muons and vertical equivalent muons.

  9. Reconstruction of air shower muon densities using segmented counters with time resolution

    Science.gov (United States)

    Ravignani, D.; Supanitsky, A. D.; Melo, D.

    2016-09-01

    Despite the significant experimental effort made in the last decades, the origin of the ultra-high energy cosmic rays is still largely unknown. Key astrophysical information to identify where these energetic particles come from is provided by their chemical composition. It is well known that a very sensitive tracer of the primary particle type is the muon content of the showers generated by the interaction of the cosmic rays with air molecules. We introduce a likelihood function to reconstruct particle densities using segmented detectors with time resolution. As an example of this general method, we fit the muon distribution at ground level using an array of counters like AMIGA, one of the Pierre Auger Observatory detectors. For this particular case we compare the reconstruction performance against a previous method. With the new technique, more events can be reconstructed than before. In addition the statistical uncertainty of the measured number of muons is reduced, allowing for a better discrimination of the cosmic ray primary mass.

  10. Stereo-scopy of γ-ray air showers with the H.E.S.S. telescopes: first images of the supernova remnants at TeV

    International Nuclear Information System (INIS)

    The H.E.S.S. (High Energy Stereoscopic System) experiment in gamma-ray Astronomy consists of four imaging atmospheric Cherenkov telescopes devoted to the observation of the gamma-ray sky in the energy domain above 100 GeV and extending up to several tens of TeV. This thesis presents a new reconstruction method of gamma-ray induced air showers which takes full advantage of the stereo-scopy and of the fine-grain imaging of the H.E.S.S. cameras. This new method provides an angular resolution better than 0.1 angle, an energy resolution of about 15% at zenith and a very efficient hadronic rejection based on a cut on the lateral spread of the electromagnetic shower which does not depend on simulations. A new background subtraction method, well adapted to the study of extended sources, was also developed. No assumption, either on the distribution of gamma-rays in the field of view, or on the distribution of hadrons are necessary. It provides two sky maps obtained from a maximum likelihood fit: one for γ-rays and the other for hadrons. These two analysis methods were applied to the study of the shell-type supernova remnants RX J1713.7-3946 and RX J0852.0-4622 (Vela Junior), allowing for the first time to resolve their morphology in the gamma-ray domain. The study of these sources should answer the question: 'can shell-type supernova remnants accelerate cosmic-rays up to the knee (5 x 1015 eV)?'. A morphological and spectral study of these sources combined with a comparison of a simple model of emission processes (from electrons and protons accelerated in supernova remnants) provides some constraints on the parameters of the leptonic process. Nevertheless, this scenario cannot be excluded. The different results obtained are discussed and compared with a third shell-type supernova remnant observed by H.E.S.S. but not detected: SN 1006. (author)

  11. Energy spectrum of primary cosmic rays from 1016eV to 1019eV determined from air showers observed at 5200 m a.s.l

    International Nuclear Information System (INIS)

    Energy spectra of primary cosmic rays from 1016eV to 1019eV have been determined from electron-sizes as well as from muon-sizes of the same air showers observed at Mt. Chacaltaya. The spectrum from electron-sizes is significantly higher than that from muon-sizes. The discrepancy is discussed and an explanation is given under the assumption of possible existence of copious direct production of photons besides the production of charged and neutral pions at these high energies. The spectra are also compared with those by other groups and the discrepancies are discussed. (author)

  12. Experimental data on high-energy muons in extensive air shower composition and primary cosmic ray nuclear composition in the 106-107 GeV

    International Nuclear Information System (INIS)

    Problem, related to the primary cosmic ray nuclear composition within 106-107 GeV energy range is discussed. Kajdalov and Ter-Martirosyan quark-gluon string model is taken as hadron-air nucleus interaction model. Spatial distribution of muons with threshold energy E=100 Ga in extensive air showers with the particle number Ne=105 and 106 are presented. To correlate calculation and experimental data both at Ne=105 and Ne=106 an assumption is made that the nuclear composition changes with the increase of primary energy E0 in the direction of its charging in the investigated energy range

  13. Simulation of a microwave antenna with extended field of view for the detection of molecular Bremsstrahlung emitted by extensive air showers

    International Nuclear Information System (INIS)

    Full text: The MIDAS (Microwave Detection of Air Showers) Collaboration is an R and D effort for the detection of Extensive Air Showers in the frequency range of microwaves. It is believed that a large amount of the atmospheric cascade energy is released in the form of electromagnetic radiation in the radio/microwave domain, due to the continuous energy loss by electrons as they collide with atmospheric neutral nitrogen (and less frequently oxygen) molecules. An apparatus developed at the University of Chicago has been constructed in order to test the feasibility of the technique. It contains a parabolic reflector illuminating a multi-pixel camera of commercial TV satellite C-band (3.4-4.2 GHz) feeds. We describe here the simulation pipe (written in C++) developed at the Universidade Federal do Rio de Janeiro (UFRJ) of the experimental apparatus mentioned. The angular resolution, directional response and frequency dependency of the main detector signals are simulated and compared with absolute calibration data performed with standard radio sources, such as the Sun, the Moon and the Crab Nebula, as well as relative calibration with a reference emitting antenna. Finally, optimization studies for the experimental apparatus were performed, such as determining the best reflectors size and focal length, operation frequency and several other parameters of the detector. (author)

  14. Combined Approach for Nonuniformity Correction in Infrared Focal Plane Array

    Institute of Scientific and Technical Information of China (English)

    XUE Hui

    2009-01-01

    A new algorithm of nonuniformity correction for infrared focal plane array(IRFPA) is reported,which is a combined algorithm based on both the two-point correction and artificial neural networks correction.The combined algorithm is calibrated by two-point correction,and the calibrated correction coefficients are automatically modified by BP algorithm.So it is not only calibrated,but also real-time processed.In adaptive nonuniformity correction algorithm,the phenomena ghost artifact and target fade-out are avoided by edge extraction.In order to get intensified image,the modified median filters are adopted.The simulated data indicates the proposed scheme is an effective algorithm.

  15. Cascaded injection resonator for coherent beam combining of laser arrays

    Science.gov (United States)

    Kireev, Vassili [Sunnyvale, CA; Liu, Yun; Protopopescu, Vladimir [Knoxville, TN; Braiman, Yehuda [Oak Ridge, TN

    2008-10-21

    The invention provides a cascaded injection resonator for coherent beam combining of laser arrays. The resonator comprises a plurality of laser emitters arranged along at least one plane and a beam sampler for reflecting at least a portion of each laser beam that impinges on the beam sampler, the portion of each laser beam from one of the laser emitters being reflected back to another one of the laser emitters to cause a beam to be generated from the other one of the laser emitters to the beam reflector. The beam sampler also transmits a portion of each laser beam to produce a laser output beam such that a plurality of laser output beams of the same frequency are produced. An injection laser beam is directed to a first laser emitter to begin a process of generating and reflecting a laser beam from one laser emitter to another laser emitter in the plurality. A method of practicing the invention is also disclosed.

  16. An upper limit of muon flux of energies above 100 TeV determined from horizontal air showers observed at Akeno

    Science.gov (United States)

    Nagano, M.; Yoshii, H.; Hara, T.; Kamata, K.; Kawaguchi, S.; Kifune, T.

    1985-01-01

    Muon energy spectrum above 100 TeV was determined by observing the extensive air showers (EAS) from the horizontal direction (HAS). No definite muon originated shower of sizes above 100,000 and zenith angles above 60 deg was observed. The upper limits of HAS intensity is 5x10/12 m/2 s/1 sn/1 above 100,000. It is indicated that the upper limit of muon flux above 100 TeV is about 1.3x10/8 m/2 s/1 sr/1 and is in agreement with that expected from the primary spectrum with a knee assuming scaling in the fragmentation region and 40% protons in the primary beam. The critical energy at which muon flux from prompt processes take over that from the conventional process is higher than 100 Tev at horizontal direction.

  17. The new Tunka-133 EAS Cherenkov array: Status of 2009

    International Nuclear Information System (INIS)

    The deployment of the new Extensive air shower Cherenkov installation Tunka-133 with about 1 km2 geometric acceptance area was completed in October 2009. The array will permit a detailed long-term study of the cosmic ray energy spectrum and mass composition in the energy range 1015-1018 eV with a unique and more elaborate method. The array construction and data acquisition system, preliminary results and plans for future development are presented.

  18. Future Plans of Telescope Array

    International Nuclear Information System (INIS)

    The Telescope Array (TA) experiment is the only ultra high energy cosmic ray observatory in the northern hemisphere. In addition, it will be the world's first air shower detector to be directly calibrated by an on-site accelerator beam. For wider and deeper understanding of cosmic rays by via high precision measurements, we have undertaken the study of extension plans for TA. One extension plan will extend the sensitive energy range of TA down to 1017 eV. A second plan would extend of the aperture area of the SD array. These plans are described in this note.

  19. Particles of primary cosmic radiation generating extensive air showers of energy above 1020 eV in the atmosphere

    Science.gov (United States)

    Dedenko, L. G.; Glushkov, A. V.; Knurenko, S. P.; Makarov, I. T.; Pravdin, M. I.; Podgrudkov, D. A.; Sleptzov, I. E.; Roganova, T. M.; Fedorova, G. F.; Fedunin, E. Yu.

    2010-12-01

    In order to construct the energy spectrum on the basis of data from the Yakutsk array, a method similar to that employed at the AGASA array is applied in addition to the standard approach based on experimental procedures. Moreover, a new, original, method underlying the calculation of the spectrum in the region of energies above 1020 eV is used to estimate energies. In order to compare data obtained at different arrays, it is proposed to harness the universal spectrum based on HiRes data. Within the QGSJET2 model, it is shown that a shower of energy 2 × 1020 eV was observed at the Yakutsk array. In the same energy region (above 2 × 1020 eV), the AGASA array recorded four showers, while the Fly's Eye array and Pierre Auger Observatory (PAO) recorded one shower each. These data do not confirm the conclusion that the flux of primary-cosmic-ray particles decreases because of the Greisen-Zatsepin-Kuzmin effect.

  20. Particles of primary cosmic radiation generating extensive air showers of energy above 1020 eV in the atmosphere

    International Nuclear Information System (INIS)

    In order to construct the energy spectrum on the basis of data from the Yakutsk array, a method similar to that employed at the AGASA array is applied in addition to the standard approach based on experimental procedures. Moreover, a new, original, method underlying the calculation of the spectrum in the region of energies above 1020 eV is used to estimate energies. In order to compare data obtained at different arrays, it is proposed to harness the universal spectrum based on HiRes data. Within the QGSJET2 model, it is shown that a shower of energy 2 x 1020 eV was observed at the Yakutsk array. In the same energy region (above 2 x 1020 eV), the AGASA array recorded four showers, while the Fly's Eye array and Pierre Auger Observatory (PAO) recorded one shower each. These data do not confirm the conclusion that the flux of primary-cosmic-ray particles decreases because of the Greisen-Zatsepin-Kuzmin effect.