Sample records for chacaltaya

  1. Search for Gamma Ray Bursts at Chacaltaya

    CERN Document Server

    Vernetto, S


    A search for Gamma Ray Bursts in the GeV-TeV energy range has been performed by INCA, an air shower array working at 5200 m of altitude at the Chacaltaya Laboratory (Bolivia). The altitude of the detector and the use of the "single particle technique" allows to lower the energy threshold up to few GeVs. No significant signals are observed during the occurrence of 125 GRBs detected by BATSE, and the obtained upper limits on the energy fluence in the interval 1-1000(100) GeV range from 3.2(8.6) 10^-5 to 2.6(7.0) 10^-2 erg/cm^2 depending on the zenith angle of the events. These limits, thanks to the extreme altitude of INCA, are the lowest ever obtained in the sub-TeV energy region by a ground based esperiment.

  2. Measurement of cosmic ray chemical composition at Mt. Chacaltaya

    Energy Technology Data Exchange (ETDEWEB)

    Ogio, S.; Kakimoto, F.; Harada, D.; Tokunou, H.; Burgoa, O.; Tsunesada, Y. [Institute of Technology, Dept. of Physics, Tokuo (Japan); Shirasaki, Y. [National Space Development Agency of Japan, Tsukuba (Japan); Gotoh, E.; Nakatani, H.; Shimoda, S.; Nishi, K.; Tajima, N.; Yamada, Y. [The Institute of Physical and Chemical Research, Wako, Saitama (Japan); Kaneko, T. [Okayama University, Dept. of Physics, Oakayama (Japan); Matsubara, Y. [Nagoya University, Solar-Terrestrial Environment Laboratory, Nagoya, Aichi (Japan); Miranda, P.; Velarde, A. [Universidad Mayor de San Andres, Institute de Investigaciones Fisicas, La Paz (Bolivia); Mizumoto, T. [National Astronomical Observatory, Mitaka, Tokyo (Japan); Yoshii, H.; Morizawa, A. [Ehime University, Dept. of Physics, Matsuyama, Ehime (Japan); Murakami, K. [Nagoya University of Foreign Studies, Nissin, Aichi (Japan); Toyoda, Y. [Fukui University of Technology, Faculty of General Education, Fukui (Japan)


    BASJE group has measured the chemical composition of primary cosmic rays with energies around the knee with several methods. These measurements show that the averaged mass number of cosmic ray particles increases with energy up to the knee. In order to measure the chemical composition in much wider energy range, it was started a new experiment at Mt. Chacaltaya in 2000.

  3. Present experiment of BASJE group at Mt. Chacaltaya

    Energy Technology Data Exchange (ETDEWEB)

    Yoshii, H.; Morizawa, A. [Ehime University, Dept. of Physics, Matsuyama, Ehime (Japan); Kakimoto, F.; Ogio, S.; Tsunesada, Y.; Tokunou, H.; Harada, D.; Burgoa, O. [Tokyo Institute of Technology, Dept. of Physics, Meguro, Tokyo (Japan); Tajima, N.; Yamada, Y.; Shimoda, S.; Nishi, K.; Nakatani, H.; Gotoh, E. [The Institute of Physics and Chemistry Research, Wako, Saitama (Japan); Shirasaki, Y. [National Space Development Agency of Japan, Tsukuba, Ibaraki (Japan); Miranda, P.; Velarde, A. [Instituto de Investigaciones en Informatica, Universidad Mayor de San Andres, La Paz (Bolivia); Kaneko, T. [Oayama University, Dept. of Physics, Okayama (Japan); Murakami, K. [Nagoya University of Foreign Studies, Nissin, Aichi (Japan); Toyoda, Y. [Fukui University of Technology, Faculty of General Education, Fukui (Japan); Matsubara, Y. [Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi (Japan); Mizumoto, Y. [National Astronomical Observatory, Mitaka, Tokyo (Japan)


    A compact air shower array to observe primary cosmic rays above a few TeV has been installed at Mt. Chacaltaya in Bolivia since 1996. This array is available to observe the air showers above 6 TeV and the longitudinal development curves above 50 TeV. The purpose of the observations is to study the chemical composition and the energy spectrum of cosmic rays in the energy region including the knee of the energy spectrum. First, the consistency between direct measurements (balloon-borne experiments) and air shower observations in the energy region from 50 TeV to 80 TeV is examined and confirmed. Next, the chemical composition and the energy spectrum are derived from the air shower observations. In the study, the longitudinal developments of shower particles are calculated by Monte Carlo simulations, assuming different chemical compositions above 80 TeV. The characteristics of the present air shower array and the comparison of the preliminary observed results with that of the simulations are presented.

  4. Emulsion chamber experiment at Mt. Chacaltaya multiple particle production and Centauro events

    Energy Technology Data Exchange (ETDEWEB)

    Ohsawa, A


    A review is made on the features of multiple particle production and the Centauro events, based on the data which are obtained by Chacaltaya emulsion chamber experiment. Discussion follows on whether the Feynman scaling law is holding or violated around 10{sup 14}, 10{sup 16} and 10{sup 18} eV, and on the origin of Centauro events.

  5. On the penetrating showers observed in Chacaltaya two-storey emulsion chambers

    Energy Technology Data Exchange (ETDEWEB)

    Tamada, M. [Kinski University, Faculty of Science and Engineering, Osaka (Japan)


    The penetrating nature of the cascade showers observed in the Chacaltaya two-storey chamber is compared with that of simulated (e, {gamma})-induced and hadron-induced cascade showers. It is shown that around 1/3 of the observed penetrating showers are neither (e, {gamma})-induced nor hadron-induced ones. A possible explanation is given in connection with mini-clusters.

  6. Atmospheric interactions detected in both the upper and the lower chambers at Chacaltaya (United States)

    Amato, N. M.; Arata, N.; Maldonado, R. H. C.


    The cosmic ray interactions in the energy region 10 to the 13th power to 10 to the 17th power eV were studied by emulsion chambers exposed at Chacaltaya, 5220 m above sea-level. The chambers have a two-storied structure, and the events observed in both chambers give important informations on these phenomena. The first Centauro event was detected as a small shower at the bottom of the upper chamber and as a big fraction of energy deposit in the lower chamber, which indicates a high contribution of hadronic showers. Results of the events with continuation in the rather low energy region are described.

  7. Study of hadron bundles observed in Chacaltaya two-story emulsion chamber (United States)

    Aoki, H.


    The existence of hadron-rich families associated with few gamma-ray emission named Centauro and Mini-Centauro phemonena was reported. It was investigated whether these are produced by the special type of interaction different from the ordinary pion multiple production or not. The experimental results are compared with simulation calculation based on ordinary multiple pion production model. Both hadron multiplicity distribution, obtained from the present observation and the simulation calculation, show almost the same distribution which means that hadron bundles of such smaller multiplicities are considered to originate from successive interactions of surviving nucleon with the nature of multiple production during passage through the atmosphere.

  8. Aligned interactions in cosmic rays

    Energy Technology Data Exchange (ETDEWEB)

    Kempa, J., E-mail: [Warsaw University of Technology Branch Plock (Poland)


    The first clean Centauro was found in cosmic rays years many ago at Mt Chacaltaya experiment. Since that time, many people have tried to find this type of interaction, both in cosmic rays and at accelerators. But no one has found a clean cases of this type of interaction.It happened finally in the last exposure of emulsion at Mt Chacaltaya where the second clean Centauro has been found. The experimental data for both the Centauros and STRANA will be presented and discussed in this paper. We also present our comments to the intriguing question of the existence of a type of nuclear interactions at high energy with alignment.

  9. Observation of genetic relation among new phenomena Geminion, Chiron and mini-Centauro (United States)


    The threshold energy problem of exotic type interactions is discussed on the basis of available information from the Chacaltaya emulsion chamber experiment. The genetic hypothesis is proposed as a working hypothesis to explain the discrepancy seen in cosmic ray study and CERN p bar -p collider experiments.

  10. Energetic delayed hadrons in large air showers observed at 5200m above sea level (United States)

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


    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.

  11. A study on hadron interactions through observation of cosmic-ray families of visible energy greater than 500 TeV in high mountain emulsion chambers

    Energy Technology Data Exchange (ETDEWEB)

    Hasegawa, S. [Waseda Univ., Tokyo (Japan). Adv. Res. Center for Sci. and Eng.; Tamada, M. [Faculty of Science and Technology, Kinki University, 3-4-1 Kowakae, Higashi-Osaka, Osaka 577 (Japan)


    The characteristics of hadron interactions are studied with emulsion chambers exposed at both Mt. Chacaltaya and the Pamirs. The total exposure is {approx}1330 m{sup 2} year. Event by event surveys on the shower configurations in a single family event were accomplished over the 75 cosmic-ray families in the highest energy range, i.e., visible energy greater than 500 TeV. Extraordinary characteristics of high energy shower clusters of small spread and the exotic type interactions, Centauro species, are discussed from the cosmic-ray-family phenomenological point of view. (orig.).

  12. Use of water-Cherenkov detectors to detect Gamma Ray Bursts at the Large Aperture GRB Observatory (LAGO)

    Energy Technology Data Exchange (ETDEWEB)

    Allard, D. [APC, CNRS et Universite Paris 7 (France); Allekotte, I. [Centro Atomico Bariloche, Instituto Balseiro (Argentina); Alvarez, C. [Facultad de Ciencias Fisico-Matematicas de la BUAP (Mexico); Asorey, H. [Centro Atomico Bariloche, Instituto Balseiro (Argentina); Barros, H. [Laboratorio de Fisica Nuclear, Universidad Simon Bolivar, Caracas (Venezuela, Bolivarian Republic of); Bertou, X. [Centro Atomico Bariloche, Instituto Balseiro (Argentina)], E-mail:; Burgoa, O. [Instituto de Investigaciones Fisicas, UMSA (Bolivia); Gomez Berisso, M. [Centro Atomico Bariloche, Instituto Balseiro (Argentina); Martinez, O. [Facultad de Ciencias Fisico-Matematicas de la BUAP (Mexico); Miranda Loza, P. [Instituto de Investigaciones Fisicas, UMSA (Bolivia); Murrieta, T.; Perez, G. [Facultad de Ciencias Fisico-Matematicas de la BUAP (Mexico); Rivera, H. [Instituto de Investigaciones Fisicas, UMSA (Bolivia); Rovero, A. [Instituto de Astronomia y Fisica del Espacio (Argentina); Saavedra, O. [Dipartimento di Fisica Generale and INFN, Torino (Italy); Salazar, H. [Facultad de Ciencias Fisico-Matematicas de la BUAP (Mexico); Tello, J.C. [Laboratorio de Fisica Nuclear, Universidad Simon Bolivar, Caracas (Venezuela, Bolivarian Republic of); Ticona Peralda, R.; Velarde, A. [Instituto de Investigaciones Fisicas, UMSA (Bolivia); Villasenor, L. [Facultad de Ciencias Fisico-Matematicas de la BUAP (Mexico); Instituto de Fisica y Matematicas, Universidad de Michoacan (Mexico)


    The Large Aperture GRB Observatory (LAGO) project aims at the detection of high energy photons from Gamma Ray Bursts (GRB) using the single particle technique in ground-based water-Cherenkov detectors (WCD). To reach a reasonable sensitivity, high altitude mountain sites have been selected in Mexico (Sierra Negra, 4550 m a.s.l.), Bolivia (Chacaltaya, 5300 m a.s.l.) and Venezuela (Merida, 4765 m a.s.l.). We report on detector calibration and operation at high altitude, search for bursts in 4 months of preliminary data, as well as search for signal at ground level when satellites report a burst.

  13. Galactic-disk enhancement of cosmic rays at E > 10{sup 12} eV

    Energy Technology Data Exchange (ETDEWEB)

    Ogio, S.; Tsunesada, Y.; Kakimoto, F.; Burgoa, O.; Harada, D. [Tokyo Institute of Technology, Dept. of Physics, Meguro, Tokyo (Japan); Gotoh, E.; Nakatani, H.; Nishi, K.; Tajima, N.; Yamada, Y. [The Institute of Physical and Chemical Research, Wako, Saitama (Japan); Kaneko, T. [Okayama University, Dept. of Phyisics, Okayama (Japan); Matsubara, Y. [Nagoya University, Solar-Terrestrial Environment Laboratory, Nagoya (Japan); Miranda, P.; Velaverde, A. [Universidad Mayor de San Andres, Institute de Investigaciones Fisicas, La Paz (Bolivia); Mizumoto, Y. [National Astronomical Observatory, Mitaka, Tokyo (Japan); Morizawa, A.; Yoshii, H. [Ehime University, Dept. of Physics, Ehime (Japan); Murakami, K. [Nagoya University of Foreing Studies, Nissin, Aichi (Japan); Shirasaki, Y. [National Space Development Agency of Space, Tsukuba, Ibaraki (Japan); Toyoda, Y. [Fukui University of Technology, Faculty of General Education, Fukui (Japan)


    It was observed an enhancement of cosmic rays from the Vela region with SAS array at Mt. Chacaltaya in Bolivia. It is not possible to conclude that this enhancement is caused by primary gamma-rays, since the observed events not limited with the less muons in the air showers show the same enhancement. In order to confirm this result with improved statistics and to investigate the energy dependence of this enhancement, it has been installed a new array, called MAS array. All the data with much higher statistics show the enhancement along the whole galactic disk.

  14. Simultaneous Observation of Solar Neutrons from the ISS and High Mountain Observatories in association with a flare on July 8, 2014

    CERN Document Server

    Muraki, Y; Koga, K; Kakimoto, F; Goka, T; Gonzalez, L X; Masuda, S; Matsubara, Y; Matsumoto, H; Miranda, P; Okudaira, O; Obara, T; Salinas, J; Sako, T; Shibata, S; Ticona, R; Tsunesada, Y; Valdes-Galicia, J F; Watanabe, K; Yamamoto, T


    An M6.5-class flare was observed at N12E56 of the solar surface at 16:06 UT on July 8, 2014. In association with this flare, solar neutron detectors located on two high mountains, Mt. Sierra Negra and Chacaltaya and at the space station observed enhancements in the neutral channel. The authors analysed these data and a possible scenario of enhancements produced by high-energy protons and neutrons is proposed, using the data from continuous observation of a solar surface by the ultraviolet telescope onboard the Solar Dynamical Observatory (SDO).

  15. Ion Acceleration in Solar Flares Determined by Solar Neutron Observations (United States)

    Watanabe, K.; Solar Neutron Observation Group


    Large amounts of particles can be accelerated to relativistic energy in association with solar flares and/or accompanying phenomena (e.g., CME-driven shocks), and they sometimes reach very near the Earth and penetrate the Earth's atmosphere. These particles are observed by ground-based detectors (e.g., neutron monitors) as Ground Level Enhancements (GLEs). Some of the GLEs originate from high energy solar neutrons which are produced in association with solar flares. These neutrons are also observed by ground-based neutron monitors and solar neutron telescopes. Recently, some of the solar neutron detectors have also been operating in space. By observing these solar neutrons, we can obtain information about ion acceleration in solar flares. Such neutrons were observed in association with some X-class flares in solar cycle 23, and sometimes they were observed by two different types of detectors. For example, on 2005 September 7, large solar neutron signals were observed by the neutron monitor at Mt. Chacaltaya in Bolivia and Mexico City, and by the solar neutron telescopes at Chacaltaya and Mt. Sierra Negra in Mexico in association with an X17.0 flare. The neutron signal continued for more than 20 minutes with high statistical significance. Intense gamma-ray emission was also registered by INTEGRAL, and by RHESSI during the decay phase. We analyzed these data using the solar-flare magnetic-loop transport and interaction model of Hua et al. (2002), and found that the model could successfully fit the data with intermediate values of loop magnetic convergence and pitch angle scattering parameters. These results indicate that solar neutrons were produced at the same time as the gamma-ray line emission and that ions were continuously accelerated at the emission site. In this paper, we introduce some of the solar neutron observations in solar cycle 23, and discuss the tendencies of the physical parameters of solar neutron GLEs, and the energy spectrum and population of the

  16. Analysis of a hadron rich event

    Energy Technology Data Exchange (ETDEWEB)

    Barroso, Sergio L.C.; C arvalho, Analzira O. de; Chinellato, Jose A.; Manganote, Edmilson J.T.; Mariano, Anderson; Shibuya, Edison H. [Universidade Estadual de Campinas (UNICAMP), SP (Brazil). Inst. de Fisica Gleb Wataghin


    Full text. In a 1975 experiment, Brazil-Japan Collaboration on Chacaltaya Emulsion Chamber observed an event that was nicknamed Centauro, after some uncommon features. The unusual aspect of small multiplicity in the upper chamber and a much bigger multiplicity in the lower part of the chamber - leading the nickname Centauro - came from an unbalanced ratio between hadrons and gamma induced showers. Other similar events were observed; from them, only one in the chamber no 16, exposed during the period March/1971 - April/1972 has their height determined. As this event has 7 hadron induced showers continuing from upper to lower chamber, the height was estimated by triangulation and ranges from (500-900) meters, approximately. Using the minimum height, main hadronic showers characteristics were reported in some occasions, for instance in 2006ISVHECRI, at Weihai Symposium. Main results there, mainly: Mean inelasticity of gamma-ray equal 0.27, mean transverse momenta about (1.2+-0.2) GeV/c, and rapidity density in (8.56-9.89) range. These and other results indicated that at least this Centauro candidate would be interpretable as a hadron rich event produced by a cosmic ray particle interaction at 1 Moliere unit above the chamber. For the 23 showers compatible with gamma induced showers we looked for possible gamma-gamma combinations that reconstruct neutral pions. (author)

  17. Exotic interactions among C-jets and Pb-jets (United States)


    The C-jets and Pb-jets were surveyed on the part of Chacaltaya emulsion chamber No.19 amounting to an exposure of 28.8 sq m yr. It is shown that the adopted events make up an unbiased sample of C-jets for sigma sub E gamma TeV. Mini-Centauro interaction gives the most natural explanation for the eight pinaught-less C-jets with three or more constituent shower core. Out of the eight double-cored pinaught-less events, three are found to have visible invariant masses 1.8 GeV/c. Three Pb-jets-lower are composed of double cores whose respective visible transverse momenta are greater than 0.5 GeV/c, suggesting that they are of Geminion origin or chiron origin. The energies of the parent particles are estimated to be 100 to 200 TeV for all three kinds of events. The implications of this energy estimate and the frequency of observed exotic events are discussed.

  18. Plasma volume expansion does not increase maximal cardiac output or VO2 max in lowlanders acclimatized to altitude. (United States)

    Calbet, José A L; Rådegran, Göran; Boushel, Robert; Søndergaard, Hans; Saltin, Bengt; Wagner, Peter D


    With altitude acclimatization, blood hemoglobin concentration increases while plasma volume (PV) and maximal cardiac output (Qmax) decrease. This investigation aimed to determine whether reduction of Qmax at altitude is due to low circulating blood volume (BV). Eight Danish lowlanders (3 females, 5 males: age 24.0 +/- 0.6 yr; mean +/- SE) performed submaximal and maximal exercise on a cycle ergometer after 9 wk at 5,260 m altitude (Mt. Chacaltaya, Bolivia). This was done first with BV resulting from acclimatization (BV = 5.40 +/- 0.39 liters) and again 2-4 days later, 1 h after PV expansion with 1 liter of 6% dextran 70 (BV = 6.32 +/- 0.34 liters). PV expansion had no effect on Qmax, maximal O2 consumption (VO2), and exercise capacity. Despite maximal systemic O2 transport being reduced 19% due to hemodilution after PV expansion, whole body VO2 was maintained by greater systemic O2 extraction (P VO2 during exercise regardless of PV. Pulmonary ventilation, gas exchange, and acid-base balance were essentially unaffected by PV expansion. Sea level Qmax and exercise capacity were restored with hyperoxia at altitude independently of BV. Low BV is not a primary cause for reduction of Qmax at altitude when acclimatized. Furthermore, hemodilution caused by PV expansion at altitude is compensated for by increased systemic O2 extraction with similar peak muscular O2 delivery, such that maximal exercise capacity is unaffected.

  19. LAGOVirtual: A Collaborative Environment for the Large Aperture GRB Observatory

    CERN Document Server

    Camacho, R; Diaz, G; Guada, C; Hamar, V; Hoeger, H; Melfo, A; Nunez, L A; Perez, Y; Quintero, C; Rosales, M; Torrens, R


    We present the LAGOVirtual Project: an ongoing project to develop platform to collaborate in the Large Aperture GRB Observatory (LAGO). This continental-wide observatory is devised to detect high energy (around 100 GeV) component of Gamma Ray Bursts, by using the single particle technique in arrays of Water Cherenkov Detectors (WCD) at high mountain sites (Chacaltaya, Bolivia, 5300 m a.s.l., Pico Espejo, Venezuela, 4750 m a.s.l., Sierra Negra, Mexico, 4650 m a.s.l). This platform will allow LAGO collaboration to share data, and computer resources through its different sites. This environment has the possibility to generate synthetic data by simulating the showers through AIRES application and to store/preserve distributed data files collected by the WCD at the LAGO sites. The present article concerns the implementation of a prototype of LAGO-DR adapting DSpace, with a hierarchical structure (i.e. country, institution, followed by collections that contain the metadata and data files), for the captured/simulate...

  20. Hadronic- and electromagnetic cores of air-showers observed by hybrid experiments at high mountains

    CERN Document Server

    Tamada, M


    Characteristics of the high energy families (bundle of high energy e, gamma) and hadrons in the air-showers detected in the hybrid experiment together with emulsion chamber and AS-array at Mt.Chacaltaya are studied in detail by comparing with those of CORSIKA simulations using interaction models of QGSJET and EPOS. Because the atmospheric families and hadron component have more direct information of the nuclear interaction, correlations between atmospheric families and burst (hadron component of air-showers) accompanied to air-showers are more sensitive to the mechanism of the the cosmic-ray interactions. The burst size dependence of the family energy is compared with those of simulations. It is found that the family energy accompanied by the air-showers with the larger burst-size is systematically smaller than that expected in the simulated events. The experimental results can not be described simply by changing the chemical composition of primary cosmic-rays and this indicates that the x-distribution of sec...

  1. Forward hard scattering in hadron-hadron collisions in the energy region approximately 10/sup 14/ eV

    CERN Document Server

    Shibata, T


    On the basis of the quark-parton picture, the author derives analytically the cross sections for production of hadrons and gamma rays through forward hard scattering in hadron-hadron collisions in the energy region approximately 10/sup 14/ eV. The author takes account of transverse motions both of partons inside proton (p/sub T/) /sub p to q/, and of hadrons fragmented from quark (gluon) (k/sub T/) /sub 1 to h/. In addition, the effects of scale violation are taken into account. The numerical results thus obtained are compared with cosmic-ray data in the energy region approximately 10/sup 14/ eV, observed at Mt. Chacaltaya by Japan-Brazil emulsion-chamber collaboration. After eliminating carefully the bias effect inherent there, it was found that the theoretical calculations reproduced surprisingly well the cosmic-ray data on large p/sub T gamma / not only in the shape, but also in the absolute value. The production cross sections of pi /sup +/ and K/sup +/ expected from the forthcoming p-p colliding beams wi...

  2. Approximation of lateral distribution of atmospheric Cherenkov light at different observation levels. Comparison with previous results

    CERN Document Server

    Mishev, A; Stamenov, J


    This work summarizes the results presented at 29th International Cosmic Ray Conference in Pune India. Generally the aim of this work is to obtain the lateral distribution of the atmospheric Cherenkov light in extensive air showers produced by different primary particles in wide energy range and at several observation levels and to fit the obtained lateral distributions. Using one large detector and partially modified CORSIKA code version are obtained the lateral distributions of Cherenkov light flux densities at several observation levels for different particle primaries precisely at 536 g/cm2 Chacaltaya, 700 g/cm2 Moussala and 875 g/cm2 Kartalska field observation levels for hadronic primaries and gamma quanta in the energy range 1011 eV-1016 eV. On the basis of the solution of over-determined inverse problem the approximation of these distributions is obtained. The same model function for all the primaries is used and for the different observation levels. The different model parameters for the different pri...

  3. Observation of very high energy cosmic-ray families in emulsion chambers at high mountain altitudes. Pt. 1

    Energy Technology Data Exchange (ETDEWEB)

    Baradzei, L.T.; Borisov, A.S.; Cherdyntseva, K.V.; Guseva, Z.M.; Denisova, V.G.; Dobrotin, N.A.; Dunaevsky, A.M.; Kanevskaya, E.A.; Karpova, S.A.; Maximenko, V.M.; Nam, R.A.; Puchkov, V.S.; Slavatinsky, S.A.; Smirnova, M.D.; Smorodin, Yu.A.; Uryson, A.V.; Zelevinskaya, N.G.; Zimin, M.V.; Zhdanov, G.B. (Lebedev Physical Inst., Academy of Sciences, Moscow (USSR)); Mikhailova, I.A.; Mukhamedshin, R.A.; Doroshenko, O.E.; Nikolaeva, L.P.; Sukhov, L.V.; Zatsepin, G.T. (Inst. for Nuclear Research, Academy of Sciences, Moscow (USSR)); Amineva, T.P.; Fedorova, G.F.; Ivanenko, I.P.; Iljina, N.P.; Kopenkin, V.V.; Managadze, A.K.; Popova, E.G.; Rakobolskaya, I.V.; Roganova, T.M.; Strogova, O.P.; Sveshnikova, L.G. (Inst. of Nuclear Physics, Moscow Univ. (USSR)); Chadranyan, L.Kh.; Khisanishvili, L.A.; Roinishvili, N.N.; Svanidze, M.S. (Inst. of Physics, Academy of Sciences, Georgia, Tbilisi (USSR)); Azimov, Z.A.; Bobodjanov, I.B.; Gubar, N.E.; Gulov, Yu.A.; Normuradov, F. (Inst. of Physics and; Chacaltaya Collaboration; Pamir Collaboration


    Characteristics of cosmic-ray hadronic interactions in the 10{sup 15}-10{sup 17} eV range are studied by observing a total of 429 cosmic-ray families of visible energy greater than 100 TeV found in emulsion chamber experiments at high mountain altitudes, Chacaltaya (5300 m above sea level) and the Pamirs (4300 m above sea level). Extensive comparisons were made with simulated families based on models so far proposed, concentrating on the relation between the observed family flux and the behaviour of high-energy showers in the families, hadronic and electromagnetic components. It is concluded that there must be global change in characteristics of hadronic interactions at around 10{sup 16} eV deviating from those known in the accelerator energy range, specially in the forwardmost angular region of the collision. A detailed study of a new shower phenomenon of small-p{sub T} particle emissions, p{sub T} being of the order of 10 MeV/c, is carried out and its relation to the origin of huge 'halo' phenomena associated with extremely high energy families is discussed as one of the possibilities. General characteristics of such super-families are surveyed. (orig.).

  4. Nuclear Track Detectors. Searches for Exotic Particles

    CERN Document Server

    Giacomelli, G


    We used Nuclear Track Detectors (NTD) CR39 and Makrofol for many purposes: i) Exposures at the SPS and at lower energy accelerator heavy ion beams for calibration purposes and for fragmentation studies. ii) Searches for GUT and Intermediate Mass Magnetic Monopoles (IMM), nuclearites, Q-balls and strangelets in the cosmic radiation. The MACRO experiment in the Gran Sasso underground lab, with ~1000 m^2 of CR39 detectors (plus scintillators and streamer tubes), established an upper limit for superheavy GUT poles at the level of 1.4x10^-16 cm^-2 s^-1 sr^-1 for 4x10^-5 Chacaltaya lab (5230 m a.s.l.), using 427 m^2 of CR39 detectors exposed for 4.22 y, gave an upper limit for IMMs of ~1.3x10^-15 cm^-2 s^-1 sr^-1. The experiments yielded interesting upper limits also on the fluxes of the other mentioned exotic particles. iii) Environmental studies, radiation monitoring, neutron dosimetry.

  5. The Energy Spectrum and the Chemical Composition of Primary Cosmic Rays with Energies from 1014 to 1016 eV (United States)

    Ogio, S.; Kakimoto, F.; Kurashina, Y.; Burgoa, O.; Harada, D.; Tokuno, H.; Yoshii, H.; Morizawa, A.; Gotoh, E.; Nakatani, H.; Nishi, K.; Shimoda, S.; Tajima, N.; Yamada, Y.; Kaneko, T.; Murakami, K.; Toyoda, Y.; Matsubara, Y.; Mizumoto, Y.; Shirasaki, Y.; Tsunesada, Y.; Miranda, P.; Velarde, A.


    We have measured extensive air showers with primary energies above 6 TeV at Mount Chacaltaya in Bolivia. The data were collected by an air shower array called the Minimum Air Shower (MAS) array starting in 2000 March. We applied an equi-intensity analysis method to the extensive air showers extended over the region of their maximum development. We varied the mixture of protons and iron in our simulations and compared these to the data to determine the mixing ratio of protons as a function of the primary energy. Using this, we derived the primary energy spectrum from 1014 to 5×1016 eV. Consequently, we conclude that the power-law index of the spectrum changes gradually around 1015.5 eV and that the obtained proton ratio decreases with increasing energy. We directly measured the longitudinal development of air showers generated by primaries with energies around the knee. We found that the average mass number of primary cosmic rays shows a steady increase with energy above 1014.5 eV and that the dominant component around the knee is not protons.

  6. The Large Aperture Gamma Ray Observatory as an Observational Alternative at High Altitude (United States)

    Rosales, M.


    Although satellite observations have revealed some mysteries about the origin and location of cosmic rays at low energies, questions remain to be resolved in higher energy ranges (>1 GeV). However, the flow of particles at high energies is very low, large sensitive areas are necessary, so that the detection of secondary particles from observatories on the surface of the earth is a technically viable solution. While the Pierre Auger Observatory has such capacity given its 16000 m^2 of detectors, low height above sea level greatly reduces its detection capability. The Large Aperture Gamma Ray Observatory (LAGO) is an observational alternative that attempts to overcome this limitation. This project was started in 2005, placing water Cherenkov Detectors at high altitude. Observation sites have been selected with some basic requirements: altitude, academic and technical infrastructure, existence of a research group responsible for assembly and maintenance of the detectors and the analysis, visualization, divulgation and data storage. This paper presents the general status of the observatories of Sierra Negra-México, Chacaltaya-Bolívia, Marcapomacocha-Perú, Mérida-Venezuela and Bucaramanga-Colombia.

  7. PREFACE: Second School on Cosmic Rays and Astrophysics (United States)

    Zepeda, Arnulfo


    The physics of cosmic rays, gamma rays and neutrinos has become nowadays a subject of fast development. On the other hand present and planed experimental facilities installed in the American continent, attract and facilitate the involvement of local young researchers. For these reasons Professor Oscar Saavedra and his team of the high altitude cosmic ray Chacaltaya laboratory and the Universidad Mayor de San Andres in La Paz Bolivia, conceived the idea of organizing the First School on Cosmic Rays and Astrophysics in La Paz 9-20 August 2004. That school was possible, in spite of the scarcity of funds, thanks to the solidary participation of several distinguish lecturers who paid their travel and local expenses. Their lectures were made available on a CD by the local students. It was then decided that a second school be organized for 2006 in Mexico. It was held from 28 August to 15 September 15. Some of the lecturers in this Second School on Cosmic Rays and Astrophysics were too busy to write their lectures, but here we put at the disposal of the interested community the contributions of Roberto Battiston, Karen S Caballero, Edgar Casimiro, David Delepine, Giorgio Giacomelli, Gonzalo Rodríguez and Luis Villaseñor. This School was possible thanks to the financial assistance of CONACyT (Mexico), the Benemerita Universidad Autonoma de Puebla, Centro de Investigacion y de Estudios Avanzados (Cinvestav), the University of Torino and the Centro Latino Americano de Fisica. Arnulfo Zepeda The editors of these proceedings are: Rebeca López Rodrigo Pelayo Oscar Saavedra Arnulfo Zepeda

  8. Glacial recession in the Tropical Andes from the Little Ice Age: the case of Ampato Volcanic Complex (Southern Peru (United States)

    Alcalá, J.; Palacios, D.; Zamorano, J. J.


    Data published over the last decade reveal substantial glacial recession in the tropical Andes since the Little Ice Age (LIA), (Ramirez, et al., 2001; Rabatel, et al., 2005; Rabatel, et al., 2008; Vuille, et al., 2008; Hastenrath, 2009; Jomelli, et al., 2009), and a growing rate of recession since the 1980’s caused by global warming (Ramirez, et al., 2001; Vuille, et al., 2008). Today there is great interest in the evolution of these ice masses due to heightened awareness of climate change and of the strategic importance that glaciers have as a hydrologic resource for communities in arid climate zones in the tropical Andes (Mark, 2008; Vuille et al., 2008). Cordillera Blanca forms part of the Andes Mountains of northern Peru, and is a chosen site for many studies on glacier evolution. Vuille et al. 2008 determined that a considerable area of ice mass was lost at Huascarán-Chopicalqui glacier (18% from 1920-1970) and Astesonraju glacier (20% from 1962-2003). Studies at Coropuna volcano, which has the most extensive glacier field in the western range of southern Peru, also report a strong melting trend that began with only minimal recession from 1955-1986 (4%), but increased to 14% from 1986-2007 (Úbeda et al., 2009). Only a few of the Andes glaciers are consistently monitored, and the most comprehensive data are for Chacaltaya and Zongo glaciers (16º S) in Bolivia. Since the maximum LIA, Chacaltaya has lost 89% of its surface area, particularly in recent years. By 1983, the totaled loss was five times the shrinkage for the period 1940-1963 (Ramirez, et al., 2001). Zongo glacier maintained equilibrium from 1956-1975, but later experienced a period dominated by continuous recession (Soruco, et al., 2009). This study expands current knowledge of glacier evolution since the LIA in the Central Volcanic Zone (CVZ; 14º - 27º S) (Stern, 2004) of the Andes. The study site was chosen in an area that had never been used for preliminary research of this type, concretely

  9. The LAGO Collaboration: Searching for high energy GRB emissions in Latin America (United States)

    Barros, H.; Lago Collaboration


    During more than a decade Gamma Ray Bursts (GRB a cosmological phenomena of tremendous power) have been extensively studied in the keV - MeV energy range. However, the higher energy emission still remains a mystery. The Large Aperture GRB Observatory (L.A.G.O.) is an international collaboration started in 2005 aiming at a better understanding of the GRB by studying their emission at high energies (> 1 GeV), where the fluxes are low and measurements by satellites are difficult. This is done using the Single Particle Technique, by means of ground-based Water Cherenkov Detectors (WCD) at sites of high altitude. At those altitudes it is possible to detect air showers produced by high energy photons from the GRB, i. e. a higher rate of events on a short time scale, of the order of the second. The Pierre Auger Observatory could detect such GRB given its large number of detectors, but at 1400 m.a.s.l. the expected signal is quite small. At higher altitudes, similar performance is expected with only a very small number of WCD. As of 2011, high altitude WCD are in operation at Sierra Negra (Mexico, 4650 m.a.s.l.), Chacaltaya (Bolivia, 5200 m.a.s.l.), Maracapomacocha (Peru, 4200 m.a.s.l.), and new WCDs are being installed in Venezuela (Pico Espejo, 4750 m.a.s.l.), Argentina, Brazil, Chile, Colombia and Guatemala. Most of the new WCDs will not be at high enough altitude to detect GRB, never the less it will allow obtaining valuable measurements of secondaries at ground level, which are relevant for solar physics. The LAGO sensitivity to GRB is determined from simulations (under a sudden increase of 1 GeV - 1 TeV photons from a GRB) of the gamma initiated particle shower in the atmosphere and the WCD response to secondaries. We report on WDC calibration and operation at high altitude, GRB detectability, background rates, search for bursts in several months of preliminary data, as well as search for signals at ground level when satellite burst is reported, all these show the