bluuebunny/crossref_metadata_2025 huggingface dataset:
FNIT: A TELESCOPE FOR SOLAR NEUTRON OBSERVATION FROM 3 TO 100 MEV
Authors: MOSER M. R. , FLÜCKIGER E. O. , RYAN J. M. , MACRI J. R. , McCONNELL M. L.
Published: December 2005

We present a Fast Neutron Imaging Telescope (FNIT) that is sensitive to neutrons in the energy range 3 – 100 MeV, optimized to study solar neutrons in the innermost heliosphere. The detection principle is based on multiple elastic neutron–proton scatterings in parallel plastic scintillator layers. Reaction kinematics allows then to determine direction and energy spectrum of the primary neutron flux. A performance evaluation prototype has been built, and we report on first laboratory measurements and Monte Carlo simulation results.
ARE THERE STRANGELETS IN COSMIC RAYS?
Authors: RYBCZYŃSKI M. , WŁODARCZYK Z. , WILK G.
Published: December 2005

Assuming that cosmic rays entering the Earth's atmosphere contain a small admixture of nuggets of strange quark matter in form of strangelets one can explain a number of apparently "strange" effects observed in different cosmic rays experiments. We shall demonstrate here that the mass spectrum of such strangelets fills the "nuclear desert" gap existing between the heaviest elements observed in Universe and the next "nuclear-like objects" represented by neutron and strange stars.
RADIAL GRADIENTS OF THE LOW-ENERGY PROTON BACKGROUND BETWEEN 20 AND 80 AU
Authors: ZELDOVICH M. A. , LOGACHEV YU. I. , KECSKEMÉTY K.
Published: December 2005

The radial variation of the ~ 0.5 – 2 MeV proton background is estimated at 20 – 80 AU during low solar activity periods using Voyager 1 LECP data. The estimation of proton radial gradient suggest an intensity drop between about 30 and 60 AU and a change of the gradient sign from negative to positive beyond about of 70 AU.
PAMELA SCIENCE
Authors:   on behalf of the PAMELA COLLABORATION., CARLSON P.
Published: December 2005

The PAMELA satellite-borne experiment1, to be launched in 2005, is a powerful spectrometer including a magnetic field tracker and particle identification detectors. PAMELA science is broad and includes studies of interstellar propagation, solar modulation and search for dark matter signals.
HINTS ON PULSAR ELECTROMAGNETIC ENERGY LOSSES FROM COSMIC-RAY POSITRON OBSERVATIONS
Authors: GRIMANI CATIA
Published: December 2005

We present preliminary results of the estimate of isolated pulsar contribution to the positron and electron interstellar fluxes when a polar cap model is assumed. Pulsars of all ages outside their host remnants have been considered. Cosmic-ray positron observations above a few GeV seem to indicate that an outer gap model is favoured over a polar cap model when the contribution of young pulsars only is taken into account. Here we show that pulsars with ages ranging between 10 kyr and 600 kyr, escaped from their remnants, give a contribution to the interstellar positron flux larger than that proposed in literature for the whole sample of pulsars younger than 10 kyr. Consequently, this result also indicates that outer gap electromagnetic energy losses overcome those at the polar cap. Future, low error e+/(e+ + e-) ratio observations as well as high energy pulsed gamma-ray measurements will allow us to verify this possibility.
COSMIC-RAY ANTIPROTON SPATIAL DISTRIBUTIONS COMPUTED IN MAGNETOSPHERE
Authors: FUKI MICHIO
Published: December 2005

The motion of antiprotons in the Magnetosphere region is computed with some initial conditions and the spatial distributions of them are plotted. The antiprotons in the polar region are looked like coming from the outer region. Meanwhile, the antiprotons on the ISS altitude are trapped in the radiation belt. This is explained by the model that antiprotons are originated in decay particles from the antineutrons produced with the cosmic ray interactions in the atmosphere. This also shows that they are rich in the SAA region in the ISS altitudes. In order to distinguish antiprotons from protons effectively, the differences of arrival directions of them are important.
THE AMS TRANSITION RADIATION DETECTOR
Authors: SPADA FRANCESCA R.
Published: December 2005

AMS-02 (Alpha Magnetic Spectrometer) will fly during three years on the International Space Station performing spectroscopy of cosmic particles, allowing the direct search of antimatter and the indirect search of dark matter. Annihilation of supersymmetric dark matter candidates could produce an excess in the 10 – 300 GeV region of the positron spectrum. An overall 10-6 separation factor for positrons from the more abundant protons is required to detect the signal. A Transition Radiation Detector (TRD) has been designed to achieve these physics goal.
ABOUT SEPARATION OF HADRON AND ELECTROMAGNETIC CASCADES IN THE PAMELA CALORIMETER
Authors:   for the PAMELA COLLABORATION., STOZHKOV YURI I. , BASILI A. , BENCARDINO R. , CASOLINO M. , DE PASCALE M. P. , FURANO G. , MENICUCCI A. , MINORI M. , MORSELLI A. , PICOZZA P. , SPARVOLI R. , WISCHNEWSKI R. , BAKALDIN A. , GALPER A. M. , KOLDASHOV S. V. , KOROTKOV M. G. , MIKHAILOV V. V. , VORONOV S. A. , YURKIN Y. T. , ADRIANI O. , BONECHI L. , BONGI M. , PAPINI P. , RICCIARINI S. B. , SPILLANTINI P. , STRAULINO S. , TACCETTI F. , VANNUCCINI E. , CASTELLINI G. , BOEZIO M. , BONVICINI M. , MOCCHIUTTI E. , SCHIAVON P. , VACCHI A. , ZAMPA G. , ZAMPA N. , CARLSON P. , LUND J. , LUNDQUIST J. , ORSI S. , PEARCE M. , BARBARINO G. C. , CAMPANA D. , OSTERIA G. , ROSSI G. , RUSSO S. , BOSCHERINI M. , MENNH W. , SIMONH M. , BONGIORNO L. , RICCI M. , AMBRIOLA M. , BELLOTTI R. , CAFAGNA F. , CIRCELLA M. , DE MARZO C. , GIGLIETTO N. , MIRIZZI N. , ROMITA M. , SPINELLI P. , BOGOMOLOV E. , KRUTKOV S. , VASILJEV G. , BAZILEVSKAYA G. A. , KVASHNIN A. N. , LOGACHEV V. I. , MAKHMUTOV V. S. , MAKSUMOV O. S. , STOZHKOV YU. I. , MITCHELL J. W. , STREITMATTER R. E. , STOCHAJ S. J.
Published: December 2005

Results of calibration of the PAMELA instrument at the CERN facilities are discussed. In September, 2003, the calibration of the Neutron Detector together with the Calorimeter was performed with the CERN beams of electrons and protons with energies of 20 – 180 GeV. The implementation of the Neutron Detector increases a rejection factor of hadrons from electrons about ten times. The results of calibration are in agreement with calculations.
UNCERTAINTIES OF ANTIPROTON SPECTRA FROM B/C DATA AND mSUGRA CONTRIBUTIONS FOR CLUMPY HALOS
Authors: ZDRAVKOVIĆ VLADIMIR , LIONETTO ANDREA , MORSELLI ALDO
Published: December 2005

We studied the total variation of e+ and [Formula: see text] spectra due to the parameters uncertainties of propagation models and cross sections. We used B/C data and Galprop code and we derived also the uncertainty bands for subFe/Fe ratio, H and He . Finally we have considered a neutralino induced component in the mSUGRA framework and we have concluded that even for the model with diffusion and convection, where secondary spectra gives a good fit of the data, neutralino induced contribution can not be excluded up to now due to the overall uncertainties.
OVERVIEW ON DIRECT AND INDIRECT MEASUREMENTS OF COSMIC RAYS
Authors: HÖRANDEL JÖRG R.
Published: December 2005

An overview is given on results from direct and indirect measurements of galactic cosmic rays. Their implications on the contemporary understanding of the origin of cosmic rays and the knee in their energy spectrum are discussed.
ON THE STATISTICAL METHODS OF THE SIGNAL SIGNIFICANCE ESTIMATION IN THE DETECTION OF THE SIGNAL FROM THE POINT SOURCES OF COSMIC RAYS
Authors: CHILINGARIAN A. , GHARAGYOZYAN G. , HOVSEPYAN G. , KARAPETYAN G.
Published: December 2005

The estimation of the significance of the peaks in 1 and 2-dimensional distributions is one of the most important problems in high-energy physics and astrophysics. The physical inference from low-statistics experiments usually is biased and many discoveries lack further confirmation. We analyze the significance of the experimental evidence in the on-going efforts of detecting the point source of Cosmic Rays. The analysis is carried out in the framework of two models utilizing the extremum statistics: first – using the fixed grid of celestial coordinates, and second – using the tuned grid (introducing more degrees of freedom in the search). The test distributions for the significance estimation are obtained both from simulation models and from the analytical treatment of the problem.
PRESENT STATUS OF COSMIC-RAY SPECTRUM AND COMPOSITION OBTAINED BY THE DIRECT MEASUREMENTS
Authors:   and the RUNJOB COLLABORATION., HAREYAMA MAKOTO , SHIBATA TORU
Published: December 2005

We report recent results on the cosmic-ray spectrum and the composition obtained by RUNJOB collaboration (RUssia-Nippon JOint Balloon collaboration). We present the preliminary spectra for individual elements from proton to iron as well as the all-particle and the average mass in the energy range 10 to ~ 1000 TeV/particle, using 95% of the total exposure, and compare them with other experimental data, particularly those recently reported by ATIC group.
INDIRECT MEASUREMENTS AROUND THE KNEE — RECENT RESULTS FROM KASCADE
Authors:   for the KASCADE COLLABORATION., ULRICH HOLGER , ANTONI T. , APEL W. D. , BADEA F. , BEKK K. , BERCUCI A. , BLÜMER H. , BOZDOG H. , BRANCUS I. M. , BÜTTNER C. , CHILINGARIAN A. , DAUMILLER K. , DOLL P. , ENGEL R. , ENGLER J. , FEßLER F. , GILS H. J. , GLASSTETTER R. , HAUNGS A. , HECK D. , HÖRANDEL J. R. , KAMPERT K.-H. , KLAGES H. O. , MAIER G. , MATHES H. J. , MAYER H. J. , MILKE J. , MÜLLER M. , OBENLAND R. , OEHLSCHLÄGER J. , OSTAPCHENKO S. , PETCU M. , REBEL H. , RISSE A. , RISSE M. , ROTH M. , SCHIELER H. , SCHOLZ J. , THOUW T. , ULRICH H. , VARDANYAN A. , VAN BUREN J. , WEINDL A. , WOCHELE J. , ZABIEROWSKI J. , ZAGROMSKI S.
Published: December 2005

In the presented analysis of air shower data measured with the KASCADE experiment energy spectra for five mass groups are reconstructed. The results show a change of composition towards heavier elements across the knee but also demonstrate an insufficient description of the data by the used hadronic interaction models QGSJet and SIBYLL.
MODERN STATE OF THE ATHLET SETUP AT THE TIEN SHAN
Authors:   The ATHLET COLLABORATION., AMURINA I. V. , ANTONOVA V. P. , AUTOVA G. M. , BABAEV M. K. , BAYGUBEKOV A. S. , BEYL' P. F. , BEISEMBAEV R. U. , BODUNOV-SKVORTSOV A. E. , BORISOV A. S. , CHERDYNTSEVA K. V. , CHUBENKO A. P. , CHUBENKO P. A. , DENISOVA V. G. , DROBZHEV V. I. , GUDKOVA E. N. , GUREVICH A. V. , GUSEVA Z. M. , KANEVSKAYA E. A. , KEMPA J. , KOGAN M. G. , KOSTIN E. V. , KRYAKUNOVA O. N. , KRUGLOV A. V. , KRYUKOV S. V. , KRYLOWA M. I. , KUPCHISHIN A. I. , MANAGADZE A. K. , MART'YANOV I. S. , MAXIMENKO V. M. , MUKASHEV K. M. , MUKHAMEDSHIN R. A. , NAM R. A. , NESTEROVA N. M. , NURITDINOV KH. , OSKOMOV V. V. , PAVLYUCHENKO V. P. , PISCAL' V. V. , YU. POLYAKOV R. , PUCHKOV V. S. , PYATOVSKY S. E. , RAKOBOL'SKAYA I. V. , ROGANOVA T. M. , ROINISHVILI N. N. , RYABOV V. A. , SADUEV N. O. , KH. SADYKOV T. , SHAULOV S. B. , SHCHEPETOV A. L. , SLAVATINSKY S. A. , STEPANOV A. V. , SVESHNIKOVA L. G. , SHOIYNBAEVA G. T. , TOLEGEN ZH. T. , VAVILOV YU. N. , VARGASOV A. V. , VIL'DANOV N. G. , VIL'DANOVA L. I. , YAKOVLEV V. I. , YULDASHBAEV T. S. , ZASTROZHNOVA N. N. , ZATSEPIN G. T. , ZHUKOV V. V.
Published: December 2005

We present up-to-date state of new experimental complex ATHLET.
THE DETECTION OF THE HIGH-ENERGY EAS MUON COMPONENT WITH THE LST DETECTOR OF KASCADE-GRANDE
Authors:   for the KASCADE-GRANDE COLLABORATION., BERCUCI A. , ANTONI T. , APEL W. D. , BADEA F. , BEKK K. , BERTAINA M. , BLÜMER H. , BOZDOG H. , BRANCUS I. M. , BRÜGGEMANN M. , BUCHHOLZ P. , BÜTTNER C. , CHIAVASSA A. , DAUMILLER K. , DI PIERRO F. , DOLL P. , ENGEL R. , ENGLER J. , FEßLER F. , GHIA P. L. , GILS H. J. , GLASSTETTER R. , HAUNGS A. , HECK D. , HÖRANDEL J. R. , KAMPERT K.-H. , KLAGES H. O. , KOLOTAEV Y. , MAIER G. , MATHES H. J. , MAYER H. J. , MILKE J. , MITRICA B. , MORELLO C. , MÜLLER M. , NAVARRA G. , OBENLAND R. , OEHLSCHLÄGER J. , OSTAPCHENKO S. , OVER S. , PETCU M. , PLEWNIA S. , REBEL H. , RISSE A. , ROTH M. , SCHIELER H. , SCHOLZ J. , STÜMPERT M. , THOUW T. , TOMA G. , TRINCHERO G. C. , ULRICH H. , VALCHIEROTTI S. , VAN BUREN J. , WALKOWIAK W. , WEINDL A. , WOCHELE J. , ZABIEROWSKI J. , ZAGROMSKI S. , ZIMMERMANN D.
Published: December 2005

A Limited Streamer Tube (LST) detector system has been installed at the KASCADE-Grande experiment to study the Extensive Air Showers (EAS) muon component above a threshold of 2.4 GeV. The extended area of 255 m2 of the LST and the fine granularity of detection enables a detailed study of the muon spatial distribution in the very central zone of the air shower. A dedicated, fractal based analysis has been developed to take advantage of the observables of this detector setup. The sensitivity on cosmic rays mass and energy discrimination has been verified, based on 1.5 years of data collection by the KASCADE experiment.
PRIMARY ENERGY ESTIMATION AND MASS DISCRIMINATION BY THE EAS LATERAL CHARGED PARTICLE DISTRIBUTIONS SIMULATED FOR KASCADE-GRANDE
Authors: BRANCUS I. M. , MITRICA B. , TOMA G. , SIMA O. , REBEL H. , HAUNGS A. , BADEA A. F. , OEHLSCHLAEGER J.
Published: December 2005

Simulation studies of the lateral distribution S(r) of charged EAS particles, as reconstructed for the detector layout of KASCADE-Grande are presented. The investigation applies the recently developed code SHOWREC designed for EAS reconstruction.
AN AIRBORNE EAS ARRAY TO ANALYSE THE KNEE ENERGY REGION
Authors: CAPDEVIELLE J. N. , COHEN F. , JȨDRZEJCZAK K. , SZABELSKA B. , SZABELSKI J. , WIBIG T.
Published: December 2005

The knee energy region contains still several ambiguities in both aspects of primary composition and possible change in the standard description of multiple production. EAS are generally detected during the cascade absorption phase where the trigger by protons dominates. On the contrary, for EAS recorded at high altitude, the trigger initiated by heavy nuclei primaries turns to be the most efficient.1 The large area of the Airbus A380 and the exposure available during several thousand hours of certification flights suggests the opportunity of an airborne experiment at 10 – 12 km altitude to follow the different size spectra up to ~ 107 GeV. Some basic simulations are carried here to point out different criteria suitable to discriminate between heavy and light primaries.
EAS ARRAY ON BOARD OF THE A380 AIRLINER
Authors: CAPDEVIELLE J. N. , COHEN F. , JȨDRZEJCZAK K. , SZABELSKA B. , SZABELSKI J. , WIBIG T.
Published: December 2005

We propose an airborne experiment to study cosmic rays at knee energy taking opportunity of 10.000 hours of Airbus A380 test flights at an altitude of 10 km. The available area of nearly 500 m2 would allow for deploying EAS array with hadron detectors to measure CR iron spectra up to ~ 107 GeV and high energy protons surviving without interaction. At an altitude of 10 km the showers initiated by heavy nuclei are more developed and stable than proton initiated showers.1 Registration of both E-M and hadron components will help to discriminate between heavy and light primaries.
THE AGE PARAMETER IN GIANT EAS
Authors: CAPDEVIELLE J. N. , COHEN F. , SANOSYAN K.
Published: December 2005

The age parameter from the longitudinal development can be used to describe the lateral distribution in giant EAS up to 5 km from the axis, even if the scaling properties of Approximation B in cascade theory fail after 3.5 Moliere radii. A set of analytic descriptions is proposed under the gaussian hypergeometric formalism replacing the Eulerian formalism of the classical NKG distribution, valid for electrons, muons and vertical equivalent muons (v.e.m.).
THE TUNKA EXPERIMENT: TOWARDS A 1-KM2 CHERENKOV EAS ARRAY IN THE TUNKA VALLEY
Authors: CHERNOV D. V. , KALMYKOV N. N. , KOROSTELEVA E. E. , KUZMICHEV L. A. , PROSIN V. V. , PANASYUK M. I. , SHIROKOV A. V. , YASHIN I. V. , BUDNEV N. M. , GRESS O. A. , PANKOV L. V. , PARFENOV YU. V. , SEMENEY YU. A. , LUBSANDORZHIEV B. K. , POKHIL P. G. , PTUSKIN V. S. , SPIERING CH. , WISCHNEWSKI R. , NAVARRA G.
Published: December 2005

The project of an EAS Cherenkov array in the Tunka Valley/Siberia with an area of about 1 km2 is presented. The new array will have a ten times bigger area than the existing TUNKA-25 array and will permit a detailed study of the cosmic ray energy spectrum and the mass composition in the energy range from 1015 to 1018 eV.
PRIMARY ENERGY SPECTRUM AND MASS COMPOSITION DETERMINED WITH THE TUNKA EAS CHERENKOV ARRAY
Authors: CHERNOV D. V. , KOROSTELEVA E. E. , KUZMICHEV L. A. , PROSIN V. V. , YASHIN I. V. , BUDNEV N. M. , GRESS O. A. , GRESS T. I. , PANKOV L. V. , PARFENOV YU. V. , SEMENEY YU. A. , LUBSANDORZHIEV B. K. , POKHIL P. G. , SCHMIDT T. , SPIERING CH. , WISCHNEWSKI R.
Published: December 2005

New results of 300 hours of operation of the TUNKA array are presented. An improved parametrization of the Cherenkov light lateral distribution function (LDF), based on CORSIKA Monte Carlo simulations and the experiment QUEST, has been used for the reconstruction of EAS parameters. The corrected energy spectrum in the knee region is obtained. The mean depth of the EAS maximum has been derived both from the analysis of LDF steepness and the FWHM of Cherenkov light pulse. The mean mass composition around the knee is estimated.
ATMOCOSMICS: A GEANT 4 CODE FOR COMPUTING THE INTERACTION OF COSMIC RAYS WITH THE EARTH'S ATMOSPHERE
Authors: DESORGHER L. , FLÜCKIGER E. O. , GURTNER M. , MOSER M. R. , BÜTIKOFER R.
Published: December 2005

We have developed a new Monte Carlo code called ATMOCOSMICS based on GEANT 4 that simulates the interaction of cosmic rays with the Earth's atmosphere. The code allows to compute the flux of secondaries (e-, e+, protons, neutrons, gammas, muons, pions, …) at user-defined atmospheric depths and/or altitudes. Profiles of the energy deposited by atmospheric shower particles into the atmosphere vs depth and/or altitude can be calculated. We present examples of simulation results obtained with the code, and compare them with experimental data.
SELECTION OF THE PRIMARY COSMIC RAY LIGHT COMPONENT WITH ARGO-YBJ
Authors: DI SCIASCIO G. , DI GIROLAMO T. , SAGGESE L.
Published: December 2005

The ARGO-YBJ experiment, currently under construction at the YangBaJing High Altitude Cosmic Ray Laboratory (Tibet, P.R. China, 4300 m a.s.l.), may be upgraded with a large muon detector (~ 2500 m2) both to extend the sensitivity to γ-ray sources to energies ≥ 20 TeV and to perform a cosmic ray primary composition study. In this paper we discuss the capability of the upgraded ARGO-YBJ detector to select the primary cosmic ray light component in the knee energy region.
LATERAL DISTRIBUTION OF MUONS IN EAS AS A FUNCTION OF PRIMARY ENERGY
Authors: EGANOV V. , GARYAKA A. , MARTIROSOV R. , MNATSAKANYAN E. , JONES L.-W. , PROCUREUR J.
Published: December 2005

Experimental EAS muon lateral distributions for Eμ ≥ 5 GeV at fixed primary energy at the knee region measured with the modernized muon hodoscope of the GAMMA installation (Mt. Aragats, Armenia) are presented. Comparison with the data of the previous hodoscope configuration for fixed shower sizes is made. The experimental muon lateral distributions at fixed primary energies are obtained using a new method for estimation of energy of the primary particles. Approximation function for experimental distributions is proposed. Data are compared with the simulated CORSIKA data.
STUDY OF PRIMARY PARTICLES IN THE KNEE REGION WITH THE GAMMA ARRAY
Authors: EGANOV V. , GARYAKA A. , MARTIROSOV R. , MNATSAKANYAN E. , SAHAKIAN V. , SOKHOYAN S. , GALLANT Y. , JONES L.-W. , PROCUREUR J.
Published: December 2005

Experimental data on extensive air shower characteristics obtained with the GAMMA array at Mt. Aragats (Armenia) at Ne ≥ 105 are used to calculate the so-called αe-parameter, which is directly connected with the energy of the primary cosmic radiation. It is shown that measurement of the αe-spectrum is an effective way to obtain the primary energy spectrum. Using the αe-parameter the primary all-particle energy spectrum of the cosmic radiation in the knee energy region is obtained and compared with the corresponding data of other experiments. Energy spectrum for "young" showers generated for the most part by protons is also obtained.
SIMULATIONS OF EXTENSIVE AIR SHOWERS TRIGGERED BY PROTON, IRON AND GAMMA PRIMARIES
Authors: GERANIOS A. , FOKITIS E. , MALTEZOS S. , PATRINOS K. , DIMOPOULOS A.
Published: December 2005

Using the AIRES code, we have generated a large number of Extensive Air Showers corresponding to Ultra high energy cosmic ray gammas, protons and iron nuclei with energy range 1015 – 1022 eV. These simulations clearly show the different atmospheric depths of the Extensive Air Shower maxima in this energy range.
THE EXPERIMENTAL DATA ON THE HIGH ENERGY GALACTIC COSMIC RAYS FROM EAS-TOP
Authors:   for the EAS-TOP COLLABORATION., GHIA P. L. , NAVARRA G.
Published: December 2005

We summarize the main results reported by EAS-TOP in the study of cosmic rays in the energy range 1012 – 1016 eV (from the direct measurements up to above the "knee"), i.e. the region which is generally considered to represent the high energy galactic radiation.
EXTENSIVE AIR SHOWER CHARACTERISTICS AS FUNCTIONS OF SHOWER AGE
Authors: GILLER MARIA , STOJEK HUBERT , WIECZOREK GRZEGORZ
Published: December 2005

We show that extensive air showers (EAS) are all very similar when described by shower age and Molière length unit. This allows to analyze fluorescence and Cherenkov light emitted by showers in a unified and simple way.
SOME ASPECTS OF THE PROPAGATION OF SUPER-HIGH ENERGETIC COSMIC RAYS IN THE GALAXY
Authors: HÖRANDEL JÖRG R. , KALMYKOV NIKOLAI N. , TIMOKHIN ALEKSEI V.
Published: December 2005

The origin of the knee in the energy spectrum of cosmic rays is one of the central questions of high-energy astrophysics. One possible explanation is the energy dependent leakage of nuclei from the Galaxy due to their propagation. The latter is investigated in a combined method using numerical calculations of trajectories and the diffusion approximation. The life time of cosmic rays in the Galaxy and the corresponding pathlength are presented. The resulting energy spectra as observed at Earth are discussed and compared to experimental data.
MEASURING RADIO PULSES FROM AIR SHOWERS WITH LOPES
Authors:   for the LOPES COLLABORATION., HORNEFFER ANDREAS , ANTONI T. , APEL W. D. , BADEA F. , BÄHREN L. , BEKK K. , BERCUCI A. , BERTAINA M. , BIERMANN P. L. , BLÜMER H. , BOZDOG H. , BRANCUS I. M. , BRÜGGEMANN M. , BUCHHOLZ P. , BUTCHER H. , BÜTTNER C. , CHIAVASSA A. , DAUMILLER K. , DE BRUYN G. , DE VOS C. M. , DI PIERRO F. , DOLL P. , ENGEL R. , ENGLER J. , FALCKE H. , FEßLER F. , GEMMEKE H. , GHIA P. L. , GILS H. J. , GLASSTETTER R. , HAUNGS A. , HECK D. , HÖRANDEL J. R. , HORNEFFER A. , HUEGE T. , KAMPERT K.-H. , KANT G. W. , KLAGES H. O. , 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. , MÜLLER M. , NAVARRA G. , NEHLS S. , NIGL A. , OBENLAND R. , OEHLSCHLÄGER J. , OSTAPCHENKO S. , OVER S. , PEPPING H. J. , PETCU M. , PLEWNIA S. , REBEL H. , RISSE A. , ROTH M. , SCHIELER H. , SCHOLZ J. , SCHOONDERBEEK G. , STÜMPERT M. , THOUW T. , TOMA G. , TRINCHERO G. C. , ULRICH H. , VALCHIEROTTI S. , VAN BUREN J. , VAN CAPELLEN W. , WALKOWIAK W. , WEINDL A. , WIJNHOLDS S. , WOCHELE J. , ZABIEROWSKI J. , ZAGROMSKI S. , ZENSUS J. A. , ZIMMERMANN D.
Published: December 2005

LOFAR is a new digital radio interferometer that is being build in The Netherlands. By sampling the radio waves with fast ADCs it can digitally store the whole waveform information and analyze transient events like air showers after they have been recorded. To demonstrate its ability to measure air showers we are building LOPES (a LOFAR PrototypeStation) at the site of an existing air shower array (KASCADE-Grande). The first phase consisting of 10 antennas is already running. It has demonstrated how digital interference suppression and beamforming can overcome the problem of radio interference and pick out air shower events.
SIMULATIONS OF RADIO EMISSION FROM COSMIC RAY AIR SHOWERS
Authors: HUEGE TIM , FALCKE HEINO
Published: December 2005

Radio emission from cosmic ray air showers has the potential to become an additional, cost-effective observing technique for cosmic ray research, being largely complementary to the well-established particle detector and air fluorescence techniques. We present Monte Carlo simulations of radio emission from extensive air showers in the scheme of coherent geosynchrotron radiation from electron-positron pairs gyrating in the earth's magnetic field. Preliminary results of our simulations are the predicted frequency, primary particle energy, shower zenith angle, shower azimuth angle and polarization dependence of the radio emission. These properties can be directly related to data measured by LOPES and other experiments.
ENERGY SPECTRA AND MASS COMPOSITION OF COSMIC RAYS IN THE FRACTAL-LIKE GALACTIC MEDIUM
Authors: LAGUTIN A. A. , TYUMENTSEV A. G. , YUSHKOV A. V.
Published: December 2005

We consider the problem of the cosmic ray spectrum formation assuming that cosmic rays are produced by galactic sources. The fractional diffusion equation proposed in our recent papers is used to describe the cosmic rays propagation in interstellar medium. We show that in the framework of this approach it is possible to explain the locally observed basic features of the cosmic rays in the energy region 1010 ÷ 1020 eV : difference between spectral exponents of protons and other nuclei, mass composition variation, "knee" problem, flattening of the primary spectrum for E ≥ 1018 ÷ 1019 eV .
PRIMARY ENERGY MEASUREMENT WITH EAS CHERENKOV LIGHT: EXPERIMENT QUEST AND CORSIKA SIMULATION
Authors:   the EAS-TOP COLLABORATION , INFN, IFSI and Universitá di Torino, Torino, I-10125 Italy, KOROSTELEVA E. E. , KUZMICHEV L. A. , PROSIN V. V. , LUBSANDORZHIEV B. K.
Published: December 2005

A new primary mass independent method of energy measurement has been developed by exploiting: a) the joint analysis of the shower size, obtained by EAS-TOP, and of the EAS atmospheric Cherenkov light lateral distribution, obtained by the QUEST array, and b) simulations based on the CORSIKA/QGSJET code. The method is based on the correlation between the size/energy ratio and the steepness of Cherenkov light lateral distribution and has been compared with a "classical" one based on the Cherenkov light flux at a fixed distance (175 m) from the EAS core. An absolute energy calibration of the EAS atmospheric Cherenkov light flux has been obtained.
COSMIC RAY ANISOTROPY WITH THE KASCADE EXPERIMENT
Authors:   for the KASCADE COLLABORATION., MAIER GERNOT , ANTONI T. , APEL W. D. , BADEA A. F. , BEKK K. , BERCUCI A. , BLÜMER H. , BOZDOG H. , BRANCUS I. M. , BÜTTNER C. , CHILINGARIAN A. , DAUMILLER K. , DOLL P. , ENGEL R. , ENGLER J. , FEßLER F. , GILS H. J. , GLASSTETTER R. , HAUNGS A. , HECK D. , HÖRANDEL J. R. , KAMPERT K.-H. , KLAGES H. O. , MATHES H. J. , MAYER H. J. , MILKE J. , MÜLLER M. , OBENLAND R. , OEHLSCHLÄGER J. , OSTAPCHENKO S. , PETCU M. , REBEL H. , RISSE A. , RISSE M. , ROTH M. , SCHATZ G. , SCHIELER H. , SCHOLZ J. , THOUW T. , ULRICH H. , VAN BUREN J. , VARDANYAN A. , WEINDL A. , WOCHELE J. , ZABIEROWSKI J.
Published: December 2005

Anisotropies in the arrival directions of cosmic rays reflect their source distribution and propagation properties. In the presented analysis extensive air shower measurements with KASCADE are analyzed with respect to large and small scale anisotropies. The resulting upper limits on large scale anisotropy amplitudes of 10-3 to 10-2 restrict the parameter space of several propagation models. No cosmic ray point sources could be found in a sky survey of the northern hemisphere. Typical upper flux limits for point sources are around 10-10 m -2 s -1.
LONG-TERM BALLOON COSMIC RAY EXPERIMENT: RESULTS OF ANALYSIS OF ENERGETIC ELECTRON PRECIPITATION EVENTS
Authors: MAKHMUTOV V. S. , BAZILEVSKAYA G. A. , STOZHKOV Y. I. , SVIRZHEVSKAYA A. K. , SVIRZHEVSKY N. S.
Published: December 2005

More than 500 energetic Electron Precipitation Events were observed in the Earth's Northern and Southern polar atmosphere during a long-term cosmic ray balloon experiment. The results of analysis of these events allow to show (1) distribution of occurrence rate of EPEs within solar activity cycle, (2) semiannual variation in the EPE occurrence, (3) interplanetary and geomagnetic conditions related to the EPEs in the atmosphere.
THE KNEE OF EAS SIZE SPECTRUM, MISSING COMPONENT AND VERY HIGH ENERGY MUONS
Authors: PETKOV V. B.
Published: December 2005

Knee formation in the EAS size spectrum as a possible result of some portion of EAS's energy carried away by some missing EAS component is discussed. To explain the absence of the bump in calculated EAS size spectrum for the standard EAS development in the present day experiments, the model of "catastrophic" EAS development was proposed. The hypothesis that all the energy lost for the further shower development ELT finally passes into neutrino (¾ELT) and muons (¼ELT) is shown to be practically excluded by present experimental data.
ALIGNED EVENTS OBSERVED BY EMULSION CHAMBERS IN THE KNEE REGION
Authors: TALAI M. C. , ATTALLAH R. , CAPDEVIELLE J. N.
Published: December 2005

The coplanar emission of very high energy secondary cosmic rays was observed at stratospheric altitudes by the X-ray emulsion chamber experiments ECHOS-Concorde and RUNJOB. This paper treats the physical relevancy of the experimental observations using Monte Carlo calculations carried out with the help of the CORSIKA program. Different high energy hadronic interaction models have been used to study the possible dependence of this effect upon the primary particle mass number.
A NEW STUDY ON THE ENERGY SPECTRUM AND COMPOSITION OF PRIMARY COSMIC RAY FLUX AT ENERGIES ~ 1014 – 1016 EV USING THE GRAPES-3 ARRAY AT OOTY
Authors: TONWAR S. C. , GUPTA S. K. , MOHANTY D. K. , MOHANTY P. K. , SIVAPRASAD K. , SREEKANTAN B. V. , HAYASHI Y. , ITO N. , KAWAKAMI S. , NONAKA T. , TANAKA H. , YOSHIKOSHI T.
Published: December 2005

Data collected with the 217-detector air shower array and the 560 m2 area tracking muon detector, being operated at Ooty in southern India by the India-Japan (Tata Institute-Osaka City University) collaboration, GRAPES, have been analyzed to study the shape of the energy spectrum and the composition around the knee. It is shown that the muon multiplicity distribution, observed with the highly modular muon detector, permits a relatively reliable measurement on the composition of primary flux which then helps in a more accurate reconstruction of the energy spectrum from the observed shower size spectrum. The highlights of the GRAPES array, the analysis procedure and the results are presented.
RECONSTRUCTION OF TOTAL MUON NUMBER IN KASCADE-GRANDE
Authors:   for the KASCADE-GRANDE COLLABORATION., VAN BUREN J. , ANTONI T. , APEL W. D. , BADEA F. , BEKK K. , BERCUCI A. , BERTAINA M. , BLÜMER H. , BOZDOG H. , BRANCUS I. M. , BRÜGGEMANN M. , BUCHHOLZ P. , BÜTTNER C. , CHIAVASSA A. , DAUMILLER K. , DI PIERRO F. , DOLL P. , ENGEL R. , ENGLER J. , FEßLER F. , GHIA P. L. , GILS H. J. , GLASSTETTER R. , HAUNGS A. , HECK D. , HÖRANDEL J. R. , KAMPERT K.-H. , KLAGES H. O. , KOLOTAEV Y. , MAIER G. , MATHES H. J. , MAYER H. J. , MILKE J. , MITRICA B. , MORELLO C. , MÜLLER M. , NAVARRA G. , OBENLAND R. , OEHLSCHLÄGER J. , OSTAPCHENKO S. , OVER S. , PETCU M. , PLEWNIA S. , REBEL H. , RISSE A. , ROTH M. , SCHIELER H. , SCHOLZ J. , STÜMPERT M. , THOUW T. , TOMA G. , TRINCHERO G. C. , ULRICH H. , VALCHIEROTTI S. , WALKOWIAK W. , WEINDL A. , WOCHELE J. , ZABIEROWSKI J. , ZAGROMSKI S. , ZIMMERMANN D.
Published: December 2005

The KASCADE-Grande experiment extends the existing extensive air shower experiment KASCADE by an array of 37 detector stations spread over an area of 0.5 km2. The new Grande array measures the charged component of the showers. To reconstruct the mass composition of the cosmic rays, additional information from the muon component of air showers is required. Using observables from the new Grande array together with the muon detectors of the original KASCADE array provides a possibility to reconstruct also the total muon number of each air shower. The quality of reconstruction based on comparison with simulated data, as well as first results of a reconstructed muon size spectrum are presented.
COSMIC RAY ANISOTROPY PROBLEM
Authors: ZIRAKASHVILI VLADIMIR N.
Published: December 2005

The anisotropy of cosmic rays, produced by Galactic supernovae is calculated. It is a factor 100 ÷ 1000 larger than the observed value at 1 PeV. It is shown that this contradiction can be explained if a cosmic ray diffusion coefficient is small in the local vicinity of the Sun.
UHECR: OVERVIEW OF EXPERIMENTS FROM SPACE
Authors: PETROLINI ALESSANDRO
Published: December 2005

An overview of the Ultra High Energy Cosmic Rays observation from Space and planned experiments is presented.
PREPARATION OF THE TUS SPACE EXPERIMENT FOR UHECR STUDY
Authors: ABRASHKIN V. I. , ALEXANDROV V. V. , ARAKCHEEV YU. A. , BITKIN V. E. , CORDERO A. , EREMIN S. A. , GARIPOV G. K. , GREBENYUK V. M. , KALMYKOV N. N. , KHRENOV B. A. , KOVAL V. V. , MARTINEZ O. , MATYUSHKIN A. M. , MORENO E. , NAUMOV D. V. , SHAT N. M. , PANASYUK M. I. , PARK I. H. , YU. POROKHOVOI S. , ROBLEDO C. , RUBINSTEIN I. A. , SHARAKIN S. A. , SILAEV A. A. , SABIROV B. M. , SALAZAR H. , SAPRYKIN O. A. , SLUNECHKA M. , SYROMYATNIKOV V. S. , TKATCHEV L. G. , TKACHENKO A. V. , TULUPOV V. I. , TYUKAEV R. I. , URMANTSEV F. F. , VILLASENOR L. , YASHIN I. V. , ZEPEDA A.
Published: December 2005

We report on the current status of the TUS space mission project: its goals and the progress achieved so far. The Fresnel mirrors design, performed checks and their production are discussed. Also we discuss our future plans including auxiliary analysis of the fluorescence light yield measured this year by LAPP (Annecy), JINR (Dubna) and LIP (Lisbon) MACFLY Collaboration.
RADIODETECTION OF COSMIC RAY EXTENSIVE AIR SHOWERS: UPGRADE OF THE CODALEMA EXPERIMENT
Authors: ARDOUIN D. , BELLETOILE A. , CHARRIER D. , DALLIER R. , DENIS L. , ESCHSTRUTH P. , GOUSSET T. , HADDAD F. , LAMBLIN J. , LAUTRIDOU P. , LECACHEUX A. , MONNIER-RAGAIGNE D. , RAHMANI A. , RAVEL O.
Published: December 2005

We present the characteristics and performance of a demonstration experiment devoted to the observation of ultra high-energy cosmic ray extensive air showers using a radiodetection technique. In a first step, one antenna narrowed band filtered acting as trigger, with a 4σ threshold above sky background-level, was used to tag any radio transient in coincidence on the antenna array. Recently, the addition of 4 particle detectors has allowed us to observe cosmic ray events in coincidence with antennas.
PHOTOMULTIPLIER DEVELOPMENT AND WAVELENGTH SHIFTER MANUFACTURING TO INCREASE THE DETECTION OF FAINT FLUORESCENCE SIGNALS
Authors: BERTAINA M. , EBISUZAKI T. , HIROTA K. , KAWASAKI Y. , SAKAKI N. , SATO M. , SHIMIZU H. M. , SHINOHARA T. , TAKIZAWA Y.
Published: December 2005

RIKEN has developed in collaboration with Hamamatsu a new type of Multi Anode Photomultiplier (MAPMT), R8900 series, with a large sensitive area of ~ 83% of the physical surface. The performance of R8900 is reviewed in the following. RIKEN has also manufactured a new type of wavelength shifter (w.s.) film to shift near-UV light (330 ÷ 400 nm ) to visible one. This film uses POPOP as a shifter and EPO-TEX as a substrate. The quantum efficiency of the film reaches ~ 80%.
MICROSCOPIC BLACK HOLE DETECTION IN UHECR: THE DOUBLE BANG SIGNATURE
Authors: CARDOSO V. , ESPÍRITO SANTO M. C. , PAULOS M. , PIMENTA M. , TOMÉ B.
Published: December 2005

According to recent conjectures on the existence of large extra dimensions in our universe, black holes could be produced during the interaction of Ultra High Energy Cosmic Rays with the atmosphere. However, and so far, the proposed signatures are based on statistical effects, not allowing identification on an event by event basis, and may lead to large uncertainties. In this note, events with a double bang topology, where the production and instantaneous decay of a microscopic black hole (first bang) is followed, at a measurable distance, by the decay of an energetic tau lepton (second bang) are proposed as an almost background free signature.
SPECTRUM OF COSMIC RAYS WITH ENERGY ABOVE 1017 EV
Authors: EGOROVA V. P. , GLUSHKOV A. V. , IVANOV A. A. , KNURENKO S. P. , KOLOSOV V. A. , KRASILNIKOV A. D. , MAKAROV I. T. , MIKHAILOV A. A. , OLZOYEV V. V. , PRAVDIN M. I. , SABOUROV A. V. , YE. SLEPTSOV I. , STRUCHKOV G. G.
Published: December 2005

The energy spectrum of primary cosmic rays with ultra-high energies based on the Yakutsk EAS Array data is presented. For the largest events values of S600 and axis coordinates have been obtained using revised lateral distribution function. The effect of the arrival time distribution at several axis distance on estimated density for Yakutsk and AGASA is considered.
THE ROLAND MAZE PROJECT — COSMIC RAY REGISTRATION AT SCHOOLS
Authors: FEDER J. , JȨDRZEJCZAK K. , KARCZMARCZYK J. , LEWANDOWSKI R. , SWARZYŃSKI J. , SZABELSKA B. , SZABELSKI J. , TOKARSKI P. , WIBIG T.
Published: December 2005

Experimental studies of cosmic rays at the highest energies (above 1018 eV) are the main scientific goal of the projected large area network of extensive air shower detectors. Placing the detectors on the roofs of high school buildings will lower the cost by using the existing urban infrastructure (INTERNET, power supply, etc.), and can be a very efficient way of science popularisation by engaging high school students in the research program. 30 high schools in Łódź are already involved in the project. The project has recently obtained some financial support from the City Council of Łódź. The donation enabled us to start experimental work on detector construction details. A cycle of lectures and seminars devoted to different aspects of project realization (detector construction, on-line data acquisition system, C++ programming) has been organized for students at our Institute and at schools.
HiSPARC AND MiniGRAIL
Authors: FROSSATI G. , HERBSCHLEB C. T. , OONK J. B. R. , DE WAARD A.
Published: December 2005

HiSPARC (High-School Project on Astrophysics Research with cosmics) is a project that envisages the use of a large array of cosmic ray detectors placed at high-schools and scientific institutions in the Netherlands in order to measure high-energy cosmic ray showers. Besides contributing to the HiSPARC project, Leiden University also uses the cosmic ray detectors as veto for the resonant gravitational wave antenna MiniGRAIL.
AIR FLUORESCENCE MEASUREMENT AT COLLEGE DE FRANCE
Authors:   for the EUSO COLLABORATION., GORODETZKY PHILIPPE
Published: December 2005

The Paris apparatus uses a 90 Sr electron source to ionize N 2. Fluorescence light is collected by a grating spectrometer, and, also by a photomultiplier tube covered by a BG3 filter (300 to 400 nm bandwidth, identical to the one used in EUSO). To get an accuracy on the fluorescence yield better than 10%, great care is applied to measure efficiencies, in particular, quantum and collection efficiencies of the photomultipliers.
THE FOCAL SURFACE OF THE EUSO TELESCOPE
Authors:   for the EUSO COLLABORATION.for the EUSO-Japan Group.for the EUSO-Italy Group.for the EUSO-France Group.for the EUSO-U.S. Group., KAWASAKI YOSHIYA , BERTAINA M. , EBISUZAKI T. , KAJINO F. , MIYAZAKI Y. , NAGANO M. , SAKAKI N. , SATO M. , SHIMIZU H. M. , TAKIZAWA Y. , AMERI M. , CATALANO O. , CUNEO S. , FONTANELLI F. , GRACCO V. , MUSICO P. , PALLAVICINI M. , PETROLINI A. , PRATOLONGO F. , SANNINO M. , BLEURVACQ N. , CADOUX F. , CHAPRON C. , GORODETZKY P. , NEDELEC P. , PATZAK T. , PLAGNOL E. , TAKAHASHI Y.
Published: December 2005

The Extreme Universe Space Observatory (EUSO) is a space mission to study extremely high-energy cosmic rays. The EUSO instrument is a wide-angle refractive telescope in near-ultraviolet wavelength region to observe time-resolved atmospheric fluorescence images of the extensive air showers from the International Space Station. The Focal surface is an aspherical curved surface, and its area amounts to about 4.5 m2. The focal surface detector is designed as a mosaic of multianode photomultipliers (MAPMT) for the single photoelectron counting capability. The strongest requirement for the focal surface detector is the maximization of the photon detection efficiency together with the uniformity over the focal surface. We have developed a new type of MAPMT. It is modified from the ordinary one and has a grid between the photocathode and the first dynode to electrostatically demagnify the photoelectron image on the dynode. We are also developing the HV supply system for a great number of MAPMTs. EUSO experiments the day-time and night-time every 90 minutes. The heat flow must be considered to stabilize the PMT characteristics, in parallel with the heat dissipation of the electronics attached on the focal surface supporting structure.
FLUCTUATIONS OF Xmax AND PRIMARY PARTICLE MASS COMPOSITION IN THE RANGE OF ENERGY 5 × 1017 - 3 × 1019EV BY YAKUTSK DATA
Authors: KNURENKO S. P. , IVANOV A. A. , KOLOSOV V. A. , PETROV Z. E. , YE. SLEPTSOV I. , STRUCHKOV G. G.
Published: December 2005

The experimental distributions of X max obtained with the Yakutsk EAS array at fixed energies of 5 × 1017, 1 × 1018 and 5 × 1018 eV are analysed. A recent version of the QGSJET model is used as a tool of our analysis. In the framework of this model, the most adequate mass composition of primary particles satisfying the experimental data on X max is selected.
INFLUENCE OF PRIMARY COSMIC RADIATION MASS COMPOSITION ON THE ESTIMATION OF EAS ENERGY
Authors: KNURENKO S. P. , IVANOV A. A. , KOLOSOV V. A. , PETROV Z. E. , YE. SLEPTSOV I. , STRUCHKOV G. G.
Published: December 2005

Fraction of energy, E em /E0, transferred to the electron-photon component of EAS at E0 = 1015 ± 1019 eV was estimated by using the Cherenkov radiation data and the data on charged particles obtained at the Yakutsk EAS array. The results are compared with predictions of different models for energy dissipation into the EAS electron-photon component and with calculations performed with different primary nuclei content. In the energy ranges 1015 ± 1016 eV and 1018 ± 1019 eV , the ratio E em /E0 is equal to (77 ± 2)% and (88 ± 2)%, respectively, that does not contradict to a mixed composition of primary particles in the first energy interval and purely proton composition in the second one.
MUONS WITH Eth ≥ 1 GEV AND MASS COMPOSITION IN THE ENERGY RANGE 1018 - 1020EV OBSERVED BY YAKUTSK EAS ARRAY
Authors: KNURENKO S. P. , KOLOSOV V. A. , MAKAROV I. T. , YE. SLEPTSOV I. , SLEPTSOVA V. R. , STRUCHKOV G. G.
Published: December 2005

The ratio of the muon flux density to charged particle flux density at distances of 300 and 600 m from the shower axis (ρμ(300)/ρ s (300) and ρμ(600)/ρ s (600)) is measured. In addition, the energy dependence of ρμ(1000) is analysed for showers with energies above 1018 eV. A comparison between the experimental data and calculations performed with the QGSJET model is given for the cases of primary proton, iron nucleus and gamma-ray. We conclude that the showers with E0 ≥ 3 × 1018 eV can be formed by light nuclei with a pronounced fraction of protons and helium nuclei. It is not excluded however that a small part of showers with energies above 1019 eV could be initiated by primary gamma-rays.
GLOBAL MEASUREMENT OF LIGHTNING-ASSOCIATED TRANSIENT LUMINOUS EVENTS (TLEs) FROM SPACE
Authors: SATO M. , EBISUZAKI T. , TAKIZAWA Y. , KAWASAKI Y. , SAKAKI N. , BERTAINA M. , SHIMIZU H. M. , TAKAHASHI Y. , ADACHI T.
Published: December 2005

In this study we present possibility of continuous measurements of lightning-associated transient luminous events (sprites, elves and blue jets) from the ISS altitude using the EUSO telescope. From global lightning data we estimated possible detection rates of lightning and TLEs. We also estimated photon numbers and optical spectra of TLEs in the near-ultraviolet region (300 – 400 nm) where the fluorescence emission caused by CRs exists. These results imply that EUSO has enough capabilities to monitor not only super-GZK CRs but also global lightning and TLEs.
DIFFUSED ČERENKOV LIGHT MEASUREMENTS FOR THE EUSO PROJECT
Authors: VALLANIA P. , CAPPA A. , FAVA L. , GALEOTTI P. , SAAVEDRA O. , VIGORITO C. , CHAUVIN J. , LEBRUN D. , MOREGGIA S. , STASSI P. , ASSIS P. , BROGUEIRA P. , ESPIRITO-SANTO M. C. , MELO L. , PIMENTA M. , SILVA J. C. , TOMÉ B. , AGNETTA G. , BIONDO B. , CATALANO O. , D'ALÍ STAITI G. , GIARRUSSO S. , GUGLIOTTA G. , LA ROSA G. , MANGANO A. , RUSSO F. , SCARSI P. , ZORA M.
Published: December 2005

The aim of the EUSO (Extreme Universe Space Observatory) experiment is to measure from space the fluorescent light produced by the interaction of Extreme Energy Cosmic Rays (EECRs) with the Earth atmosphere. Besides the fluorescent signal, a huge amount of Čerenkov photons is emitted in a narrow cone hitting the Earth surface, where it is partially diffused. The detection of this diffused signal, in a delayed coincidence with the fluorescent signal, allows the absolute positioning of the EECR track, while the knowledge of the diffusing properties of the surface gives an independent indication of the shower energy. Measuring simultaneously on ground the electromagnetic component, the direct Čerenkov light, and the diffused Čerenkov light over different surfaces, we aim to characterize the emitted signal as a function of the energy and the arrival direction of the Extensive Air Shower (EAS), and to evaluate its possible detection from space. This is implemented by the ULTRA (Uv Light Transmission and Reflection in the Atmosphere) experiment composed by a small EAS array and a UltraViolet (UV) telescope. The experimental setups used in the first runs at sea level and at 1970 m a.s.l. are described and the first preliminary results are presented.
HIGH ENERGY NEUTRINOS AS A PROBE FOR NEW PHYSICS AND ASTROPHYSICS
Authors: BUGAEV E. V.
Published: December 2005

A review of the recent achievements in high energy neutrino physics and, partly, neutrino astrophysics is presented. It is argued that experiments with high energy neutrinos of natural origin can be used for a search of new physics effects beyond the electroweak scale.
RESULTS FROM THE HARP EXPERIMENT
Authors:   on behalf of the HARP COLLABORATION., ORESTANO D.
Published: December 2005

The HARP experiment at CERN is performing extensive measurements of hadron production cross sections and secondary particle yields in the energy range 2 – 15 GeV over the full solid angle, using a large set of cryogenic and solid targets. First measurements of hadron production cross sections in the forward region (up to about 300 mrad), using a replica of the K2K target and a proton beam of 12.9 GeV/c, are reported.
RESULTS FROM L3+C
Authors:   for the L3 COLLABORATION., UNGER MICHAEL
Published: December 2005

The L3+C measurement of the momentum spectrum of atmospheric muons between 20 and 3000 GeV for zenith angles ranging from 0° to 58° is presented and compared to theoretical predictions. An upper flux limit on the antiproton to proton ratio using the moon shadow is reported and an overview on the ongoing L3+C data analysis is given.