ALBERT

Description: An air shower array for LOFAR: LORA Astrophysics and Space Sciences Transactions, 7, 195-199, 2011 Author(s): S. Thoudam, G. v. Aar, M. v. d. Akker, L. Bähren, A. Corstanje, H. Falcke, J. R. Hörandel, A. Horneffer, C. James, M. Mevius, O. Scholten, K. Singh, and S. ter Veen LOFAR is a new form of radio telescope which can detect radio emission from air showers induced by very high-energy cosmic rays. It can also look for radio emission from particle cascades on the Moon induced by ultra high-energy cosmic rays or neutrinos. To complement the radio detection, we are setting up a small particle detector array LORA (LOfar Radboud Air shower array) within an area of ~300 m diameter in the LOFAR core. It will help in triggering and confirming the radio detection of air showers with the LOFAR antennas. In this paper, we present a short overview about LORA and discuss its current status.

Description: Overview of radio detection of cosmic ray air showers in the MHz range, and prospects for a large scale experiment Astrophysics and Space Sciences Transactions, 7, 207-210, 2011 Author(s): Maximilien Melissas 1 for the Pierre AUGER Collaboration 2,* Since its revival in the last decade, radio detection of cosmic ray air showers has made tremendous progress. Today, several experiments are routinely detecting radio signals associated with air showers. Large cosmic ray observatories such as the Pierre Auger Observatory are also pursuing radio detection activities. As an introduction, in this article we will summarize the main results from the first generation of radio detection experiments: LOPES and CODALEMA. Then, we will show which questions concerning the radio emission mechanisms can be answered from larger-scale experiments like the Auger Engineering Radio Array (AERA), which is a 20 km 2 antenna array under construction close to other enhancement devices at the Pierre Auger Observatory.

Description: Measurements of cosmic-ray antiprotons with PAMELA Astrophysics and Space Sciences Transactions, 7, 225-228, 2011 Author(s): J. Wu on behalf of the PAMELA collaboration The PAMELA experiment is a satellite-borne apparatus designed to study charged particles, and especially antiparticles, in the cosmic radiation. The apparatus is mounted on the Resurs DK1 satellite which was launched on 15 June 2006. PAMELA has been traveling around the earth along an elliptical and semi-polar orbit for almost five years. It mainly consists of a permanent magnetic spectrometer, a time of flight system and an electromagnetic imaging calorimeter, which allows antiprotons to be identified from a dominating cosmic-ray background. New measurements of the cosmic-ray antiproton flux and the antiproton-to-proton flux ratio between 60 MeV and 180 GeV are presented, employing data collected between June 2006 and December 2008. Compared to previous experiments, PAMELA extends the energy range of antiproton measurements and provides significantly higher statistics. The derived antiproton flux and antiproton-to-proton flux ratio indicates that the main source of cosmic-ray antiprotons is considered to be secondary production and no primary contribution has to be invoked.

Description: The cosmic ray energy spectrum in the range 10 16 –10 18 eV measured by KASCADE-Grande Astrophysics and Space Sciences Transactions, 7, 229-234, 2011 Author(s): M. Bertaina, W.D. Apel, J.C. Arteaga-Velázquez, K. Bekk, J. Blümer, H. Bozdog, I.M. Brancus, P. Buchholz, E. Cantoni, A. Chiavassa, F. Cossavella, K. Daumiller, V. de Souza, F. Di Pierro, P. Doll, R. Engel, J. Engler, M. Finger, D. Fuhrmann, P.L. Ghia, H.J. Gils, R. Glasstetter, C. Grupen, A. Haungs, D. Heck, J.R. Hörandel, T. Huege, P.G. Isar, K.-H. Kampert, D. Kang, D. Kickelbick, H.O. Klages, K. Link, P. Łuczak, M. Ludwig, H.J. Mathes, H.J. Mayer, M. Melissas, J. Milke, B. Mitrica, C. Morello, G. Navarra, S. Nehls, J. Oehlschläger, S. Ostapchenko, S. Over, N. Palmieri, M. Petcu, T. Pierog, H. Rebel, M. Roth, H. Schieler, F. Schröder, O. Sima, G. Toma, G.C. Trinchero, H. Ulrich, A. Weindl, J. Wochele, M. Wommer, and J. Zabierowski The KASCADE-Grande experiment, located at Campus North of the Karlsruhe Institute of Technology (Germany) is a multi-component extensive air-shower experiment devoted to the study of cosmic rays and their interactions at primary energies 10 14 –10 18 eV. One of the main goals of the experiment is the measurement of the all particle energy spectrum in the 10 16 –10 18 eV range, i.e. extending the range accessible by KASCADE alone. The Grande detector samples the charged component ( N ch ) of the air shower while the original KASCADE array provides in addition a measurement of the muon component ( N μ ). The combined information of N ch and N μ is used to estimate the energy on an event-by-event basis and to derive the all-particle energy spectrum. Since the calibration of the observables in terms of the primary energy depends on Monte Carlo simulations, three different methods with partially different sources of uncertainties, have been considered and compared to each other to derive the systematics on the energy spectrum. The different methods employed to derive the spectrum and their uncertainties, as well as the implications of the obtained result, are discussed in detail.

Description: Directional correlations between UHECRs and neutrinos observed with IceCube Astrophysics and Space Sciences Transactions, 7, 201-205, 2011 Author(s): R. Lauer 1,2 for the IceCube Collaboration * Ultra-high energy cosmic rays (UHECR) above an energy threshold of tens of EeV might undergo only small deflections due to interstellar magnetic fields. Their arrival directions would then point to regions of possible hadronic acceleration processes, which are likely to be also sources of high energy neutrinos. To search for such cosmic accelerators, we present here the first multi-messenger analysis of directional correlations between neutrino candidates from the IceCube Observatory and UHECR events. Data taken with IceCube in a configuration of 22 strings provided the basis for using published events from both the Pierre Auger Observatory and the HiRes experiment as reference directions in a search for coincidences with neutrinos. The analysis was optimized according to strict blindness criteria and showed an excess of neutrino candidates close to UHECR directions with a probability of 1% to occur as a random fluctuation, consistent with a background-only hypothesis. An extension of this analysis to include newer IceCube data, taken with 40 strings and using a likelihood approach, is discussed in the outlook.

Description: Observation of the Fermi pulsar catalog at TeV energies with the Tibet air shower experiment Astrophysics and Space Sciences Transactions, 7, 211-215, 2011 Author(s): M. Amenomori, X. J. Bi, D. Chen, S. W. Cui, Danzengluobu, L. K. Ding, X. H. Ding, C. Fan, C. F. Feng, Zhaoyang Feng, Z. Y. Feng, X. Y. Gao, Q. X. Geng, Q. B. Gou, H. W. Guo, H. H. He, M. He, K. Hibino, N. Hotta, Haibing Hu, H. B. Hu, J. Huang, Q. Huang, H. Y. Jia, L. Jiang, F. Kajino, K. Kasahara, Y. Katayose, C. Kato, K. Kawata, Labaciren, G. M. Le, A. F. Li, H. C. Li, J. Y. Li, C. Liu, Y.-Q. Lou, H. Lu, X. R. Meng, K. Mizutani, J. Mu, K. Munakata, H. Nanjo, M. Nishizawa, M. Ohnishi, I. Ohta, S. Ozawa, T. Saito, T. Y. Saito, M. Sakata, T. K. Sako, M. Shibata, A. Shiomi, T. Shirai, H. Sugimoto, M. Takita, Y. H. Tan, N. Tateyama, S. Torii, H. Tsuchiya, S. Udo, B. Wang, H. Wang, Y. Wang, Y. G. Wang, H. R. Wu, L. Xue, Y. Yamamoto, C. T. Yan, X. C. Yang, S. Yasue, Z. H. Ye, G. C. Yu, A. F. Yuan, T. Yuda, H. M. Zhang, J. L. Zhang, N. J. Zhang, X. Y. Zhang, Y. Zhang, Yi Zhang, Ying Zhang, Zhaxisangzhu, and X. X. Zhou Using the Tibet-III air shower array, we search for steady TeV γ-rays from 18 pulsars in the Fermi Large Area Telescope pulsar catalog. Among them, we observe 8 sources including the Crab instead of the expected 0.41 sources at a significance of 2 σ or more excess. Under the assumption of Poisson distribution, the chance probability is estimated to be 1.4×10 −8 . When the Crab is excluded, it becomes 1.8×10 −7 . These low chance probabilities clearly show that the Fermi pulsars have a statistically significant correlations with TeV γ-ray excesses.

Description: The Proton and Helium cosmic ray spectra from 50 GeV to 15 TeV Astrophysics and Space Sciences Transactions, 7, 235-238, 2011 Author(s): A. V. Karelin, S. V. Borisov, A. M. Galper, and S. A. Voronov for PAMELA collaboration To date, very little has been done in the field of research of the nuclei cosmic ray spectra in the energy range between 1 and 10 TeV per nucleon and especially there were even fewer direct measurements in space. The PAMELA experiment (Casolini et al., 2008) has a possibility to make progress in this range. The method of the measurement of the helium and proton cosmic ray spectra with the energy higher than 50 GeV/nucleon was developed mainly with the use of the PAMELA calorimeter. This analysis method and the results obtained based on 3 years of measurements are presented.

Description: Recent results from VHE gamma astrophysics related to fundamental physics and cosmic rays Astrophysics and Space Sciences Transactions, 7, 217-224, 2011 Author(s): A. De Angelis High-energy photons are a powerful probe for astrophysics and for fundamental physics under extreme conditions. During the recent years, our knowledge of the most violent phenomena in the universe has impressively progressed thanks to the advent of new detectors for very-high-energy (VHE) gamma rays (above 100 GeV). Ground-based detectors like the Cherenkov telescopes (H.E.S.S., MAGIC and VERITAS) recently discovered more than 80 new sources. This talk reviews the present status of VHE gamma astrophysics, with emphasis on the recent results and on the experimental developments, keeping an eye on the future. The impact on fundamental physics and on cosmic-ray physics is emphasized.

Description: Young supernova remnants and the knee in the cosmic ray spectrum Astrophysics and Space Sciences Transactions, 7, 179-182, 2011 Author(s): A. Erlykin, T. Wibig, and A. W. Wolfendale It has recently been suggested that neutron stars inside the shells of young supernova remnants (SNR) are the sources of PeV cosmic rays and that the interaction of the particles with the radiation field in the SNR causes electron pair production, which has relevance to recent observations of "high" positron fluxes. Furthermore, the character of the interaction is such that the well-known knee in the cosmic ray energy spectrum can be explained. Our examination of the mechanism leads us to believe that the required parameters of SN and pulsars are so uncommon that the knee and positron fraction can only be explained if a single, local and recent SN – and associated pulsar – are concerned. In this case the mechanism can be valid.

Description: Measurement of the all-particle cosmic ray energy spectrum with IceTop Astrophysics and Space Sciences Transactions, 7, 175-178, 2011 Author(s): F. Kislat 1 for the IceCube collaboration 2 IceTop is an air shower array at the geographic South Pole forming the surface component of the IceCube Neutrino Observatory. In this paper, a method to reconstruct shower size and primary energy spectrum from data measured by IceTop is described. Data were divided into three zenith angle bins. Using Monte Carlo based on the SIBYLL and Fluka hadronic interaction models, agreement with an isotropic flux can only be achieved under the assumption of a mixed composition. A preliminary all-particle energy spectrum is presented.

Description: Primary energy reconstruction from the charged particle densities recorded at 500 m distance from shower core with the KASCADE-Grande detector Astrophysics and Space Sciences Transactions, 7, 191-194, 2011 Author(s): G. Toma, W. D. Apel, J. C. Arteaga, K. Bekk, M. Bertaina, J. Blümer, H. Bozdog, I. M. Brâncuş, P. Buchholz, E. Cantoni, A. Chiavassa, F. Cossavella, K. Daumiller, V. de Souza, F. Di Pierro, P. Doll, R. Engel, J. Engler, M. Finger, D. Fuhrmann, P. L. Ghia, H. J. Gils, R. Glasstetter, C. Grupen, A. Haungs, D. Heck, J. R. Hörandel, T. Huege, P. G. Isar, K.-H. Kampert, D. Kang, D. Kickelbick, H. O. Klages, K. Link, P. \L uczak, M. Ludwig, H. J. Mathes, H. J. Mayer, M. Melissas, J. Milke, B. Mitrică, C. Morello, G. Navarra, S. Nehls, J. Oehlschläger, S. Ostapchenko, S. Over, N. Palmieri, M. Petcu, T. Pierog, H. Rebel, M. Roth, H. Schieler, F. G. Schröder, O. Sima, G. C. Trinchero, H. Ulrich, A. Weindl, J. Wochele, M. Wommer, and J. Zabierowski Previous EAS investigations have shown that for a fixed primary energy the charged particle density becomes independent of the primary mass at certain (fixed) distances from the shower axis. This feature can be used as an estimator for the primary energy. We present results on the reconstruction of the primary energy spectrum of cosmic rays from the experimentally recorded S(500) observable (the density of charged particles at a distance of 500 m to the shower core as measured in a plane normal to the shower axis) using the KASCADE-Grande detector array. The KASCADE-Grande experiment is hosted by the Karlsruhe Institute for Technology – Campus North, Karlsruhe, Germany, 110 m a.s.l. and operated by an international collaboration. The obtained primary energy spectrum is presented along with the result of another reconstruction technique presently employed at KASCADE-Grande.

Description: The features of electronics structure of the multichannel scintillation module for the EMMA experiment Astrophysics and Space Sciences Transactions, 7, 171-174, 2011 Author(s): V. Volchenko, G. Volchenko, E. Akhrameev, L. Bezrukov, I. Dzaparova, T. Enqvist, L. Inzhechik, A. Izmaylov, J. Joutsenvaara, M. Khabibullin, A. Khotjantsev, P. Kuusiniemi, B. Lubsandorzhiev, O. Mineev, V. Petkov, R. Poleshuk, B. Shaibonov, J. Sarkamo, A. Shaykhiev, W. Trzaska, A. Yanin, and N. Yershov A brief description of the developed structural electric diagrams of 16-channel scintillation module for the underground EMMA experiment, the basic characteristics and parameters of the electrical diagrams of this module are presented. Multi-pixel photodiodes operating in a limited Geiger mode are used for photoreadout of the scintillator detectors in 16-channel scintillation module. The method of the automatic tuning of the photosensors gain based on the stabilization of an average counting rate of the scintillation detectors from gamma rays of a natural radioactive background is described.

Description: Solar activity and the associated ground level enhancements of solar cosmic rays during solar cycle 23 Astrophysics and Space Sciences Transactions, 7, 439-443, 2011 Author(s): M. Andriopoulou, H. Mavromichalaki, P. Preka-Papadema, C. Plainaki, A. Belov, and E. Eroshenko The solar cycle 23 seems to be of great interest for the researchers due to many peculiarities. A study of the parameters of the sixteen ground level enhancements recorded during the approximately 12-year period of it (1996–2008) together with the associated solar activity, including the main properties of the solar flares, the coronal mass ejections and the radio bursts has been realized, in an effort to understand the connection of these events. All studied cases seem to be connected with very intense flares of long duration, having a mean importance value of X 5.9 and a mean duration of 164.5 min, with either halo or partial halo coronal mass ejections with a mean linear velocity of 1876 km/sec, as well as with intense radio bursts. It is also noticed that the ground level enhancements of the 23rd solar cycle occurred after the onset time of the associated solar X -ray flares with a mean time delay of about 38 min, very useful result for their monitoring and prediction.

Description: An explanation of the Pioneer anomaly involving accelerated atomic clocks Astrophysics and Space Sciences Transactions, 7, 487-494, 2011 Author(s): K. Wilhelm and B. N. Dwivedi The Pioneer anomaly stands for unexplained frequency shifts of the Doppler radio-tracking signals received at the ground stations from the Pioneer 10 and 11 spacecraft in disagreement with expectations based on model calculations. We consider here observations of Pioneer 10 at heliocentric distances between 40 ua and 70.5 ua over a time interval of 11.55 years from 1987 to 1998. The anomaly has been interpreted in the literature either as a Doppler shift caused by an apparent spacecraft deceleration not accounted for by known effects, or as an unexpected clock acceleration of the frequency standards at the ground stations. The reasons for the anomalous behaviour are not understood in both cases. Based on a gravitational impact model – requiring a secular mass increase of all massive bodies – a solution is proposed that implies a clock acceleration with a value close to that of the Hubble constant.

Description: Academician S. N. Vernov and cosmic ray variations research in the former USSR Astrophysics and Space Sciences Transactions, 8, 25-28, 2012 Author(s): L. Dorman During my long scientific career of about 60 years (from 1951), I was happy to meet and cooperate with Academician S. N. Vernov. During the first step (1950–1952), S. N. Vernov together with N. V. Pushkov organized the first Soviet network of cosmic ray (CR) stations equipped by large automatically operating ionization chambers of A. Compton type shielded by 10 cm of Pb. This was the beginning of the CR variations research in the former USSR. In the present paper I consider step by step the development of experimental and theoretical basis of CR variations research in the former USSR and the great role of S. N. Vernov in this process.

Description: Improvement of charge resolution for trans-iron nuclei ( Z ≥ 30) in CR-39 plastic nuclear track detectors using trajectory tracing technique Astrophysics and Space Sciences Transactions, 7, 495-500, 2011 Author(s): S. Ota, N. Yasuda, L. Sihver, S. Kodaira, S. Naka, Y. Ideguchi, and N. Hasebe Charge identification of trans-iron nuclei (nuclear charge: Z ≥ 30) using CR-39 plastic nuclear track detector (PNTD) is essential as a part of an effort to our future measurements of the projectile charge changing cross sections for galactic cosmic ray nuclei, but extremely hard. Therefore, an improvement method of the charge resolution (δ Z ) for 350 MeV/n Ge in CR-39 PNTD using the trajectory tracing technique with averaging the signals of nuclear tracks for each ion was studied. Eight sheets of CR-39 PNTDs were aligned and exposed to Ge beam behind a graphite target to produce projectile fragments. Average of the nuclear track data was taken over 16 detector surfaces for each ion, then the δ Z of Ge was successfully improved from 0.31 charge unit on single surface to 0.15 charge unit in rms, which is good enough for making the precise cross section measurements and no other experiments using CR-39 PNTDs or the other passive detectors have achieved such a good δ Z for the trans-iron nuclei with Z /β 〈 50 (β: relativistic velocity). This method will be very important for our future cross section measurements toward the study of galactic cosmic ray origin.

Description: Helium counters for low neutron flux measurements Astrophysics and Space Sciences Transactions, 7, 511-514, 2011 Author(s): Z. Dębicki, K. Jędrzejczak, J. Karczmarczyk, M. Kasztelan, R. Lewandowski, J. Orzechowski, B. Szabelska, J. Szabelski, P. Tokarski, and T. Wibig We present a comparison of some characteristics of helium counters for measurements of low intensity neutron flux. We focus on neutron flux density measurements in low background laboratories. Because of an extremely low counting rate (few events per hour or less), we have concentrated on counter parameters which are sometimes meaningless under regular conditions, i.e. background from internal alpha radioactivity, percentage of events in full energy peak, and the width of this peak. The background depends on residual radioactivity of the counter tube material and can not be eliminated. The full energy peak characteristics can be specified by counter gas composition. We will present a comparison of four types of helium gas counters.

Description: Observations with the High Altitude GAmma-Ray (HAGAR) telescope array in the Indian Himalayas Astrophysics and Space Sciences Transactions, 7, 501-505, 2011 Author(s): R. J. Britto, B. S. Acharya, G. C. Anupama, N. Bhatt, P. Bhattacharjee, S. Bhattacharya, V. R. Chitnis, R. Cowsik, N. Dorji, S. K. Duhan, K. S. Gothe, P. U. Kamath, R. Koul, J. Manoharan, P. K. Mahesh, A. Mitra, B. K. Nagesh, N. K. Parmar, T. P. Prabhu, R. C. Rannot, S. K. Rao, L. Saha, F. Saleem, A. K. Saxena, S. K. Sharma, A. Shukla, B. B. Singh, R. Srinivasan, G. Srinivasulu, P. V. Sudersanan, A. K. Tickoo, D. Tsewang, S. S. Upadhya, P. R. Vishwanath, and K. K. Yadav The High Altitude GAmma-Ray (HAGAR) array is a wavefront sampling array of 7 telescopes, set-up at Hanle, at 4270 m amsl, in the Ladakh region of the Himalayas (Northern India). It constitutes the first phase of the HImalayan Gamma-Ray Observatory (HIGRO) project. HAGAR is the first array of atmospheric Cherenkov telescopes established at a so high altitude, and was designed to reach a relatively low threshold (currently around 200 GeV) with quite a low mirror area (31 m 2 ). Regular source observations are running since September 2008. Estimation of the sensitivity of the experiment is undergoing using several hours of data from the direction of Crab nebula, the standard candle source of TeV gamma-ray astronomy, and from dark regions. Data were acquired using the On-source/Off-source tracking mode, and by comparing these sky regions the strength of the gamma-ray signal could be estimated. Gamma-ray events arrive close to telescope axis direction while the cosmic-ray background events arrive from the whole field of view. We discuss our analysis procedures for the estimate of arrival direction, estimate of gamma ray flux from Crab nebula, and the sensitivity of the HAGAR system, in this paper.

Description: High-energy photons connected to atmospheric precipitations Astrophysics and Space Sciences Transactions, 7, 471-475, 2011 Author(s): A. V. Germanenko, Yu. V. Balabin, E. V. Vashenyuk, B. B. Gvozdevsky, and L. I. Schur Increases in intensity of X-radiation in the ground layer of the atmosphere observed during various atmospheric phenomena in two points: Apatity (Kola Peninsula) and Barentsburg (Spitsbergen) have been studied. A clear relationship between the increases and such atmospheric phenomena as rain and snowfall has been found. It is shown that these increases are not connected with any radionuclides. This research suggests that the principal cause of high-energy photons increase during precipitations are bremsstrahlung X -rays created by energetic electrons accelerated by electric fields in the clouds. A possible mechanism of generation of X -ray photons is discussed.

Description: Detecting ultra-high energy cosmic rays from space with unprecedented acceptance: objectives and design of the JEM-EUSO mission Astrophysics and Space Sciences Transactions, 7, 477-482, 2011 Author(s): M. Casolino, J. H. Adams, M. E. Bertaina, M. J. Christl, T. Ebisuzaki, P. Gorodetzky, Y. Hachisu, F. Kajino, Y. Kawasaki, G. Medina-Tanco, H. Miyamoto, H. Ohomori, E. Parizot, I. Park, P. Picozza, N. Sakaki, A. Santangelo, K. Shinozaki, Y. Takizawa, K. Tsuno, and JEM-EUSO collaboration The Extreme Universe Space Observatory on the Japanese Experiment Module (JEM-EUSO) of the International Space Station (ISS) is the first mission that will study from space Ultra High-Energy Cosmic Rays (UHECR). JEM-EUSO will observe Extensive Air Showers (EAS) produced by UHECRs traversing the Earth's atmosphere from above. For each event, the detector will make accurate measurements of the energy, arrival direction and nature of the primary particle using a target volume far greater than what is achievable from ground. The corresponding increase in statistics will help to clarify the origin and sources of UHECRs as well as the environment traversed during production and propagation. Possibly this will bring new light onto particle physics mechanisms operating at energies well beyond those achievable by man-made accelerators. The spectrum of scientific goals of the JEM-EUSO mission includes as exploratory objectives the detection of high-energy gamma rays and neutrinos, the study of cosmic magnetic fields, and tests of relativity and quantum gravity effects at extreme energies. In parallel JEM-EUSO will systematically perform observation of the surface of the Earth in the infra-red and ultra-violet ranges, studying also atmospheric phenomena (Transient Luminous Effects). The apparatus is a 2 t detector using Fresnel-based optics to focus the UV-light from EAS on a focal surface composed of about 6 000~multianode photomultipliers for a total of ~ 3 · 10 5 channels. A multi-layer parallel architecture has been devised to handle the data flow and select valid triggers, reducing it to a rate compatible with downlink constraints. Each processing level filters the event with increasingly complex algorithms using ASICs, FPGAs and DSPs in this order to reject spurious triggers and reduce the data rate.

Description: Features of relativistic solar proton spectra derived from ground level enhancement events (GLE) modeling Astrophysics and Space Sciences Transactions, 7, 459-463, 2011 Author(s): E. V. Vashenyuk, Yu. V. Balabin, and B. B. Gvozdevsky With the developed by the authors of a ground level enhancements events (GLE) modeling technique, the modeling study of 35 large GLEs for the period 1956–2006 has been carried out. The basic characteristics of relativistic solar protons (RSP) are obtained: a rigidity (energetic) spectrum, anisotropy axis direction, and pitch angle distributions for each event. It is shown that in nearly all events there existed two components (population) of relativistic solar particles: prompt and delayed. The prompt component (PC) prevails in the beginning of the event. It is characterized by an impulsive profile, strong anisotropy and exponential energetic spectrum. The delayed component (DC) dominates during maximum and decline phases of the events. It has a gradual intensity profile, moderate anisotropy and a power law energetic spectrum. The analysis of the large number GLE shows the value of a characteristic energy in the exponential spectrum of PC has rather stable meaning ~0.5 GeV and well agrees with the spectrum of protons accelerated in an electric field arising during the magnetic reconnection in the solar corona. The value of a spectral exponent of the power law spectrum of DC is distributed from 4 up to 6 with most at 5. This is close to the simulated spectrum arising in the process of stochastic acceleration in turbulent solar plasma.

Description: EAS hadronic component as registered by a neutron monitor Astrophysics and Space Sciences Transactions, 7, 507-510, 2011 Author(s): Yu. V. Balabin, B. B. Gvozdevsky, E. V. Vashenyuk, and D. D. Dzhappuev For the purposes of a study of hadron component of an extended air shower (EAS), two detectors of cosmic rays (CR) were joined at the Baksan Neutrino Observatory. They are an EAS array detector (the "Carpet") and a neutron monitor (NM). Due to the versatility of a new recording system a master-pulse, which comes from the "Carpet" and marks to occurring of EAS, is joined to NM data. After processing of the huge data set it is found that the time of EAS influence on NM is less than 1 ms. The distribution of time intervals between pulses in the first millisecond after EAS onset is essentially different from the background and shows presence of two processes with characteristic times 45 and 230 μs.

Description: A Shannon entropy approach to the temporal evolution of SEP energy spectrum Astrophysics and Space Sciences Transactions, 8, 19-24, 2012 Author(s): M. Laurenza, G. Consolini, M. Storini, and A. Damiani The kinetic energy spectra of solar energetic particle (SEP) events contain information on the particle acceleration mechanisms. A novel approach is proposed to investigate the time evolution of the spectral shape for the 20 February 2002 SEP event. Proton differential fluxes recorded by the ERNE instrument aboard SOHO, in the energy range 1.67–112 MeV, are analyzed. The solar source is associated with this SEP event by studying solar and interplanetary conditions during the considered time period. The energy spectrum evolution is studied by evaluating the time history of Shannon's differential entropy derived from the SEP fluxes. Our findings suggest that particle acceleration in the considered event is produced by a perpendicular shock in the solar corona. Moreover, dropouts in the particle flux are clearly identified up to energies of at least ~10 MeV.

Description: Measurements of He isotopic ratio in cosmic rays in the 100 MeV – 1 GeV range with the PAMELA experiment Astrophysics and Space Sciences Transactions, 7, 465-469, 2011 Author(s): M. Casolino, C. De Santis, N. De Simone, V. Formato, N. Nikonov, P. Picozza, and the PAMELA collaboration The PAMELA satellite-borne experiment was launched on 15 June 2006 from the Baikonur cosmodrome and it has been collecting data since then. The apparatus comprises a time-of-flight system, a silicon-microstrip magnetic spectrometer, a silicon-tungsten electromagnetic calorimeter, an anticoincidence system, a shower tail counter scintillator and a neutron detector. The combination of these devices allows precision studies of the charged cosmic radiation to be conducted over a wide energy range (100 MeV – 1 TeV) with high statistics, with particular focus on the antiparticle component. In this work we present 3 He/ 4 He isotopic ratio in the energy range from 100 MeV nucleon −1 to ~1 GeV nucleon −1 . The measured abundances are compared with different interstellar/heliospheric propagation calculations which are tuned on previous proton and helium measurements.

Description: A method for real-time GLE modeling Astrophysics and Space Sciences Transactions, 7, 453-458, 2011 Author(s): E. V. Vashenyuk By now real time systems of data collection of neutron monitor network have been created. The main goal of such systems is early detection of dangerous events of space weather, such as GLE, caused by arrival to the Earth of relativistic solar protons. Characteristics of these particles are determined from the data of the worldwide neutron monitor network by methods of GLE modeling. Traditional GLE modeling requires data of no less than 30–35 stations and takes a long time of computations. We developed a truncated technique of solar proton spectrum determination by data of limited number (20–25) of neutron monitor stations and with a simplified procedure of computations adapted for operative diagnostics of relativistic solar protons just arriving to the Earth. Possibilities of this truncated GLE modeling for the early forecast of radiation-dangerous fluxes of solar particles with moderate energies are also shown.

Description: The effect of cosmic ray intensity variations and geomagnetic disturbances on the physiological state of aviators Astrophysics and Space Sciences Transactions, 7, 373-377, 2011 Author(s): M. Papailiou, H. Mavromichalaki, K. Kudela, J. Stetiarova, S. Dimitrova, and E. Giannaropoulou Over the last few years various researches have reached the conclusion that cosmic ray variations and geomagnetic disturbances are related to the condition of the human physiological state. In this study medical data regarding 4018 Slovak aviators were analyzed in relation to daily variations of cosmic ray and geomagnetic activity. Specifically daily data concerning mean values of heart rate which were registered during the medical examinations of the Slovak aviators, were related to daily variations of cosmic ray intensity, as measured by the Neutron Monitor Station on Lomnicky Stit ( http://neutronmonitor.ta3.sk/realtime.php3 ) and the high resolution neutron monitor database ( http://www.nmdb.eu ) and daily variations of Dst and Ap geomagnetic indices. All subjects were men in good health of age 18–60 yrs. This particular study refers to the time period from 1 January 1994 till 31 December 2002. Statistical methods were applied to establish a statistical significance of the effect of geomagnetic activity levels and cosmic ray intensity variations on the aforementioned physiological parameters for the whole group. The Pearson r-coefficients were calculated and the Analysis of Variance (ANOVA) method was applied to establish the statistical significance levels (p-values) of the effect of geomagnetic activity and cosmic ray intensity variations on heart rate up to three days before and three days after the respective events. Results show that there is an underlying effect of geomagnetic activity and cosmic ray intensity variations on the cardiovascular functionality.

Description: Measurement of high-energy neutrons at ISS by SEDA-AP Astrophysics and Space Sciences Transactions, 7, 411-416, 2011 Author(s): K. Koga, T. Goka, H. Matsumoto, T. Obara, Y. Muraki, and T. Yamamoto A new type of solar neutron detector (NEM) was launched by the space shuttle Endeavour on 16 July 2009 and it began collecting data on 25 August 2009 at the International Space Station (ISS). In this paper we introduce preliminary results obtained by the NEM.

Description: Large area scintillation muon hodoscope for monitoring of atmospheric and heliospheric processes Astrophysics and Space Sciences Transactions, 7, 435-438, 2011 Author(s): N. V. Ampilogov, I. I. Astapov, N. S. Barbashina, V. V. Borog, D. V. Chernov, A. N. Dmitrieva, K. G. Kompaniets, A. A. Petrukhin, V. V. Shutenko, A. I. Teregulov, and I. I. Yashin A new muon hodoscope for investigations of the processes in heliosphere and terrestrial atmosphere by means of cosmic ray muons is described. The setup design is based on multi-layer assemblies of narrow long scintillation strips with WLS fiber readout. Features of the hodoscope design are described and results of tests of a full-scale prototype of the basic unit of the hodoscope detection system – the module – are discussed.

Description: Latitudinal and radial gradients of galactic cosmic ray protons in the inner heliosphere – PAMELA and Ulysses observations Astrophysics and Space Sciences Transactions, 7, 425-434, 2011 Author(s): N. De Simone, V. Di Felice, J. Gieseler, M. Boezio, M. Casolino, P. Picozza, PAMELA Collaboration†, and B. Heber Ulysses, launched on 6 October 1990, was placed in an elliptical, high inclined (80.2°) orbit around the Sun, and was switched off in June 2009. It has been the only spacecraft exploring high-latitude regions of the inner heliosphere. The Kiel Electron Telescope (KET) aboard Ulysses measures electrons from 3 MeV to a few GeV and protons and helium in the energy range from 6 MeV/nucleon to above 2 GeV/nucleon. The PAMELA (Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics) space borne experiment was launched on 15 June 2006 and is continuously collecting data since then. The apparatus measures electrons, positrons, protons, anti-protons and heavier nuclei from about 100 MeV to several hundreds of GeV. Thus the combination of Ulysses and PAMELA measurements is ideally suited to determine the spatial gradients during the extended minimum of solar cycle 23. For protons in the rigidity interval 1.6–1.8 GV we find a radial gradient of 2.7%/AU and a latitudinal gradient of −0.024%/degree. Although the latitudinal gradient is as expected negative, its value is much smaller than predicted by current particle propagation models. This result is of relevance for the study of propagation parameters in the inner heliosphere.

Description: Cosmic ray composition at the ankle in the energy spectrum Astrophysics and Space Sciences Transactions, 7, 275-278, 2011 Author(s): T. Wibig and A. W. Wolfendale Recent results from the Pierre Auger Observatory and the Hi-Res array have been analysed hoping to derive a strong statement about the mass composition in the region of the ankle, where the change from Galactic to ExtraGalactic cosmic ray flux should take place, at least according to some theoretical predictions. It is shown that there are problems in reconciling the data with expectation.

Description: On the energy spectrum of cosmic ray muons in 100 TeV region Astrophysics and Space Sciences Transactions, 7, 483-486, 2011 Author(s): Yu. F. Novoseltsev, A. G. Bogdanov, R. P. Kokoulin, R. V. Novoseltseva, V. B. Petkov, and A. A. Petrukhin The energy spectrum of cosmic ray muons in the energy range from several TeV to ~1 PeV obtained by means of the analysis of multiple interactions of muons (pair meter technique) in the Baksan underground scintillation telescope is presented. Some evidence for the additional muon flux (to the conventional one from pion and kaon decays) has been obtained at energies ~100 TeV.

Description: General overview of recent results from the Pierre Auger Observatory Astrophysics and Space Sciences Transactions, 7, 445-451, 2011 Author(s): R. Caruso on behalf of the Pierre Auger Collaboration Since June 2008 the Pierre Auger Observatory, designed for the research of ultra high energy cosmic rays, is taking data in its final configuration. In this paper I will present a short overview of its recent scientific results. More specifically, I will discuss the all particle energy spectrum and the evidence for the GZK features, the measurement of the elongation rate and the resulting inferences on mass composition, the evidence for anisotropy in the subset of the highest energy events.

Description: High-energy neutrino astronomy Astrophysics and Space Sciences Transactions, 7, 35-41, 2011 Author(s): A. Kouchner Neutrinos constitute a unique probe since they escape from their sources, travel undisturbed on cosmological distances and are produced in high-energy (HE) hadronic processes. In particular they would allow a direct detection and unambiguous identification of the acceleration sites of HE baryonic cosmic rays (CR), which remain unknown. The latest results achieved with the current experiments are briefly reviewed, including the efforts towards a multi-messenger approach.

Description: POLAR: A Space-borne X-Ray Polarimeter for Transient Sources Astrophysics and Space Sciences Transactions, 7, 43-47, 2011 Author(s): S. Orsi on behalf of the POLAR collaboration POLAR is a novel compact Compton X-ray polarimeter designed to measure the linear polarization of the prompt emission of Gamma Ray Bursts (GRB) and other strong transient sources such as soft gamma repeaters and solar flares in the energy range 50−500 keV. A detailed measurement of the polarization from astrophysical sources will lead to a better understanding of the source geometry and emission mechanisms. POLAR is expected to observe every year several GRBs with a minimum detectable polarization smaller than 10%, thanks to its large modulation factor, effective area, and field of view. POLAR consists of 1600 low-Z plastic scintillator bars, divided in 25 independent modular units, each read out by one flat-panel multi-anode photomultiplier. The design of POLAR is reviewed, and results of tests of one modular unit of the engineering and qualification model (EQM) of POLAR with synchrotron radiation are presented. After construction and testing of the full EQM, we will start building the flight model in 2011, in view of the launch foreseen in 2013.

Description: CZELTA: An overview of the CZECH large-area time coincidence array Astrophysics and Space Sciences Transactions, 7, 69-73, 2011 Author(s): F. Blaschke, J. Čermák, J. Hubík, P. Lichard, P. Přidal, J. Smejkal, K. Smolek, I. Štekl, and V. Vícha Main goal of the project CZELTA (CZEch Large-area Time coincidence Array) is to study global properties of high-energetic cosmic rays. To present date, project consists of 5 stations covering large area in the Czech republic capable of detection of extensive air showers with energy exceeding 10 14 eV. Such a network of distant stations can be an ideal tool for probing global structure of cosmic rays. We present the design of the detection system and obtained results.

Description: The possibilities of simultaneous detection of gamma rays, cosmic-ray electrons and positrons on the GAMMA-400 space observatory Astrophysics and Space Sciences Transactions, 7, 75-78, 2011 Author(s): A. M. Galper, R. L. Aptekar, I. V. Arkhangelskaya, M. Boezio, V. Bonvicini, B. A. Dolgoshein, M. O. Farber, M. I. Fradkin, V. Ya. Gecha, V. A. Kachanov, V. A. Kaplin, E. P. Mazets, A. L. Menshenin, P. Picozza, O. F. Prilutskii, V. G. Rodin, M. F. Runtso, P. Spillantini, S. I. Suchkov, N. P. Topchiev, A. Vacchi, Yu. T. Yurkin, N. Zampa, and V. G. Zverev The GAMMA-400 space observatory will provide precise measurements of gamma rays, electrons, and positrons in the energy range 0.1–3000 GeV. The good angular and energy resolutions, as well as identification capabilities (angular resolution ~0.01°, energy resolution ~1%, and proton rejection factor ~10 6 ) will allow us to study the main galactic and extragalactic sources, diffuse gamma-ray background, gamma-ray bursts, and to measure electron and positron fluxes. The peculiar characteristics of the experiment is simultaneous detection of gamma rays and cosmic-ray electrons and positrons, which can be connected with annihilation or decay of dark matter particles.

Description: The ANTARES neutrino telescope Astrophysics and Space Sciences Transactions, 7, 61-64, 2011 Author(s): A. Margiotta for the ANTARES Collaboration The ANTARES detector is the largest underwater neutrino telescope. It is installed in the Mediterranean Sea, at a depth of about 2500 m, close to Toulon, France. The Cherenkov photons emitted along the path of neutrino induced muons are detected by a 3-dimensional array of photomultipliers and used to reconstruct their trajectory. The construction of the detector was completed in May 2008. A short description of the experimental setup is given and some selected results are presented.

Description: Gamma ray sources observation with the ARGO-YBJ detector Astrophysics and Space Sciences Transactions, 7, 65-68, 2011 Author(s): S. Vernetto on behalf of the ARGO-YBJ collaboration In this paper we report on the observations of TeV gamma ray sources performed by the air shower detector ARGO-YBJ. The objects studied in this work are the blazar Markarian 421 and the extended galactic source MGROJ1908+06, monitored during ~2 years of operation. Mrk421 has been detected by ARGO-YBJ with a statistical significance of ~11 standard deviations. The observed TeV emission was highly variable, showing large enhancements of the flux during active periods. The study of the spectral behaviour during flares revealed a positive correlation of the hardness with the flux, as already reported in the past by the Whipple telescope, suggesting that this is a long term property of the source. ARGO-YBJ observed a strong correlation between TeV gamma rays and the X-ray flux measured by RXTM/ASM and SWIFT/BAT during the whole period, with a time lag compatible with zero, supporting the one-zone SSC model to describe the emission mechanism. MGROJ1908+06 has been detected by ARGO-YBJ with ~5 standard deviation of significance. From our data the source appears extended and the measured extension is σ ext = 0.48°  +0.26 −0.28 , in agreement with a previous HESS observation. The average flux is in marginal agreement with that reported by MILAGRO, but significantly higher than that obtained by HESS, suggesting a possible flux variability.

Description: Ionization in the atmosphere, comparison between measurements and simulations Astrophysics and Space Sciences Transactions, 7, 29-33, 2011 Author(s): T. Sloan, G. A. Bazilevskaya, V. S. Makhmutov, Y. I. Stozhkov, A. K. Svirzhevskaya, and N. S. Svirzhevsky A survey of the data on measured particle fluxes and the rate of ionization in the atmosphere is presented. Measurements as a function of altitude, time and cut-off rigidity are compared with simulations of particle production from cosmic rays. The simulations generally give a reasonable representation of the data. However, some discrepancies are found. The solar modulation of the particle fluxes is measured and found to be a factor 2.7 ± 0.8 greater than that observed for muons alone near sea level.

Description: Neutrino bursts from gravitational stellar collapses with LVD Astrophysics and Space Sciences Transactions, 7, 49-52, 2011 Author(s): A. Molinario and C. Vigorito The main goal of the Large Volume Detector (LVD), in the INFN Gran Sasso National Laboratory (Italy), is the study of neutrino bursts from gravitational stellar collapses in the Milky Way. Both the detector and the data analysis procedure have been actually optimized for this purpose. Moreover the modularity of the apparatus allows to obtain a duty cycle that is very close to 100%, so that the experiment is continuously monitoring the Galaxy. The search for Supernova neutrino signal is performed online, within fixed duration time windows (20 s), and offline with variable duration time windows from few ms up to 200 s. In both cases, LVD is able to disentangle a cluster of neutrino signals from the background fluctuations, and its sensitivity extends to the whole Galaxy. No candidates have been detected during almost 18 years of observation (6013 days of lifetime): the resulting 90% c.l. upper limit to the rate of gravitational stellar collapses in the Galaxy is 0.14 events/year. Detector performances, search method and data results are here reported.

Description: Different concepts of next generation IACT arrays Astrophysics and Space Sciences Transactions, 7, 53-59, 2011 Author(s): V. Bugaev Having matured over a few decades, the IACT technique is now ready to widen its energy domain as well as to increase sensitivity in its core region (0.1–50 TeV) by as much as one order of magnitude as compared to existing facilities. This will allow to use γ astronomy to search for dark matter, probe intergalactic space and quantum gravity as well as to make efficient observations of extended sources. The design of a new-generation IACT array is motivated by the key science questions to be addressed and constrained by the cost of the experiment. A number of performance characteristics impact the scientific capabilities, not just point-source sensitivity, but also field-of-view, angular resolution, energy threshold and others, and the optimization of the parameters at fixed cost defines the approach to simulation studies. In this paper, I will highlight IACT array design studies carried through to optimize the array configuration, optical and mechanical designs as well as possible designs for telescope cameras.

Description: Semi-analytical model of cosmic ray electron transport Astrophysics and Space Sciences Transactions, 7, 265-269, 2011 Author(s): A. Ivascenko and F. Spanier We present a numerical extension to the analytical propagation model introduced in Hein and Spanier (2008) to describe the leptonic population in the galactic disc. The model is used to derive a possible identification of the components that contribute to the leptonic cosmic ray spectrum, as measured by PAMELA, Fermi and HESS, with an emphasis on secondary e + − e − production in collisions of cosmic ray particles with ambient interstellar medium (ISM). We find that besides secondaries, an additional source symmetric in e + and e − production is needed to explain both the PAMELA anomaly and the Fermi bump, assuming a power-law primary electron spectrum. Our model also allows us to derive constraints for some properties of the ISM.

Description: HEAT – a low energy enhancement of the Pierre Auger Observatory Astrophysics and Space Sciences Transactions, 7, 183-186, 2011 Author(s): C. Meurer 1 and N. Scharf 1 on behalf of the Pierre Auger Collaboration 2,* The High Elevation Auger Telescopes (HEAT) are three tiltable fluorescence telescopes which represent a low energy enhancement of the fluorescence telescope system of the southern site of the Pierre Auger Observatory in Argentina. The Pierre Auger Observatory is a hybrid cosmic ray detector consisting of 24 fluorescence telescopes to measure the fluorescence light of extensive air showers complemented by 1600 water Cherenkov detectors to determine the particle densities at ground. In this configuration air showers with a primary energy of 10 18 eV and above are investigated. By lowering the energy threshold by approximately one order of magnitude down to a primary energy of 10 17 eV, HEAT provides the possibility to study the cosmic ray energy spectrum and mass composition in a very interesting energy range, where the transition from galactic to extragalactic cosmic rays is expected to happen. The installation of HEAT was finished in 2009 and data have been taken continuously since September 2009. Within these proceedings the HEAT concept is presented. First data already demonstrate the excellent complement of the standard Auger fluorescence telescopes by HEAT.

Description: Baksan Underground Scintillation Telescope upgrade and DAQ of additional layers Astrophysics and Space Sciences Transactions, 7, 187-189, 2011 Author(s): I. M. Dzaparova, A. F. Yanin, M. M. Boliev, Zh. Sh. Guliev, L. V. Inzhechik, M. M. Kochkarov, M. G. Kostyuk, A. N. Kurenya, R. V. Novoseltseva, Yu. F. Novoseltsev, V. B. Petkov, P. S. Striganov, V. I. Volchenko, and G. V. Volchenko The project of the Baksan Underground Scintillation Telescope (BUST) upgrade is presented. Additional outer layers of the detectors with fine spatial resolution will be mounted around BUST. Optimal dimensions of a counter, 0.125 m × 0.125 m × 0.03 m were chosen with a simulation program. The functional diagram of BUST’s DAQ additional layers is presented. Modernization allows us to study the knee region using muon number spectrum measurements.

Description: Neutrinos from Starburst-Galaxies – A source stacking analysis of AMANDA II and IceCube data Astrophysics and Space Sciences Transactions, 7, 7-10, 2011 Author(s): J. Dreyer, J. K. Becker, W. Rhode, and the IceCube Collaboration A stacking analysis performed with data from the IceCube neutrino observatory is presented in this paper. In general, the stacking technique is sensitive to a cumulative signal from a generic source class. This can lead to a significant signal for the most luminous sources of the class, even if the individual sources cannot be detected. Here, the final data set of the AMANDA-II experiment, which is the predecessor of the IceCube, is used for an analysis. In a second analysis, data from a quarter of the IceCube detector is used. IceCube consists of so called stings, these are steel cables with photo multipliers hooked up which are deployed into the Antarctic ice to depths between 1450 m and 2450 m. This analysis covers data taken with 22 strings of IceCube (IC-22) within one year. For the first time, a sample of Starburst Galaxies was analyzed. In addition, several AGN catalogs are used as well as a catalog of pulsars. The analysis did not reveal a significant neutrino signal for any of the analyzed source classes, neutrino flux limits were improved. The strongest limit was received for the class of Gigahertz Peaked / Compact Steep Spectrum sources (GPS/CSS), E ν 2 dN ν /dE ν | GPS 〈 8.2⋅10 −12 GeV/s/sr per source, assuming an E ν −2 -shaped spectrum. This corresponds to an improvement of a factor of 2.5 compared with the average point source limit for single sources.

Description: Solar particle event analysis using the standard radiation environment monitors: applying the neutron monitor's experience Astrophysics and Space Sciences Transactions, 7, 1-5, 2011 Author(s): A. Papaioannou, H. Mavromichalaki, M. Gerontidou, G. Souvatzoglou, P. Nieminen, and A. Glover The Standard Radiation Environment Monitor (SREM) is a particle detector developed by the European Space Agency for satellite applications with the main purpose to provide radiation hazard alarms to the host spacecraft. SREM units have been constructed within a radiation hardening concept and therefore are able to register extreme solar particle events (SPEs). Large SPEs are registered at Earth, by ground based detectors as neutron monitors, in the form of Ground Level Enhancements of solar cosmic rays. In this work, a feasibility study of a possible radiation alert, deduced by SREM measurements was implemented for the event of 20 January 2005. Taking advantage of the neutron monitor's experience, the steps of the GLE alert algorithm were put into practice on SREM measurements. The outcome was that SREM units did register the outgoing SPE on-time and that these could serve as indicators of radiation hazards, leading to successful alerts.

Description: Cosmic-ray energy spectrum around the knee observed with the Tibet air-shower experiment Astrophysics and Space Sciences Transactions, 7, 15-20, 2011 Author(s): M. Amenomori, X. J. Bi, D. Chen, S. W. Cui, Danzengluobu, L. K. Ding, X. H. Ding, C. Fan, C. F. Feng, Zhaoyang Feng, Z. Y. Feng, X. Y. Gao, Q. X. Geng, Q. B. Gou, H. W. Guo, H. H. He, M. He, K. Hibino, N. Hotta, Haibing Hu, H. B. Hu, J. Huang, Q. Huang, H. Y. Jia, L. Jiang, F. Kajino, K. Kasahara, Y. Katayose, C. Kato, K. Kawata, Labaciren, G. M. Le, A. F. Li, H. C. Li, J. Y. Li, C. Liu, Y.-Q. Lou, H. Lu, X. R. Meng, K. Mizutani, J. Mu, K. Munakata, H. Nanjo, M. Nishizawa, M. Ohnishi, I. Ohta, S. Ozawa, T. Saito, T. Y. Saito, M. Sakata, T. K. Sako, M. Shibata, A. Shiomi, T. Shirai, H. Sugimoto, M. Takita, Y. H. Tan, N. Tateyama, S. Torii, H. Tsuchiya, S. Udo, B. Wang, H. Wang, Y. Wang, Y. G. Wang, H. R. Wu, L. Xue, Y. Yamamoto, C. T. Yan, X. C. Yang, S. Yasue, Z. H. Ye, G. C. Yu, A. F. Yuan, T. Yuda, H. M. Zhang, J. L. Zhang, N. J. Zhang, X. Y. Zhang, Y. Zhang, Yi Zhang, Ying Zhang, Zhaxisangzhu, and X. X. Zhou The energy spectrum of cosmic rays around the knee measured by Tibet air-shower experiment is summarized and its characteristic features are discussed under two possible scenarios. The result of Tibet experiment measured over wide range of 10 14 –10 17 eV with high statistics provided details of the knee at the energy around 4×10 15 eV. The study of the chemical composition based on measurements of proton and helium spectra obtained from air-shower core detection indicates the dominance of heavy nuclei around the knee. Such feature can be explained either by contribution of nearby sources with source composition dominated by heavy nuclei or by nonlinear effect in diffusive shock acceleration mechanism.

Description: Simulation of Charged Particle Diffusion in MHD plasmas Astrophysics and Space Sciences Transactions, 7, 21-27, 2011 Author(s): F. Spanier and M. Wisniewski Magnetohydrodynamical simulations of turbulent plasmas have been performed to study the transport of energetic test particles. Several parameters of the underlying MHD simulation have been varied to gain insight into the main processes governing transport. Here also the distinct effects of wave-particle resonance and field line wandering shall be studied.

Description: A new modular cosmic-ray detector Astrophysics and Space Sciences Transactions, 7, 11-14, 2011 Author(s): F. Signoretti and M. Storini Comparing the mean features of helium proportional counters with the ones of the standard boron trifluoride tubes, it appears at glance that, in equal term of efficiency and for the same active length, the 3 He filled counters are characterized by a very smaller diameter which optimizes their spectral resolution and minimizes wall effects. Moreover helium counters are usually designed in standard diameters and the 2 inch size is commonly available in a wide set of sensitive lengths. This manufacturing characteristic suggested us the realization of a modular neutron detector with a variable geometry to be adapted to counters of different lengths. At first a small modular detector (length of 80 cm) was assembled in Rome at SVIRCO Observatory and TPL during 2006. In March 2010 a second larger modular neutron monitor (length of 216 cm) was realized as well to be used for cosmic ray registration with a higher counting rate and better reliability. A short description of both modular cosmic-ray detectors is given.

Description: Understanding cosmic rays and searching for exotic sources with PAMELA Astrophysics and Space Sciences Transactions, 7, 85-91, 2011 Author(s): P. Picozza, R. Sparvoli, and the "PAMELA collaboration" The instrument PAMELA, in orbit since 15~June 2006 on board of the Russian satellite Resurs DK1, is designed to study charged particles in the cosmic radiation, with a particular focus on antimatter and signals of dark matter annihilation. PAMELA is also looking for primordial antinuclei, measuring light nuclei energy spectra, studying the mechanisms of acceleration and propagation of the cosmic rays in the Galaxy, and monitoring the solar activity and the radiation belts. A review of the main experimental results obtained by PAMELA is presented in this paper. The observed anomalous positron excess is discussed in terms of annihilation of dark matter particles as well as in terms of standard astrophysical sources. Moreover constraints on dark matter models from antiproton data are shown.

Description: Cosmic ray physics with the ARGO-YBJ experiment Astrophysics and Space Sciences Transactions, 7, 131-136, 2011 Author(s): A. Surdo (on behalf of the ARGO-YBJ Collaboration) The main scientific goals of the ARGO-YBJ experiment are γ-ray astronomy with a few hundreds GeV energy threshold and cosmic ray physics below and around the knee of the primary energy spectrum (10 12 –10 16 eV), where the transition from direct to indirect measurement techniques takes place. The ARGO-YBJ experiment, located at the Cosmic Ray Observatory of Yangbajing (Tibet, P.R. of China, 4 300 m a.s.l.), is an unconventional Extensive Air Shower array of about 6,700 m 2 of active area, the only one exploiting the full-coverage technique at very high altitude currently in operation. The detector space-time granularity, performance and location offer a unique chance to make a detailed study of the structure of cosmic ray showers, in particular of the hadronic component. In this work we will focus on the main experimental results concerning cosmic ray and hadronic interaction physics: primary cosmic ray energy spectrum, antiproton over proton ratio, anisotropy in the cosmic ray flux and proton-air cross-section. Moreover, the possible data analysis improvements based on the use of all detailed information on the shower front (curvature, time width, rise time, ..), as well as the extension of the investigable energy range, allowed by the analog RPC readout, will be pointed out.

Description: Cosmic ray physics in space: the role of Sergey Vernov's scientific school Astrophysics and Space Sciences Transactions, 7, 151-156, 2011 Author(s): M. I. Panasyuk Cosmic rays were discovered almost 100 years ago. Since then the scientific world has learned a lot from their nature: the particles nascent in the Universe, both in our Galaxy and outside, the basic mechanisms of their acceleration, transfer in the interstellar environment and the interaction of the primary cosmic rays with the atmosphere surrounding the Earth. Before 1957, i.e., the beginning of the Space Era, researchers' capabilities were limited to experiments performed on the ground, underground and in near-ground atmosphere to flight altitudes of aerostats, airplanes and rockets, i.e., where only secondary radiation is in existence, this is the result of the interaction of cosmic rays with the Earth's atmosphere. The launching of spacecraft allowed the scientists to commence exploring the Universe's primordial matter itself outside the atmosphere, i.e., the primary cosmic rays. Sergey Vernov, the Russian scientist, was among them.

Description: The IceCube neutrino observatory: status and initial results Astrophysics and Space Sciences Transactions, 7, 157-162, 2011 Author(s): T. Karg 1 for the IceCube collaboration * The IceCube collaboration is building a cubic kilometer scale neutrino telescope at a depth of 2 km at the geographic South Pole, utilizing the clear Antarctic ice as a Cherenkov medium to detect cosmic neutrinos. The IceCube observatory is complemented by IceTop, a square kilometer air shower array on top of the in-ice detector. The construction of the detector is nearly finished with 79 of a planned 86 strings and 73 of 80 IceTop stations deployed. Its completion is expected in the winter 2010/11. Using data from the partially built detector, we present initial results of searches for neutrinos from astrophysical sources such as supernova remnants, active galactic nuclei, and gamma ray bursts, for anisotropies in cosmic rays, and constraints on the dark matter scattering cross section. Further, we discuss future plans and R&D (research and development) activities towards new neutrino detection techniques.

Description: The focal surface of the JEM-EUSO instrument Astrophysics and Space Sciences Transactions, 7, 167-169, 2011 Author(s): Y. Kawasaki, M. Casolino, P. Gorodetzky, A. Santangelo, M. Ricci, F. Kajino, T. Ebisuzaki, and the JEM-EUSO collaboration The Extreme Universe Space Observatory on JEM/EF (JEM-EUSO) is a space mission to study extremely high-energy cosmic rays. The JEM-EUSO instrument is a wide-angle refractive telescope in the near-ultraviolet wavelength region which will be mounted to the International Space Station. Its goal is to measure time-resolved fluorescence images of extensive air showers in the atmosphere. In this paper we describe in detail the main features and technological aspects of the focal surface of the instrument. The JEM-EUSO focal surface is a spherically curved surface, with an area of about 4.5 m 2 . The focal surface detector is made of more than 5000 multi-anode photomultipliers (MAPMTs). Current baseline is Hamamatsu R11265-03-M64. The approach to the focal surface detector is highly modular. Photo-Detector-Modules (PDM) are the basic units that drive the mechanical structure and data acquisition. Each PDM consists of 9 Elementary Cells (ECs). The EC, which is the basic unit of the MAPMT support structure and of the front-end electronics, contains 4 units of MAPMTs. In total, about 1 200 ECs or about 150 PDMs are arranged on the whole of the focal surface of JEM-EUSO.

Description: Measurements and interpretation of registration of large number of neutrons generated in lead: the role of particle cascades Astrophysics and Space Sciences Transactions, 7, 101-104, 2011 Author(s): Z. Dębicki, K. Jędrzejczak, J. Karczmarczyk, M. Kasztelan, R. Lewandowski, J. Orzechowski, B. Szabelska, J. Szabelski, P. Tokarski, and T. Wibig We register events with large number of neutrons at the ground level as well as in the underground laboratory. These neutrons are produced in secondary cosmic ray interactions with matter surrounding the neutron detectors. We used the set of helium-3 filled gas proportional counters and plastic scintillators. We performed a series of measurements in different experimental setups to determine a role of particle cascades in generation of large neutron multiplicities. With GEANT4 simulation of experimental setup we estimated number of neutrons produced in a single event which is required to explain our measurements.

Description: Large scale anisotropy studies with the Pierre Auger Observatory Astrophysics and Space Sciences Transactions, 7, 125-129, 2011 Author(s): M. Grigat 1 for the Pierre Auger Collaboration 2 The Pierre Auger Observatory in Argentina measures air showers initiated by cosmic rays at EeV energy scales (1 EeV = 10 18 eV). An important goal of the collaboration is to study the distribution of arrival directions of the primary particles and quantify potential anisotropies therein. Using data collected by the surface detector (SD) array of the Pierre Auger Observatory since 1 January 2004, we study large scale anisotropies in different energy windows. Modulations of the event rate within the period of a sidereal day are studied by means of a periodicity analysis accounting for local effects which may induce an artificial anisotropy. We present results for the event rate modulation in right ascension and derive upper limits for the equatorial component of a dipole amplitude (Auger Coll., 2011; Bonino, 2009).

Description: Do we see an 'Iron Peak' ? Astrophysics and Space Sciences Transactions, 7, 145-150, 2011 Author(s): A. D. Erlykin and A. W. Wolfendale An update of the fine structure in the cosmic ray (CR) energy spectrum at PeV and tens of PeV energies is presented. The existence of the bump at 50–80 PeV found in the GAMMA experiment is supported by 9 other experiments. If it is a real feature it might indicate the existence of the so called 'Iron Peak', i.e. the end of the contribution of a 'Single Source' to the background of CR from other sources. We argue that the new feature in the fine structure of the CR energy spectrum makes the evidence in favour of the presence of a 'Single Source' stronger than before.

Description: Scientific activity of academician Sergei Vernov in Apatity (Kola Peninsula) and Leningrad during the years 1968–1982 Astrophysics and Space Sciences Transactions, 7, 137-144, 2011 Author(s): V. A. Dergachev This paper is dedicated to the 100th birthday anniversary of academician S. N. Vernov. Academician Sergei Vernov (1910–1982), an outstanding Russian space physicist, was the first national scientist who initiated the cosmic ray programme and radiation studies onboard the first Soviet artificial satellites. He initiated the holding of All-Union conferences, seminars and winter schools on space physics and was the chairman of these events.

Description: A mobile detector for measurements of the atmospheric muon flux Astrophysics and Space Sciences Transactions, 7, 163-166, 2011 Author(s): B. Mitrica, I. M. Brancus, R. Margineanu, M. Petcu, M. Dima, O. Sima, A. Haungs, H. Rebel, M. Petre, G. Toma, A. Saftoiu, and A. Apostu Measurements of the underground atmospheric muon flux are important in order to determine accurately the overburden in mwe (meter water equivalent) of an underground laboratory for appreciating which kind of experiments are feasible for that location. Slanic- Prohava is one of the 7 possible locations for the European large underground experiment LAGUNA (Large Apparatus studying Grand Unification and Neutrino Astrophysics). A mobile device consisting of 2 scintillator plates (≈0.9 m 2 , each) one above the other and measuring in coincidence, was set-up for determining the muon flux. The detector it is installed on a van which facilitates measurements on different positions at the surface or in the underground and it is in operation since autumn 2009. The measurements of muon fluxes presented in this contribution have been performed in the underground salt mine Slanic-Prahova, Romania, where IFIN-HH has built a low radiation level laboratory, and at the surface on different sites of Romania, at different elevations from 0 m a.s.l up to 655 m a.s.l. Based on our measurements we can say that Slanic site is a feasible location for LAGUNA in Unirea salt mine at a water equivalent depth of 600 mwe. The results have been compared with Monte-Carlo simulations performed with the simulation codes CORSIKA and MUSIC.

Description: Study of EAS neutron component temporal structure Astrophysics and Space Sciences Transactions, 7, 115-117, 2011 Author(s): D. M. Gromushkin, A. A. Petrukhin, Yu. V. Stenkin, and I. I. Yashin The neutron component of Extensive Air Showers (EAS) carries information about the primary cosmic ray flux as well as about parameters of hadronic interactions at ultra-high energies. We present here the data obtained with the "Neutron" array which is a prototype of a novel type EAS array PRISMA (Stenkin, 2009). The prototype consists of 5 large area scintillator detectors (0.75 m 2 each) placed in the corners and in the center of 5 m side square. The scintillator consisting of an alloy of ZnS(Ag) and 6 LiF is shaped as a thin layer of grains covered with thin transparent plastic film.

Description: Possible structure in the cosmic ray electron spectrum measured by the ATIC-2 and ATIC-4 experiments Astrophysics and Space Sciences Transactions, 7, 119-124, 2011 Author(s): A. D. Panov, V. I. Zatsepin, N. V. Sokolskaya, J. H. Adams Jr., H. S. Ahn, G. L. Bashindzhagyan, J. Chang, M. Christl, T. G. Guzik, J. Isbert, K. C. Kim, E. N. Kouznetsov, M. I. Panasyuk, E. B. Postnikov, E. S. Seo, J. Watts, J. P. Wefel, and J. Wu A strong excess in a form of a wide peak in the energy range of 300–800 GeV was discovered in the first measurements of the electron spectrum in the energy range from 20 GeV to 3 TeV by the balloon-borne experiment ATIC (Chang et al., 2008b). The experimental data processing and analysis of the electron spectrum with different criteria for selection of electrons, completely independent of the results reported in Chang et al. (2008b) is employed in the present paper. The new independent analysis generally confirms the results of Chang et al. (2008b), but shows that the spectrum in the region of the excess is represented by a number of narrow peaks. The measured spectrum is compared to the spectrum of Chang et al. (2008b) and to the spectrum of the Fermi/LAT experiment.

Description: Underground multi-muon experiment EMMA Astrophysics and Space Sciences Transactions, 7, 93-96, 2011 Author(s): P. Kuusiniemi, L. Bezrukov, T. Enqvist, H. Fynbo, L. Inzhechik, P. Jones, J. Joutsenvaara, T. Kalliokoski, J. Karjalainen, K. Loo, B. Lubsandorzhiev, T. Monto, V. Petkov, T. Räihä, J. Sarkamo, M. Slupecki, W.H. Trzaska, and A. Virkajärvi EMMA is a new experiment designed for cosmic-ray composition studies around the knee energy operating at the shallow depth underground in the Pyhäsalmi mine, Finland. The array has sufficient coverage and resolution to determine the multiplicity, the lateral density distribution and the arrival direction of high-energy muons on an event by event basis. Preliminary results on the muon multiplicity extracted using one detector station of the array are presented.

Description: Search for high energy gamma-ray bursts Astrophysics and Space Sciences Transactions, 7, 97-100, 2011 Author(s): V. B. Petkov, A. S. Pozanenko, V. M. Loznikov, A.N. Gaponenko, M. V. Andreev, and A.V. Sergeev We report results of the search for high energy GRBs and high energy radiation in correlation with GRBs. The search has been performed at "Andyrchy" EAS array, for this purpose the single particle counting rate of the array has been used. The data were collected during 1996 – 2006 years with a live time 2290 days.

Description: Radiation doses along selected flight profiles during two extreme solar cosmic ray events Astrophysics and Space Sciences Transactions, 7, 105-109, 2011 Author(s): R. Bütikofer and E. O. Flückiger The radiation dose rates at flight altitudes may be hazardously increased during solar cosmic ray events. Within the scope of this paper we investigate the total accumulated radiation doses, i.e. the contribution of galactic and solar cosmic rays, during the two extreme solar cosmic ray events on 29 September 1989 and on 20 January 2005 along selected flight profiles. In addition, the paper discusses the consequences of possible solar cosmic ray flux approximations on the results of the radiation dose computations.

Description: Study of the primary spectrum and composition around the knee at the Andyrchy-BUST experiment Astrophysics and Space Sciences Transactions, 7, 111-114, 2011 Author(s): V. B. Petkov and J. Szabelski The experimental data of the Andyrchy-BUST experiment are presented. The three types of experimental data, taken in our experiment, have been analyzed: high energy muon number spectrum, EAS size spectrum and dependence of the mean number of high energy muons on EAS size. Joint analysis of these experimental data have been used for both studying the primary composition and testing interaction models.

Description: Measurement of the charge ratio of atmospheric muons with the CMS detector Astrophysics and Space Sciences Transactions, 7, 79-83, 2011 Author(s): A. Calderón for the CMS Collaboration We present a measurement of the ratio of positive to negative muon fluxes from cosmic ray interactions in the atmosphere, using data collected by the CMS detector both at ground level and in the underground experimental cavern at the CERN LHC. Muons were detected in the momentum range from 5 GeV/c to 1 TeV/c. The surface flux ratio is measured to be 1.2766 ± 0.0032 (stat.) ± 0.0032 (syst.), independent of the muon momentum, below 100 GeV/c. This is the most precise measurement to date. At higher momenta the data are consistent with an increase of the charge ratio, in agreement with cosmic ray shower models and compatible with previous measurements by underground experiments.

Description: Results from the Telescope Array Experiment Astrophysics and Space Sciences Transactions, 7, 257-263, 2011 Author(s): D. Ikeda 1 for the Telescope Array collaboration * The Telescope Array experiment is the largest hybrid detector to observe ultra-high energy cosmic rays in the northern hemisphere. The observation started in November 2007 for Fluorescence Detector (FD) and in March 2008 for Surface Detectors (SD). Here we present the preliminary results of energy spectra measured by three different methods, mass composition, photon search and AGN correlation search from the Telescope Array. The energy spectra measured by the Middle-Drum FD station, which is the refurbished detector of the High Resolution Fly's Eye (HiRes) experiment, and hybrid technique with two new FDs and SD were consistent with the result of HiRes. The systematic error of the energies in hybrid measurement is 19%. The SD spectrum showed the suppression above 10 19.75 eV with 3.5σ away from the continuous spectrum. The measured mass composition with stereo technique of new FDs was consistent with pure proton model between 10 18.6 eV to 10 19.3 eV. Photon search resulted in an improved flux limit above 10 19 eV. The result of AGN correlation from TA was consistent with background.

Description: Antiproton modulation in the Heliosphere and AMS-02 antiproton over proton ratio prediction Astrophysics and Space Sciences Transactions, 7, 245-249, 2011 Author(s): P. Bobik, M. J. Boschini, C. Consolandi, S. Della Torre, M. Gervasi, D. Grandi, K. Kudela, S. Pensotti, and P. G. Rancoita We implemented a quasi time-dependent 2-D stochastic model of solar modulation describing the transport of cosmic rays (CR) in the heliosphere. Our code can modulate the Local Interstellar Spectrum (LIS) of a generic charged particle (light cosmic ions and electrons), calculating the spectrum at 1 AU. Several measurements of CR antiparticles have been performed. Here we focused our attention on the CR antiproton component and the antiproton over proton ratio. We show that our model, using the same heliospheric parameters for both particles, fit the observed p / p ratio. We show a good agreement with BESS-97 and PAMELA data and make a prediction for the AMS-02 experiment.

Description: Gamma ray bursts monitoring with the ARGO-YBJ experiment in scaler mode Astrophysics and Space Sciences Transactions, 7, 239-243, 2011 Author(s): T. Di Girolamo, P. Vallania, and C. Vigorito We report on the search for Gamma Ray Bursts (GRBs) in the energy range 1–100 GeV in coincidence with the prompt emission detected by satellites, using the Astrophysical Radiation Ground-based Observatory at YangBaJing (ARGO-YBJ). With its big active surface (~6700 m 2 ) and large field of view (≥2 sr) the ARGO-YBJ air shower detector is particularly suitable to detect unpredictable and short duration events such as GRBs. The search has been performed using the single particle technique in time coincidence with satellite detections both for single events and for the piling up of all the GRBs in time and in phase. Between November 2004 and June 2010 115 GRBs, detected by different satellites (mainly Swift and Fermi), occurred within the field of view of ARGO-YBJ. For 94 of these we searched for a counterpart in the ARGO-YBJ data finding no statistically significant emission. Search methods and results are discussed.

Description: The depth of maximum shower development and its fluctuations: cosmic ray mass composition at E 0 ≥10 17 eV Astrophysics and Space Sciences Transactions, 7, 251-255, 2011 Author(s): S. P. Knurenko and A. Sabourov We present new data on Cherenkov light observations obtained during 1994–2009 period, after a modernization of the Yakutsk EAS array. A complex analysis of x max and its fluctuations σ( x max ) was performed in a wide energy range. With the new data, according to QGSJet II model, an estimation was made of cosmic rays mass composition for E 0 ~10 17 –3×10 19 eV. The result points towards a mixed composition with a large portion of heavy nuclei at E 0 ~10 17 eV and the dominance of light nuclei at E 0 ~10 19 eV. The analysis of σ x max energy dependence for the same energies qualitatively confirms this result. A shape of x max distribution at fixed energy 10 18 eV is analysed to make more precise conclusion on cosmic ray mass composition.

Description: New measuring system of multipurpose Cherenkov water detector NEVOD Astrophysics and Space Sciences Transactions, 7, 271-273, 2011 Author(s): S. S. Khokhlov, M. B. Amelchakov, V. V. Ashikhmin, V. G. Gulyi, I. S. Kartsev, V. V. Kindin, K. G. Kompaniets, M. A. Korolev, A. A. Petrukhin, I. A. Shulzhenko, V. V. Shutenko, I. A. Vorobiev, I. I. Yashin, and E. A. Zadeba The purposes, tasks and design features of the new measuring system of the Cherenkov water detector NEVOD are discussed.

Description: An evaluation of electron-photon cascades developing in matter, photon and magnetic fields Astrophysics and Space Sciences Transactions, 7, 345-350, 2011 Author(s): T. Nakatsuka, A. Iyono, and J. Nishimura Electromagnetic cascades in matter, photon fields, and magnetic fields are solved by a standard numerical method, integrating the diffusion equations of respective cascade processes numerically. Our results and those of Aharonian and Plyasheshnikov agree very well for cascades in matter and magnetic fields, though they show some slight discrepancies for cascades in photon fields of high incident energies. Transport properties of electron and photon spectra are also investigated by solving differential-difference equations for cascades with simplified cross-sections, and the spectra under the electron cooldown process are well explained quantitatively.

Description: The northern site of the Pierre Auger Observatory Astrophysics and Space Sciences Transactions, 7, 319-325, 2011 Author(s): M. Kleifges The Pierre Auger Observatory studies cosmic ray extensive air showers with energies at and above the EeV range with a hybrid instrument consisting of a surface detector array and air fluorescence telescopes. Science results obtained with the southern observatory located near Malargüe, Province of Mendoza, Argentina, are the driving force to build a second observatory in southeast Colorado (USA) in the rural environment of Lamar. This Auger North Observatory will focus on measurements in the highest energy range above 50 EeV with the highest possible acceptance. As a consequence of the different energy range of the southern and northern sites, the designs of the instruments are different in some aspects. We present the proposed Auger North layout, the changes in the design of the detectors, and the current site activities with the Research and Development Array (RDA).

Description: Cosmic ray composition studies through the Gerasimova-Zatsepin effects of heavy nuclei at LAAS Astrophysics and Space Sciences Transactions, 7, 327-333, 2011 Author(s): A. Iyono, H. Matsumoto, K. Okei, S. Tsuji, S. Ohara, N. Ochi, T. Konishi, N. Takahashi, I. Yamamoto, T. Nakatsuka, T. Nakamura, N. Ohmori, and K. Saitoh Extensive air showers (EASs) originated from primary cosmic ray energies above 10 15 eV have been measured at multiple EAS observatories deployed in Japan since Sept. 1996. The typical EAS array has been located at the rooftop of the buildings in the university campus, and has GPS-disciplined 10 MHz oscillator to provide the UTC time stamp for each EAS event within a few μs accuracies. Searching for simultaneous and parallel EAS events at multiple EAS observatories due to Gerasimova-Zatsepin (GZ) effects have been carried out by comparing EAS arrival time stamps and directions detected by several baseline combinations of EAS arrays. The EAS pairs whose time difference and angular distance were less than 5 ms and less than 15° respectively, were selected and their angular distances from the solar direction and the lunar direction were examined. The data were compared with numerical GZ probability as a function of arrival directions of cosmic ray nuclei. Consequently, significant excesses of these events in the solar direction as expected in the numerical prediction of GZ effects were not found. We however found that the deficiencies of EAS pairs in the lunar direction, but its deviation is not significant.

Description: Linsley's EAS time structure method for the primary cosmic ray spectrum at LAAS Astrophysics and Space Sciences Transactions, 7, 335-344, 2011 Author(s): A. Iyono, H. Matsumoto, K. Okei, S. Tsuji, S. Ohara, N. Ochi, T. Konishi, N. Takahashi, I. Yamamoto, T. Nakatsuka, T. Nakamura, N. Ohmori, and K. Saito We have installed a shift register system of extensive air show (EAS) particles in a compact EAS array built on the rooftop of the Faculty of Engineering building in the campus of Okayama University of Science and being operated since April 2006 as part of Large Area Air Shower (LAAS) experiments , in order to register each arrival time of EAS particles within 5 μs. Detector simulations based on the database obtained from one of the standard cosmic ray propagation simulator in the atmosphere (AIRES) have also been carried out and the procedures to estimate the primary cosmic ray energy from the Linsley's method have been developed and examined. Applying Linsley's method to the EAS data obtained by our EAS arrays and the simulation results, we derived the energy spectrum from 10 16 eV to 10 19.5 eV. Consequently, we obtained the power-law index of −3.2 (+0.46−0.8) in the primary energy range of 10 16 eV to 10 18.5 eV, and obtained that a change around 10 18 eV appeared if not taking account of the zenith angle distribution of primary cosmic rays. We compared the obtained energy spectrum with other experimental data above 10 16 eV energies, and showed the two components of power-law energy spectra well described our data. We also showed the improvement of energy resolution by applying the restriction of zenith angle of primary cosmic rays in our simulation results, as well as the potential of the Linsley's method with a compact EAS array.

Description: NOY: a neutrino observatory network project based on stand alone air shower detector arrays Astrophysics and Space Sciences Transactions, 7, 369-372, 2011 Author(s): F. Montanet, D. Lebrun, J. Chauvin, E. Lagorio, and P. Stassi We have developed a self powered stand alone particle detector array dedicated to the observation of horizontal tau air showers induced by high energy neutrinos interacting in mountain rock. Air shower particle detection reaches a 100% duty cycle and is practically free of background when compared to Cherenkov light or radio techniques. It is thus better suited for rare neutrino event search. An appropriate mountain to valley topological configuration has been identified and the first array will be deployed on an inclined slope at an elevation of 1500 m facing Southern Alps near the city of Grenoble (France). A full simulation has been performed. A neutrino energy dependent mountain tomography chart is obtained using a neutrino and tau propagation code together with a detailed cartography and elevation map of the region. The array acceptance is then evaluated between 1 PeV and 100 EeV by simulating decaying tau air showers across the valley. The effective detection surface is determined by the shower lateral extension at array location and is hence much larger than the array geometrical area. The array exposure will be 10 14 cm 2 sr s at 100 PeV. Several independent arrays can be deployed with the aim of constituting a large distributed observatory. Some other sites are already under study. At last, special care is dedicated to the educational and outreach aspects of such a cosmic ray detector.

Description: Hadrons with energies of E h 〉 50 MeV in EAS with N e = 10 5 –10 7 Astrophysics and Space Sciences Transactions, 7, 365-367, 2011 Author(s): D. D. Dzhappuev, Yu. V. Balabin, B. B. Gvozdevskii, N. F. Klimenko, A. U. Kudzhaev, O. I. Mikhailova, V. B. Petkov, and E. V. Vashenyuk The characteristics of hadrons with E h 〉 50 MeV in EAS have been obtained. The measurements were performed at the CARPET-2 extensive air shower array. For showers with E 0 〉 6 · 10 13 eV the duration of hadronic cascade in NM has been estimated. The dependence of the mean neutron multiplicity in the neutron monitor on the total number of the change particles for EAS with N e = 10 5 –10 7 at a distance of 17–30 m from EAS axis has been measured.

Description: Constraints on long-term changes in solar activity from the range of variability of cosmogenic radionuclide records Astrophysics and Space Sciences Transactions, 7, 355-364, 2011 Author(s): R. Muscheler and U. Heikkilä There is a variety of different cosmogenic radionuclide-based reconstructions of solar activity variations for the past. Especially the longer-term changes and the absolute levels of past solar activity are uncertain as it is illustrated by the differences between these reconstructions. On the one hand there are differences between 10 Be and 14 C records that are commonly used as proxies for the varying solar modulation of galactic cosmic rays. On the other hand estimates of past changes in the geomagnetic shielding also include relatively large uncertainties. Here, we concentrate on variations in cosmogenic radionuclide records on time scales of 50 to 500 yr. We show that these are to a large extent independent of the geomagnetic field intensity. The range of variability of cosmogenic radionuclide records allows us to set constraints about long-term changes in solar activity. These records indicate that present solar activity levels were reached or exceeded regularly in the past.

Description: MHD simulation of the evolution of shock structures in the solar corona: implications for coronal shock acceleration Astrophysics and Space Sciences Transactions, 7, 387-394, 2011 Author(s): J. Pomoell, R. Vainio, and R. Kissmann We have employed magnetohydrodynamic (MHD) simulations to study the dynamics of shocks in a solar minimum-like corona caused by an erupting coronal mass ejection (CME). Our simulations show that a highly non-trivial evolution of the shock properties on coronal field lines occurs even for simple coronal conditions. By comparing with recent test particle simulations of an evolving coronal shock employing a simplified shock model, we qualitatively assess the possibility of the shocks given by the MHD simulations to produce energetic particles. Our conclusion is that the evolution of parameters most crucial to particle acceleration at shocks, such as the compression ratio and obliquity, need to be more accurately taken into account in models and simulations of particle acceleration than has been customary, so far.

Description: A method to constrain the characteristic angular size of the brightest cosmic-ray sources observed above 57 × 10 18 eV Astrophysics and Space Sciences Transactions, 7, 403-410, 2011 Author(s): P. W. Younk We introduce a method to constrain the characteristic angular size of the brightest cosmic-ray sources observed above 57 × 10 18 eV. By angular size of a source, we mean the effective angular extent over which cosmic-rays from that source arrive at earth. The method is based on the small-scale (

Description: Lower limits on the lifetime of massive neutrino radiative decay from the 2006 total solar eclipse Astrophysics and Space Sciences Transactions, 7, 419-423, 2011 Author(s): V. Popa We report on the search for signatures of possible neutrino radiative decays, in occasion of the 2006 total solar eclipse (TSE). The lower lifetime limits obtained in the hypothesis of normal mass hierarchy ( m 3 〉〉 m 2 〉 m 1 ) are about 3 orders of magnitude better than the previous results. The inverted mass hierarchy scenario ( m 2 〉 m 1 〉〉 m 3 ) is also investigated. The reached sensitivity suggests that the limits presented here are the best obtainable using this technique.

Description: Multiple scattering measurement with laser events Astrophysics and Space Sciences Transactions, 7, 383-386, 2011 Author(s): P. Assis, R. Conceição, P. Gonçalves, M. Pimenta, B. Tomé, and the Pierre Auger Collaboration The Pierre Auger Observatory Fluorescence Detector (FD) performs a calorimetric measurement of the primary energy of cosmic ray showers. The level of accuracy of this technique is determined by the uncertainty in several parameters, among them the fraction of shower light (both from fluorescence and Cherenkov light) that reaches the detector after being multiply scattered (MS) in the atmosphere. This component depends on atmospheric conditions, namely on Rayleigh and Mie scattering processes. Using laser events it is possible to study these processes and deconvolute them from the shower's electromagnetic lateral distribution. We propose a new method to measure the Rayleigh and Mie MS components seen in laser events, and correlate them with atmospheric conditions. In order to study in detail the effect of such conditions in the scattering of photons, a Geant4 dedicated laser simulation was developed. % In this framework photons are individually followed through the atmosphere allowing for any number of scatterings, from both processes This combination of a MS dedicated data analysis with a realistic laser simulation enables to explore MS characteristics, in particular the evolution with time, altitude and distance from the FD.

Description: Cosmic rays in the stratosphere in 2008–2010 Astrophysics and Space Sciences Transactions, 7, 379-382, 2011 Author(s): Y. I. Stozhkov, N. S. Svirzhevsky, G. A. Bazilevskaya, M. B. Krainev, A. K. Svirzhevskaya, V. S. Makhmutov, V. I. Logachev, and E. V. Vashenyuk The experimental data on the galactic cosmic ray fluxes obtained from the measurements in the atmosphere during the period 2008–2010 are presented. They include the unusual long-term period of the low solar activity. In 2009, we recorded the highest cosmic ray fluxes (particles with energy more than 0.2 GeV) in the history of the cosmic particle measurements. The reasons for the extremely low solar modulation of galactic cosmic ray (GCR) fluxes are briefly discussed.

Description: Solar variability and width of tree ring Astrophysics and Space Sciences Transactions, 7, 395-401, 2011 Author(s): Y. Muraki, K. Masuda, K. Nagaya, K. Wada, and H. Miyahara The relationship between solar activity and the global climate is not only an academically interesting problem but also an important subject for human beings. We have found an interesting relation that may be connected with above profound problem. We have analyzed the tree rings that had survived for 391 years in Japan. The tree archive is very important since it includes the period of the Maunder minimum. Quite surprisingly, Fourier analyses of the annual growth rate identified two cycles with periodicities of 12 and 25 years during the Maunder minimum, but no such cycles were found for other time periods. Possible interpretations of this result are presented.

Description: Corrigendum to "Linsley's EAS time structure method for the primary cosmic ray spectrum at LAAS" published in Astrophys. Space Sci. Trans., 7, 335–344, 2011 Astrophysics and Space Sciences Transactions, 7, 417-417, 2011 Author(s): A. Iyono, H. Matsumoto, K. Okei, S. Tsuji, S. Ohara, N. Ochi, T. Konishi, N. Takahashi, I. Yamamoto, T. Nakatsuka, T. Nakamura, N. Ohmori, and K. Saito No abstract available.

Description: The effect of cosmic rays on biological systems – an investigation during GLE events Astrophysics and Space Sciences Transactions, 8, 7-17, 2012 Author(s): N. K. Belisheva, H. Lammer, H. K. Biernat, and E. V. Vashenuyk In this study, first direct and circumstantial evidences of the effects of cosmic rays (CR) on biological systems are presented. A direct evidence of biological effects of CR is demonstrated in experiments with three cellular lines growing in culture during three events of Ground Level Enhancement (GLEs) in the neutron count rate detected by ground-based neutron monitor in October 1989. Various phenomena associated with DNA lesion on the cellular level demonstrate coherent dynamics of radiation effects in all cellular lines coincident with the time of arrival of high-energy solar particles to the near-Earth space and with the main peak in GLE. These results were obtained in the course of six separate experiments, with partial overlapping of the time of previous and subsequent experiments, which started and finished in the quiet period of solar activity (SA). A significant difference between the values of multinuclear cells in all cellular lines in the quiet period and during GLE events indicates that the cause of radiation effects in the cell cultures is an exposure of cells to the secondary solar CR near the Earth's surface. The circumstantial evidence was obtained by statistical analysis of cases of congenital malformations (CM) at two sites in the Murmansk region. The number of cases of all classes of CM reveals a significant correlation with the number of GLE events. The number of cases of CM with pronounced chromosomal abnormalities clearly correlates with the GLE events that occurred a year before the birth of a child. We have found a significant correlation between modulations of the water properties and daily background variations of CR intensity. We believe that the effects of CR on biological systems can be also mediated by fluctuations in water properties, considered as one of possible mechanisms controlling the effects of CRs on biological systems.

Description: Observation of solar energetic particle (SEP) events associated with narrow CMEs Astrophysics and Space Sciences Transactions, 8, 1-5, 2012 Author(s): A. Al-Sawad, H. Allawi, W. Al-Ramdhan, and E. Valtonen We report here on two proton energetic particle events observed by the Energetic and Relativistic Nuclei and Electron (ERNE) instrument on the Solar and Heliospherical Observatory (SOHO). Both events were impulsive (SEP) events with intensities of 〉10 −3 cm −2 sr −1 s −1 MeV −1 at an energy range of tens of MeVs and were associated with CMEs of angular widths 800 kms −1 . In one of the events there was no associated solar flare, which indicates that the first injected protons were completely due to the associated CME and in the second event the associated solar flare was an impulsive M1.1 class flare and the calculated first injection time for protons of energies ~36 MeV and propagating along 1.2 AU path length, was close to the liftoff time of the CME. These observations are inconsistent with the view presented in some studies that narrow fast CME are not associated with SEP events.

Description: TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field ASTRA Proceedings, 1, 65-71, 2014 Author(s): P. Desiati and A. Lazarian Cosmic rays are observed to possess a small non uniform distribution in arrival direction. Such anisotropy appears to have a roughly consistent topology between tens of GeV and hundreds of TeV, with a smooth energy dependency on phase and amplitude. Above a few hundreds of TeV a sudden change in the topology of the anisotropy is observed. The distribution of cosmic ray sources in the Milky Way is expected to inject anisotropy on the cosmic ray flux. The nearest and most recent sources, in particular, are expected to contribute more significantly than others. Moreover the interstellar medium is expected to have different characteristics throughout the Galaxy, with different turbulent properties and injection scales. Propagation effects in the interstellar magnetic field can shape the cosmic ray particle distribution as well. In particular, in the 1–10 TeV energy range, they have a gyroradius comparable to the size of the Heliosphere, assuming a typical interstellar magnetic field strength of 3 μG. Therefore they are expected to be strongly affected by the Heliosphere in a manner ordered by the direction of the local interstellar magnetic field and of the heliotail. In this paper we discuss on the possibility that TeV cosmic rays arrival distribution might be significantly redistributed as they propagate through the Heliosphere.

Description: Lyman-α observations of astrospheres ASTRA Proceedings, 1, 43-49, 2014 Author(s): J. L. Linsky and B. E. Wood Charge-exchange reactions between outflowing stellar wind protons and interstellar neutral hydrogen atoms entering a stellar astrosphere produce a region of piled-up-decelerated neutral hydrogen called the hydrogen wall. Absorption by this gas, which is observed in stellar Lyman-α emission lines, provides the only viable technique at this time for measuring the mass-loss rates of F–M dwarf stars. We describe this technique, present an alternative way for understanding the relation of mass-loss rate with X-ray emission, and identify several critical issues.

Description: MHD flows at astropauses and in astrotails ASTRA Proceedings, 1, 51-60, 2014 Author(s): D. H. Nickeler, T. Wiegelmann, M. Karlický, and M. Kraus The geometrical shapes and the physical properties of stellar wind – interstellar medium interaction regions form an important stage for studying stellar winds and their embedded magnetic fields as well as cosmic ray modulation. Our goal is to provide a proper representation and classification of counter-flow configurations and counter-flow interfaces in the frame of fluid theory. In addition we calculate flows and large-scale electromagnetic fields based on which the large-scale dynamics and its role as possible background for particle acceleration, e.g., in the form of anomalous cosmic rays, can be studied. We find that for the definition of the boundaries, which are determining the astropause shape, the number and location of magnetic null points and stagnation points is essential. Multiple separatrices can exist, forming a highly complex environment for the interstellar and stellar plasma. Furthermore, the formation of extended tail structures occur naturally, and their stretched field and streamlines provide surroundings and mechanisms for the acceleration of particles by field-aligned electric fields.

Description: Effects of stellar evolution and ionizing radiation on the environments of massive stars ASTRA Proceedings, 1, 61-63, 2014 Author(s): J. Mackey, N. Langer, S. Mohamed, V. V. Gvaramadze, H. R. Neilson, and D. M.-A. Meyer We discuss two important effects for the astrospheres of runaway stars: the propagation of ionizing photons far beyond the astropause, and the rapid evolution of massive stars (and their winds) near the end of their lives. Hot stars emit ionizing photons with associated photoheating that has a significant dynamical effect on their surroundings. 3-D simulations show that H ii regions around runaway O stars drive expanding conical shells and leave underdense wakes in the medium they pass through. For late O stars this feedback to the interstellar medium is more important than that from stellar winds. Late in life, O stars evolve to cool red supergiants more rapidly than their environment can react, producing transient circumstellar structures such as double bow shocks. This provides an explanation for the bow shock and linear bar-shaped structure observed around Betelgeuse.

Description: Numerical modeling of relativistic particle shock acceleration Astrophysics and Space Sciences Transactions, 7, 287-294, 2011 Author(s): A. Meli The shock acceleration mechanism is invoked to explain non-thermal cosmic rays in Supernova Remnants, Active Galactic Nuclei and Gamma Ray Bursts jets. Especially, the importance of relativistic shock acceleration in extragalactic sources is a recurring theme raising a significant interest in the research community. We will briefly overview the shock acceleration mechanism and we will address the properties of non-relativistic and relativistic shocks, particularly focusing on relativistic simulation studies.

Description: Fine structure of neutron multiplicity on neutron monitors Astrophysics and Space Sciences Transactions, 7, 283-286, 2011 Author(s): Yu. V. Balabin, B. B. Gvozdevsk, E. A. Maurchev, E. V. Vashenyuk, and D. D. Dzhappuev Based on a huge data set acquired with a unique recording system, multiplicity events M  =4–50 on a neutron monitor have been analyzed in detail. The multiplicity events are recorded in detail for the first time, their structure being examined. The multiplicity processes in a neutron monitor have been numerically simulated by a toolkit GEANT4. Analysis of neutron monitor data with high temporal and spatial resolution reveals that most multiplicity events involving more than three adjacent counter tubes are due to local hadronic air showers with characteristic dimensions of size 1–3 m and duration of ~1 ms.

Description: Strong variations of cosmic ray intensity during thunderstorms and associated pulsations of the geomagnetic field Astrophysics and Space Sciences Transactions, 7, 279-282, 2011 Author(s): K. Kh. Kanonidi, N. S. Khaerdinov, A. S. Lidvansky, and L. E. Sobisevich Strong variations of the intensity of secondary cosmic rays during thunderstorms are found to be accompanied in some cases by very clear pulsations of the geomagnetic field. The experiment is carried out in the Baksan Valley, North Caucasus, the Carpet air shower array being used as a particle detector. Magnetic field measurements are made with high-precision magnetometers located deep underground in the tunnel of the Baksan Neutrino Observatory, several kilometers apart from the air shower array.

Description: Cosmic rays in the knee energy range Astrophysics and Space Sciences Transactions, 7, 295-301, 2011 Author(s): A. Haungs In the energy range of the so called 'knee' between 100 TeV and 1 EeV one expects to identify the end of the galactic origin of cosmic rays. Only for the lowest energies a direct detection with instruments on high-altitude, long-flying balloons are possible. Measurements of the high-energy particles are performed indirectly via the detection of extensive air showers by extended arrays of particle or Cherenkov light sensitive detectors. Multidimensional analyses of the air shower data indicate a distinct knee in the energy spectra of light primary cosmic rays at few PeV and an increasing dominance of heavy ones towards higher energies. This provides implications for discriminating astrophysical models of the origin of the knee and of the physics of the transition from galactic to extragalactic cosmic ray origin. Where around 1 PeV many experiments were in operation and have given valuable results in the last decade, at higher energies there was a lack of experimental efforts. To improve the reconstruction quality and statistics at energies from 10 to 1000 PeV, where the transition can be expected, presently several experiments are in operation or going to be in operation. First results of these experiments, as well as perspectives of future efforts in this energy range will be discussed.

Description: Background radioactivity in the scaler mode technique of the Argo-YBJ detector Astrophysics and Space Sciences Transactions, 7, 311-314, 2011 Author(s): I. Bolognino, C. Cattaneo, E. Giroletti, G. Liguori, and P. Salvini ARGO-YBJ is an extensive air shower detector located at the Yangbajing Cosmic Ray Laboratory (4300 m a.s.l., 606 g cm −2 atmospheric depth, Tibet, China). It is made by a single layer of Resistive Plate Chambers (RPCs, total surface ~6700 m 2 ) grouped into 153 units called "clusters". The low energy threshold of the experiment is obtained using the "scaler operation mode", counting all the particles hitting the detector without reconstruction of the shower size and arrival direction. For each cluster the signals generated by these particles are put in coincidence in a narrow time window (150 ns) and read by four independent scaler channels, giving the counting rates of channel ≥1, ≥2, ≥3 and ≥4 hits. The study of these counting rates pointed out a different behavior of channel ≥1 respect to the higher multiplicity channels: while the MC simulations can account fairly well for the coincident counting rates, the expectation for channel ≥1 is sensibly less than the measured value. Moreover, the regression coefficient with the atmospheric pressure for channel ≥1 is also about half of the value measured for the coincident counting rates: seemingly half of these counts did not cross the atmosphere.Measurements of the natural radioactivity background in the air of the detector hall and a MC simulation to estimate its contribution on our counting rates are presented and discussed.

Description: Forbush decreases – clouds relation in the neutron monitor era Astrophysics and Space Sciences Transactions, 7, 315-318, 2011 Author(s): A. Dragić, I. Aničin, R. Banjanac, V. Udovičić, D. Joković, D. Maletić, and J. Puzović The proposed influence of cosmic rays on cloud formation is tested for the effect of sudden intensity changes of CR (Forbush decreases) on cloudiness. An attempt is made to widen the investigated period covered by satellite observation of cloudiness. As an indicator of cloud cover, the diurnal temperature range (DTR - a quantity anticorrelated with cloudiness) is used. The superposed epoch analysis on a set of isolated Forbush decreases is conducted and the results for a region of Europe are presented. The effect of Forbush decrease on DTR is statistically significant only if the analysis is restricted to high amplitude FDs (above the threshold value of 7% with the respect to undisturbed CR intensity). The magnitude of the effect on DTR is estimated to be (0.38 ± 0.06) °C.

Description: Developments in shower reconstruction and composition analysis for CARPET-3 EAS array Astrophysics and Space Sciences Transactions, 7, 307-310, 2011 Author(s): J. Sarkamo, V. B. Petkov, D. D. Dzhappuev, N. F. Klimenko, and T. Raiha This contribution describes the current progress on the composition analysis of data recorded with Carpet EAS detector. The focus of the paper is on the methodological side of analysis.

Description: New measurements of cosmic ray air showers with the digital radio interferometer LOPES Astrophysics and Space Sciences Transactions, 7, 303-306, 2011 Author(s): F. G. Schröder, W. D. Apel, J. C. Arteaga, T. Asch, L. Bähren, K. Bekk, M. Bertaina, P. L. Biermann, J. Blümer, H. Bozdog, I. M. Brancus, P. Buchholz, S. Buitink, E. Cantoni, A. Chiavassa, K. Daumiller, V. de Souza, P. Doll, R. Engel, H. Falcke, M. Finger, D. Fuhrmann, H. Gemmeke, C. Grupen, A. Haungs, D. Heck, J. R. Hörandel, A. Horneffer, D. Huber, T. Huege, P. G. Isar, K.-H. Kampert, D. Kang, O. Krömer, J. Kuijpers, S. Lafebre, K. Link, P. Łuczak, M. Ludwig, H.J. Mathes, M. Melissas, C. Morello, S. Nehls, J. Oehlschläger, N. Palmieri, T. Pierog, J. Rautenberg, H. Rebel, M. Roth, C. Rühle, A. Saftoiu, H. Schieler, A. Schmidt, O. Sima, G. Toma, G. C. Trinchero, A. Weindl, J. Wochele, M. Wommer, J. Zabierowski, and J. A. Zensus LOPES is a digital radio interferometer which measures the radio emission of extensive cosmic ray air showers. It mainly consists of 30 dipole antennas installed in co-location with KASCADE-Grande at the Karlsruhe Institute of Technology (KIT) in Germany. KASCADE-Grande measures the secondary air shower particles at ground. Whenever KASCADE-Grande detects a high-energy cosmic ray event (≳10 16 eV), it triggers LOPES which then digitally records the radio signal in the frequency band from 40 to 80 MHz. Using interferometric methods, LOPES is able to successfully detect air shower induced radio pulses, even in the noisy environment at the KIT. In the present studies, a considerable progress in understanding the radio emission mechanism is shown: The latest version of the "radio emission in air shower" simulation program, REAS3, seems to be the first Monte Carlo tool which is able to reproduce the magnitude and slope of most of the measured lateral distributions.

Description: Three dimensional model of the interplanetary magnetic field and 27-day variation of the galactic cosmic ray intensity Astrophysics and Space Sciences Transactions, 7, 351-354, 2011 Author(s): A. Wawrzynczak, R. Modzelewska, and M. V. Alania We present a model of the 27-day variation of the galactic cosmic ray (GCR) intensity for three dimensional (3-D) heliosphere with the heliolongitudinal and heliolatitudinal dependent radial solar wind speed for the period of 1995 – minimum epoch of solar activity ( A 〉0). In the present model we implement heliolongitudinal asymmetry of solar wind velocity reproducing as the sum of first and second harmonics depending on the heliolatitudes and the regular part of the solar wind velocity ( V 0 ) changing versus heliolatitudes in accord to in situ measurements of the Ulysses spacecraft. We show that the range of changes of the sum of the first and second harmonics of the 27-day variation of the GCR intensity for Kiel neutron monitor is little less than expected from the modelling, however, they are comparable.