BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Intermediate GRBs as observed by various satellite experiments DTSTART;VALUE=DATE-TIME:20161011T104500Z DTEND;VALUE=DATE-TIME:20161011T110000Z DTSTAMP;VALUE=DATE-TIME:20260814T161843Z UID:indico-contribution-98-760@cern.ch DESCRIPTION:Speakers: Irene ARKHANGELSKAJA (National Research Nuclear Univ ersity MEPhI (Moscow Engineering Physics Institute))\nUsually two GRBs gro ups separated in duration distribution: short and long. These types events classified due analysis of duration of interval which the integrated coun ts from the GRB raise from $5\\%$ to $95\\%$ ($t_{90}$). The value $t_{90} ~\\sim~2$s used as boundary between short and long events. Firstly GRB dur ation distribution was analysed on data of BATSE experiment onboard the (C GRO) Compton Gamma Ray Observatory ($\\sim ~2700$ bursts) operated from Ap ril 1991 until to June 2000. However in 1999 third burst subgroup (interme diate GRBs) was found due GRBs duration and duration-hardness distribution s analysis of 4B current BATSE catalogue (recently available as 5B one) in interval 1~s~$\\le t_{90} \\le 40$~s.\n\nSince CGRO operation finished fi ve satellite experiments GRBs catalogues (Wind\, Suzaku\, RHESSI\, Swift/B AT and Fermi/GBM) contain sufficient amount of bursts for duration distrib ution precision investigation. The results of these distributions analysis are discussed. It allows concluding the appearance of intermediate GRB su bgroup on data of six experiments: BATSE/CGRO\, Wind\, Suzaku\, RHESSI\, S wift/BAT and Fermi/GBM.\n\nhttps://indico.particle.mephi.ru/event/4/contri butions/760/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/760/ END:VEVENT BEGIN:VEVENT SUMMARY:Investigations of CME in muon flux detected in hodoscopic mode DTSTART;VALUE=DATE-TIME:20161011T111500Z DTEND;VALUE=DATE-TIME:20161011T113000Z DTSTAMP;VALUE=DATE-TIME:20260814T161843Z UID:indico-contribution-98-666@cern.ch DESCRIPTION:Speakers: Ivan Astapov (National Research Nuclear University M EPhI (Moscow Engineering Physics Institute))\nCoronal mass ejections (CME) have an impact on the flux of cosmic rays that penetrate the space around us. Unlike most ground-based cosmic ray detectors\, muon hodoscope URAGAN (MEPhI) allows to investigate both the integrated counting rate of regist ered particles and the spatial and angular characteristics of the muon flu x at the ground level. This approach to particle detection allows to fix c hanges in the flux of cosmic rays not only for geoeffective CMEs but also for non-geoeffective ones. The results of the study of different types of CMEs at different stages of the 24 solar cycle are presented.\n\nhttps://i ndico.particle.mephi.ru/event/4/contributions/666/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/666/ END:VEVENT BEGIN:VEVENT SUMMARY:Plasma Focus for Laboratory Simulation of Astrophysical Jets. DTSTART;VALUE=DATE-TIME:20161011T110000Z DTEND;VALUE=DATE-TIME:20161011T111500Z DTSTAMP;VALUE=DATE-TIME:20260814T161843Z UID:indico-contribution-98-643@cern.ch DESCRIPTION:Speakers: Ilya Kalashnikov (National Research Nuclear Universi ty MEPhI)\nOne of the most interesting properties of astrophysical jets is that they propagates along the axis of rotation of the accretion disk on the distances\, which are many times greater than its diameter. \n\nUsing $Z$-Pinch facilities for laboratory simulation of astrophysical jets seems very logical. The Plasma focus is supposed to be a very suitable device f or simulation of astrophysical jets. \n\nResults of MHD simulations of jet propagation and its compare with known properties of the laboratory and y oung stellar object's jets are presented.\n\nhttps://indico.particle.mephi .ru/event/4/contributions/643/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/643/ END:VEVENT BEGIN:VEVENT SUMMARY:Energy characteristics of Forbush decreases accompanied by magneti c storms according to muon hodoscope URAGAN data DTSTART;VALUE=DATE-TIME:20161011T113000Z DTEND;VALUE=DATE-TIME:20161011T114500Z DTSTAMP;VALUE=DATE-TIME:20260814T161843Z UID:indico-contribution-98-610@cern.ch DESCRIPTION:Speakers: Elena Yakovleva (National Research Nuclear Universit y (MEPhI))\nMuon hodoscope URAGAN operates in MEPhI since 2006 and allows to register muons at various zenith angles. In this work\, the experimenta lly obtained temporal changes of the index of amplitude spectrum of Forbus h decreases registered by muon hodoscope URAGAN are studied. To obtain the Forbush decrease amplitude energy spectrum in the flux of muons\, the cal culated coupling functions of primary and secondary cosmic ray fluxes for five zenith-angular intervals are used. Analysis of the energy characteris tics is based on the dependence of the decrease amplitude in the intensity of cosmic ray muons on the mean log energy of primary particles\, which i nfluence to the change in the counting rate of the muon hodoscope URAGAN d uring Forbush decrease. Distributions of values of amplitude spectrum inde x of Forbush decreases accompanied by magnetic storms at different stages of their development are obtained. It is shown that the energy characteris tics of Forbush decreases accompanied by magnetic storms are different for various values of the geomagnetic indices.\n\nhttps://indico.particle.mep hi.ru/event/4/contributions/610/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/610/ END:VEVENT BEGIN:VEVENT SUMMARY:Multiband observations of the Crab Nebula DTSTART;VALUE=DATE-TIME:20161011T103000Z DTEND;VALUE=DATE-TIME:20161011T104500Z DTSTAMP;VALUE=DATE-TIME:20260814T161843Z UID:indico-contribution-98-492@cern.ch DESCRIPTION:Speakers: Alexander Krassilchtchikov (A.F. Ioffe Institute for Physics and Technology)\nThe results of simultaneous imaging of the Crab Nebula in the radio (JVLA)\,\noptical (HST ACS and WFC3)\, and X-ray (Chan dra) bands are presented. \nThe images show a variety of small-scale emitt ing structures\, including wisps\nmainly located to the north-west of the pulsar and knots forming a ring-like structure\nusually associated with th e termination shock of the pulsar wind.\n\nhttps://indico.particle.mephi.r u/event/4/contributions/492/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/492/ END:VEVENT BEGIN:VEVENT SUMMARY:Testing cascade models of extragalactic gamma-ray propagation usin g observations of extreme TeV blazars with imaging Cherenkov telescopes DTSTART;VALUE=DATE-TIME:20161011T101500Z DTEND;VALUE=DATE-TIME:20161011T103000Z DTSTAMP;VALUE=DATE-TIME:20260814T161843Z UID:indico-contribution-98-487@cern.ch DESCRIPTION:Speakers: Emil Khalikov (SINP MSU)\nRecent observations made b y imaging Cherenkov telescopes have found a pile-up in the TeV region of s ome blazar spectra in the optically thick regions (optical depth in this c ase is the measure of absorption of primary gamma rays on extragalactic ba ckground light (EBL) due to the γγ→e+e- process). This pile-up is not consistent with the predictions of the commonly-used models which include only absorption of primary photons and adiabatic losses. We believe that t his “anomaly” may be accounted for if certain mechanisms such as elect romagnetic (EM) cascade development are taken into consideration.\n The re are three distinct regimes of cascade development depending on the ener gy of the incident particle. If this energy is high enough\, then there ar e several generations of cascade particles and the observable spectrum is practically independent of the energy and type (electron/photon) of the pr imary particle but it depends on the distance to the source (the so-called universal regime). If that energy is comparatively low\, the number of ge nerations decreases and the spectrum becomes dependent on both energy and type of the primary particle (one-generation regime). The third possible r egime is the “extreme Klein-Nishina regime” in which electrons transfe r most of their energy to the background photons via inverse Compton scatt ering process (this regime may take place at ultrahigh energies of primary photons\, E>1 EeV). In our work we\, for the first time\, consider in det ail the “one-generation regime”\, the universal regime and the transit ion between them.\n In this talk we will mainly focus on the so-called hadronic cascade models\, in which primary protons create secondary photon s by means of pair-production and photopion processes and these photons\, in turn\, initiate EM cascades. We will compare the results obtained in ha dronic and electromagnetic cascade models (in the latter primary particles are photons instead of protons) and provide formal best fits for these mo dels to the widely available data from the HESS and VERITAS experiments (w hich has never been done before). The sample of observations used in our w ork includes 6 blazars with hard spectra. In addition to that\, to calcula te observable spectra for the case of hadronic models\, we will introduce a fast and reasonably accurate hybrid method using a large pre-computed da tabase of cascades from primary electrons and photons.\n We also\, for the first time\, consider a possibility that the beam of primary protons i s affected by an intervening galaxy clusters near the source and on the wa y from the source to the observer. For the first case\, we perform a detai led statistical analysis for the case of blazar 1ES 0229+200 using the emi ssion model of Tavecchio (2013) and show that this model is excluded with significance > 5σ unless the magnetic field strength near the source of p rotons is much lower than 100 nG. Finally\, we show that the intermediate cluster may significantly affect both shape and normalization of the obser vable spectrum.\n\nhttps://indico.particle.mephi.ru/event/4/contributions/ 487/ LOCATION:Milan Hotel Verdi URL:https://indico.particle.mephi.ru/event/4/contributions/487/ END:VEVENT END:VCALENDAR