BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Hybrid method for identifying mass groups of primary cosmic rays i n the joint operation of IACTs and wide angle Cherenkov timing arrays DTSTART;VALUE=DATE-TIME:20161010T140000Z DTEND;VALUE=DATE-TIME:20161010T141500Z DTSTAMP;VALUE=DATE-TIME:20260814T161137Z UID:indico-contribution-89-791@cern.ch DESCRIPTION:Speakers: Evgeny Postnikov (SINP MSU)\nThe mass composition of cosmic rays in the hundreds of TeV energy range is purely measured and un certain\, because primary cosmic rays measurements on satellites require s a large area of detectors\, but energy is too low for application of me thods developed for EAS measurements. In this paper we consider a possib ility to use the hybrid method originally aimed to gamma hadron separati on in TAIGA experimrnt\, to distinguish the diffrent mass groups among c osmic rays in the energy range 100 TeV- 500 TeV. The international gamma- observatory TAIGA (Tunka Advanced Instrument for cosmic rays and Gamma-Ast ronomy) is intended for ultra high energy gamma-ray astronomy (>30 TeV). I t aims at combining the cost-effective timing-array technique with IACTs\, allowing to reach a total area up to a few square kilometers and strong s uppressing hadron background because of a very precise angular resolution (order of 0.1 degrees at the energy >100 TeV). Hybrid operation of both of these techniques can lead to a relatively cheap way of development of a l arge area array. \n\nWe analyze Hillas’s parameters of images produced by different nuclei in IACT together with known arrival direction and show er core position\, measured by Hiscore timing arrays. We show that hybrid method can be very effective for this task.\n\nhttps://indico.particle.me phi.ru/event/4/contributions/791/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/791/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for diffuse gamma radiation with energy Eγ > 100 TeV at th e “Carpet-3” array DTSTART;VALUE=DATE-TIME:20161010T141500Z DTEND;VALUE=DATE-TIME:20161010T143000Z DTSTAMP;VALUE=DATE-TIME:20260814T161137Z UID:indico-contribution-89-777@cern.ch DESCRIPTION:Speakers: Aleksahdr Kudzhaev (Baksan Neutrino Observatory\,INR of RAS)\nStudying diffuse gamma-ray emission with energies higher than 10 0 TeV has become especially topical due to detection of astrophysical neut rinos in the IceCube experiment. If these neutrinos are a result of decays of charged pions\, neutral pions of the same energy should exist\, and th eir decays must generate considerable flux of gamma rays with energies abo ve 0.1 PeV. In order to confirm these expectations\, one should carry out new high-precision experiments in this energy range. An experiment for mea suring the flux of gamma rays with energy above 100 TeV is currently being prepared at the Baksan Neutrino Observatory (the Carpet-3 experiment). St ep-by-step increase of area of the muon detector of the Carpet air shower array is planned in this experiment. We present some results of calculatio ns of selection efficiency of air showers from primary gamma rays for diff erent configurations of the array. It is demonstrated that by increasing t he muon detector area up to 615 m^2 (the maximum possible value) one can r each with the Carpet-3 the world-best sensitivity to 100 TeV gamma rays.\n \nhttps://indico.particle.mephi.ru/event/4/contributions/777/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/777/ END:VEVENT BEGIN:VEVENT SUMMARY:The Impact of Standard Neutrino Processes into Positron and Antipr oton Fluxes DTSTART;VALUE=DATE-TIME:20161010T134500Z DTEND;VALUE=DATE-TIME:20161010T140000Z DTSTAMP;VALUE=DATE-TIME:20260814T161137Z UID:indico-contribution-89-644@cern.ch DESCRIPTION:Speakers: Anastasia Shitova (Yaroslavl P.G. Demidov State Univ ersity)\nThe possibility of the contribution from standard neutrino proces ses to \nthe total secondary positron and antiproton fluxes detected by \n contemporary experiments is analyzed in details. The results show that \nt he considered impact is negligible that confirms once more a necessity \no f application a new physics beyond the standard conceptions. The \ndesigne d technique could be implied to the further studies that is \nextremely in teresting in the light of the results of the recent \nexperiments in high energy cosmic ray physics such as PAMELA and AMS-02.\n\nhttps://indico.par ticle.mephi.ru/event/4/contributions/644/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/644/ END:VEVENT BEGIN:VEVENT SUMMARY:The process of splitting a photon in a strong magnetic field with taking account of the positronium influence on the photon dispersion DTSTART;VALUE=DATE-TIME:20161010T133000Z DTEND;VALUE=DATE-TIME:20161010T134500Z DTSTAMP;VALUE=DATE-TIME:20260814T161137Z UID:indico-contribution-89-639@cern.ch DESCRIPTION:Speakers: Anatoly Mosichkin (Yaroslavl State P.G. University)\ nWe study the process of splitting a photon in a strong magnetic field wit h taking account of the positronium influence on the photon dispersion. Th e positronium contribution into the photon polarization oprator leads to an essential modification of the photon dispersion law\, and of the photon decay amplitude. It has been shown that the probability of the photon dec ay changes under an influence of the positronium on the photon dispersion. \n\nhttps://indico.particle.mephi.ru/event/4/contributions/639/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/639/ END:VEVENT BEGIN:VEVENT SUMMARY:Nonlocal relativistic diffusion (NoRD) model of galactic cosmic ra y propagation DTSTART;VALUE=DATE-TIME:20161010T124500Z DTEND;VALUE=DATE-TIME:20161010T130000Z DTSTAMP;VALUE=DATE-TIME:20260814T161137Z UID:indico-contribution-89-633@cern.ch DESCRIPTION:Speakers: Renat Sibatov (Ulyanovsk State University)\nMost of the modern calculations of galactic cosmic-ray (GCR) propagation are based on the local diffusion model acceptable for the Brownian motion (BM) of a heavy particle through the system of uniformly distributed uncorrelated ( i.e. non-interacting) molecules. However\, about 60 years ago it has been found that the BM model is unable to adequately describe the diffusion in turbulent media [1-3]. Without doubt\, interstellar medium belongs to this class. For this reason\, the nonlocal transport theory based on fractiona l calculus is developed in [4]. The series of calculations performed to 20 10 confirmed the effectiveness of the approach\, improved parameters and led eventually to involving the relativistic speed limit [5]. The obtained model was described in [5\,6] and called NoRD in [7].\n\nIn this work\, t he key parameters of the NoRD model are obtained by specifying the Kolmogo rov spectra of turbulence near the inertial interval edges. This specifica tion leads to tempered power law distributions of free path lengths. The f ractional differential operators are modified into their tempered generali zations. We coordinate energy dependent diffusion coefficient and truncati on factor. For energies small enough for interested temporal and spatial s cales\, diffusion is normal. Extrapolating this dependence on large energi es\, we observe superdiffusive motion and tendency to ballistic motion. No RD propagators are calculated and analyzed. Under basic assumptions about the GCR origin\, the relativistic principle of maximum speed of propagatio n leads to the steepening of the equilibrium spectrum at energies close to the observed `knee'. In frames of the NoRD-model\, we estimate the role o f the local sources and the mass composition at PeV-energies.\n\n1. Monin A.S.\, Yaglom A.M. Statistical fluid mechanics\, Vol.II: mechanics of turb ulence\, 1965. \n2. Heisenberg W. Proc Roy. Soc\, A195 (1948) 402. (1948) .\n3. Tchen C. M. Physical Review 93 (1954) 4.\n4. Lagutin A.A.\, Nikulin Y.A.\, Uchaikin V.V. Nuclear Physics B-Proceedings Supplements 97 (2001) 2 67.\n5. Uchaikin V. V. JETP letters 91 (2010) 105.\n6. Uchaikin V.V. Physi cs-Uspekhi 56 (2013) 1074.\n7. Uchaikin V. V.\, Sibatov R. T. IJARSET 11 ( 2015) 1081.\n\nhttps://indico.particle.mephi.ru/event/4/contributions/633/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/633/ END:VEVENT BEGIN:VEVENT SUMMARY:Identification of high-energy antiprotons on electrons background based on calorimeter data in PAMELA experiment DTSTART;VALUE=DATE-TIME:20161010T131500Z DTEND;VALUE=DATE-TIME:20161010T133000Z DTSTAMP;VALUE=DATE-TIME:20260814T161137Z UID:indico-contribution-89-517@cern.ch DESCRIPTION:Speakers: Olga Dunaeva (Aleksandrovna)\nIn modern experimental physics a heterogeneous coordinate-sensitive calorimeters are widely used due to their good characteristics and possibilities to obtain a three-dim ensional information of particles interactions. Espesially it is important at high-energies when electromagnetic or hadronic showers are arise. We p ropose a quit efficient method to identify antiprotons (positrons) with en ergies more than 10 GeV on electron (proton) background by calorimeter of such kind. We construct the AdaBoost classifier to separate particles into two classes\, different combinations of energy release along reconstructe d particle trajectorywere used as feature vector. We test\na preliminary v erson of the method on a calorimeter of the PAMELA magnetic spectrometer. For high-energy particles we got a good quality of classification: it lost only $4*10^{-4}$ of antiprotons\, while less than $10^{-3}$ of electrons were classified to antiproton class.\n\nhttps://indico.particle.mephi.ru/e vent/4/contributions/517/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/517/ END:VEVENT BEGIN:VEVENT SUMMARY:The spectrum of relativistic cosmic rays measurements and numerica l simulation DTSTART;VALUE=DATE-TIME:20161010T130000Z DTEND;VALUE=DATE-TIME:20161010T131500Z DTSTAMP;VALUE=DATE-TIME:20260814T161137Z UID:indico-contribution-89-498@cern.ch DESCRIPTION:Speakers: Alexander Podgorny (Lebedev Physical Institute RAS)\ nThe spectra of relativistic proton were obtained from measurements with t he worldwide network of neutron monitors. The relativistic protons appeare d after the flares occurring in the west side of the Sun disk arrive to th e Earth after time of flight $\\sim$15 min without collisions. This prompt anisotropic flux must bring information about spectrum of protons ejected from the solar cosmic ray source. The spectrum of prompt component of relativistic protons is exponential $\\sim e^{-E/E_{0}}$\, where ty pical $E_{0}$ is order of 0.5 GeV. After delay of 15 - 20 min the proton f lux becomes isotropic with power spectrum $E^{-\\gamma}$ where $\\gamma \\ sim 5$. Apparently\, beam instability is developed. The proton acceleratio n in the flare is numerically simulated. The MHD simulation of current she et creation before the flare is carried out. Initial and boundary conditio ns have been set using photospheric magnetic field measurements. No assump tion about solar flare mechanism is used. Appearance of a current sheet in the solar corona above the active region is proved by comparison of the c urrent sheet position obtained by MHD simulations and the position of obse rved flare thermal X-ray source. During a flare the magnetic field energy is transferred into the particle energy. The positions of current sheets o btained by MHD simulation above the active region NOAA 10365 are coincided with the positions of soft X-ray emission sources for flares M1.4 May 27\ , 2003 in 02:53 and X1.2 May 29\, 2003 in 00:51. Proton acceleration up to relativistic energy can occur in the electric field applied along the sin gular line in a current sheet. The electric field E = $-V \\times B/c$ is created due to the rate reconnection V. At typical V = $2 \\times 10^7$ cm /s the measured spectrum coincides with the calculated spectrum.\n\nhttps: //indico.particle.mephi.ru/event/4/contributions/498/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/498/ END:VEVENT END:VCALENDAR