BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:A new break near 10 TeV in the energy spectrum of protons accordin g to data from space-based instruments: astrophysical interpretation DTSTART;VALUE=DATE-TIME:20230629T070000Z DTEND;VALUE=DATE-TIME:20230629T071500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-254@indico.nevod.mephi.ru DESCRIPTION:Speakers: Anatoly Lagutin (Altai State University)\nRecent exp erimental data from space-based instruments of the DAMPE and CALET collabo rations have shown that the energy spectrum of protons has a new feature\, a break in the $\\sim 10$ TeV region. In this energy range\, the spectrum index of the observed particles varies from $-2.6$ to $-2.9$.\n\nThe purp ose of this work is to establish the location zone of the sources that det ermine this break\, the index of the proton generation spectrum in them\, as well as the astrophysical interpretation of the results obtained in the DAMPE and CALET experiments.\n\nWithin the framework of the model of nonc lassical diffusion of cosmic rays developed by the authors\, which has bre ak due to the propagation of particles in a sharply inhomogeneous (fractal type) galactic medium\, it is shown that break in this energy range is fo rmed by sources located at a distance of $300-400$ pc from the Earth. Thes e sources\, whose age is $\\sim (5-10)\\cdot 10^4$ years\, generate partic les with a spectrum index $\\sim 2.8$.\n\nThe power-law behavior of the pr oton spectrum before and after the break\, first obtained in the DAMPE and CALET experiments\, confirms the conclusion made earlier by the authors t hat cosmic ray diffusion is nonclassical. The results of these experiments should also be considered as an indication of the need to revise the stan dard paradigm accepted today about the sources of cosmic rays and the mech anisms of particle acceleration in them.\n\nhttps://indico.nevod.mephi.ru/ event/9/contributions/254/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/254/ END:VEVENT BEGIN:VEVENT SUMMARY:Energy deposit of EAS cores detected by the facilities of the Expe rimental Complex NEVOD DTSTART;VALUE=DATE-TIME:20230628T101500Z DTEND;VALUE=DATE-TIME:20230628T103000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-187@indico.nevod.mephi.ru DESCRIPTION:Speakers: Semyon Khokhlov (National Research Nuclear Universit y MEPhI)\nThe Experimental Complex (EC) NEVOD (MEPhI\, Moscow) includes th e NEVOD-EAS array\, detecting electron-photon component of extensive air s howers (EAS)\, and the Cherenkov water calorimeter (CWC)\, measuring energ y deposit of particles passing through its operating volume.\nReconstructi on of main EAS parameters (axis position\, arrival direction\, age and siz e) is performed according to the data of the NEVOD-EAS array\, the cluster s of which are installed around the building of the CWC. The System of Glo bal Time Synchronization of the EC NEVOD provides timestamping events dete cted by the NEVOD-EAS and CWC with an accuracy of up to 25 ns\, which make s it possible to select joint events in these facilities.\nIn this work\, from all joint events in the NEVOD-EAS and CWC\, we selected for the analy sis only those events in which the EAS cores passed through the volume of the water detector. Since EAS cores include different types of particles\, the response of CWC to electrons\, muons and hadrons of various energies has been simulated in the Geant4 software package. Based on simulation\, t he estimates of the contribution of various components to the total energy deposit of EAS cores have been obtained. In the report we present the res ults of comparing simulation with experimental data.\n\nhttps://indico.nev od.mephi.ru/event/9/contributions/187/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/187/ END:VEVENT BEGIN:VEVENT SUMMARY:Elaboration of a model of SPHERE-3 telescope for the studies of th e primary cosmic rays in 10^15 — 10^18 eV energy range using reflected from snowed surface and direct Cherenkov light from extensive air showers DTSTART;VALUE=DATE-TIME:20230627T124500Z DTEND;VALUE=DATE-TIME:20230627T130000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-221@indico.nevod.mephi.ru DESCRIPTION:Speakers: Elena Bonvech (SINP MSU)\nPaper contains the first r esults of our attempts in the development of a model of SPHERE-3 telescope for the primary cosmic ray studies in 1-1000 PeV energy range with reflec ted and direct Cherenkov light generated by extensive air showers (EAS).\n \nThe aim of the work is to develop an automated method for the design of SPHERE-3 telescope\, which\, on one hand\, will enable it to obtain the be st possible estimates of EAS primary parameters and\, on the other\, will result in a set of rules and recommendations on how to design other detect ors of the type.\n\nHandling of samples of Cherenkov light images accordin g to the available processing codes will give estimates of the uncertainti es of the primary parameters\, which integrally characterize the quality o f measurements with a given version of the telescope and the procedures fo r their processing. As a result\, the optimal version of the telescope wil l be selected and a general approach to the choice of its design and data processing algorithms will be developed.\n\nA preliminary version of the S PHERE-3 optical scheme is shown as a basis for further improvement and dev elopment of optimized optical schemes that will be combined with various s chemes of sensitive mosaics\, electronics\, trigger algorithm and off-line processing algorithms.\n\nThe description of the created database of arti ficial events of EAS with the generation of Cherenkov light for protons\, nitrogen and iron nuclei with energies in the range of 1-100 PeV and zenit h angles of 5-25 degrees according to two models of interaction and three models of the atmosphere is given.\n\nA scheme for calculating artificial images of reflected and direct EAS Cherenkov light on the mosaic of optica l sensors of the telescope is presented.\n\nhttps://indico.nevod.mephi.ru/ event/9/contributions/221/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/221/ END:VEVENT BEGIN:VEVENT SUMMARY:30 years of cosmic ray research in the Tunka Valley DTSTART;VALUE=DATE-TIME:20230627T080000Z DTEND;VALUE=DATE-TIME:20230627T083000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-240@indico.nevod.mephi.ru DESCRIPTION:Speakers: Nikolay Budnev (Irkutsk State University)\nA brief h istory and the main results of the study of cosmic rays and high-energy ga mma radiation using the Cherenkov EAS installations located in the Tunka V alley 50 km from the southwestern tip of Lake Baikal are presented. Since 1993\, the important results have been got about the energy spectrum and m ass composition of cosmic rays in the energy range of 1 – 1000 PeV with the Tunka-4\, Tunka-13\, Tunka-25\, Tunka-133 installations. The spectrum indicates a significantly more complex dependence of the intensity of cos mic rays on energy than previously assumed and serves as a natural bridge between the results obtained in experiments on satellites and balloon expe riments and the results of the giant international observatories Auger and Telescope Array.\n\nBased on the experience gained\, in 2014\, the creati on of a hybrid complex TAIGA was launched\, aimed at solving a lot of tas ks in the field of astroparticle physics\, cosmic ray physics and high-ene rgy gamma astronomy. In 2022\, the creation of the TAIGA-1 pilot complex w as completed\, including 120 low-threshold wide-angle Cherenkov stations d istributed over an area of 1.2 km ^ 2\, and three Imaging Atmospheric Cher enkov Telescopes. The report will present the first results of studies of high-energy gamma radiation from a number of sources.\n\nhttps://indico.ne vod.mephi.ru/event/9/contributions/240/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/240/ END:VEVENT BEGIN:VEVENT SUMMARY:Development of 10 sq.m hodoscope made of drift tubes for cosmic ra y muon registration DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-190@indico.nevod.mephi.ru DESCRIPTION:Speakers: Mikhail Barinov ()\nM.E.Barinov\, V.V.Biryukov\, A.A . Borisov\, S.V.Erin\, R.M. Fakhrutdinov\, A.P.Filin\, V.N.Gushchin\, A.N. Isaev\, A.S.Kozhin\, A.V.Larionov\, M.M.Soldatov\n\nThe 10 sq.m muon hodos cope made of drift tubes with length 3.7 m and diameter 52 mm is under dev elopment and construction in NRC “Kurchatov institute” – IHEP. Total ly 768 drift tubes are grouped into 6 identical multilayers\, each consist ing of two tube layers with parallelly placed tubes. Tube orientation in n eighbouring multilayers is orthogonal\, thus the hodoscope has six X and s ix Y tube layers. Detailed mechanical structure\, on-chamber electronic an d data acquisition systems are described. Expected technical characteristi cs and some test results are presented.\n\nKeywords: Muon hodoscope\, Trac k chamber\, Drift tube\, On-chamber electronics\, Data acquisition system. \n\nhttps://indico.nevod.mephi.ru/event/9/contributions/190/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/190/ END:VEVENT BEGIN:VEVENT SUMMARY:Study of cosmic ray variations in 2021-2022 based on the ENU scien tific complex data DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-248@indico.nevod.mephi.ru DESCRIPTION:Speakers: Aidar Morzabaev (L.N. Gumilyov Eurasion National Uni versity)\nThis work presents a comparative analysis of the time changes in the secondary cosmic ray fluxes recorded by the detector modules of the L .N. Gumilyov ENU scientific complex during the period of powerful geomagne tic disturbances on 04.11.2021 and 13-14.03.2022. Noticeable changes in th e geomagnetic indices\, solar wind plasma velocity and the potential gradi ent of the surface electric field were observed. The results of the analys is are presented\, the Forbush-decreasing effect is highlighted\, and the characteristics and features are considered.\nThe time intervals in 2021 f or which an increase in the particle flux relative to the background one w as also observed and registered by the ENU detectors. They are in possible association to electrified clouds\, lightning activity\, thunderstorms\, emission of natural radionuclides\, variations of the surface electric fi eld are discussed. The main features of each recorded event are considered . It’s shown that several increase events correlate with the dynamics of the surface electric field potential gradient.\nThis work supported by th e Program-Targeted Funding Program of the Ministry of Education and Scienc e of the Republic of Kazakhstan IRN BR10965191 "Integrated Research in Nuc lear and Radiation Physics\, High Energy Physics and Cosmology for the Dev elopment of Competitive Technologies".\n\nhttps://indico.nevod.mephi.ru/ev ent/9/contributions/248/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/248/ END:VEVENT BEGIN:VEVENT SUMMARY:High-frequency antenna cluster at the Tien Shan High-Mountain Scie ntific Station DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-259@indico.nevod.mephi.ru DESCRIPTION:Speakers: Saken Shinbulatov (KazNU al Farabi)\, Yerzhan Mukham ejanov (Joint Institute for Nuclear Research)\nAntenna clusters located in the Tien Shan High Mountaine Scientific Station (TSHMSS) are designed for radio detection of Extensive Air Showers (EAS) of cosmic rays. The cluste r consists of 4 radio antennas\, which each of them consists of mutually p erpendicular arcs distributed over an area of 1700 m2. The analog part of the measuring path consists of a SALLA type antenna. These high-frequency antennas of the ”SALLA" type were used in the Tunka-REX experiment\, ope rating in the frequency range of 30-80 MHz.\nThe antenna cluster works in conjunction with other installations to register SHAL. The cluster registe rs radio signals emitted by showers with energy above 10^15-10^16 eV. The purpose of the cluster is to investigate the possibilities of radio detect ion of the EAS\, at an altitude of 3440 m above sea level\, to determine t he energy and elemental composition of primary cosmic rays.\nPreliminary e xperimental data were obtained from the antenna cluster located at the Tie n Shan high-Mountain Scientific Station. The experimental data were compar ed with the data obtained as a result of modeling in the CORSIKA package. \n\nhttps://indico.nevod.mephi.ru/event/9/contributions/259/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/259/ END:VEVENT BEGIN:VEVENT SUMMARY:Project of a mobile muon hodoscope for muonography of various obje cts DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-245@indico.nevod.mephi.ru DESCRIPTION:Speakers: Maxim Tselinenko (Национальный иссл едовательский ядерный университет «МИФ И»)\nAt present\, the method of muonography (by analogy with X-ray radio graphy) of the internal structure of various objects of natural or artific ial origin using the natural flux of cosmic ray muons has become widesprea d. \nTo implement this method\, a mobile muon hodoscope (MMH) is being dev eloped at the NEVOD Scientific and Educational Center (MEPhI). The design of the MMH is a multichannel detecting system consisting of six single-pro jection planes with an active area of about 1 m2. Each single-projection p lane is an assembly of two layers of 96 scintillation strips in each layer with geometric dimensions of 10 × 7 × 1000 mm3 with light collection us ing wavelength-shifting optical fibers to silicon photomultipliers (SiPM). The layers are shifted by half of the width of the strip relative to each other and fixed between two aluminium sheets. 32 SiPM signals are transmi tted to an electronic reading system based on a 32-channel ASIC PETIROC 2A . Two adjacent single-projection planes are rotated relative to each other by 90 degrees. \nIn this report the features of the construction and regi stration system of MMH are discussed. The results of tests of a sample of a silicon photomultiplier\, as well as a prototype of a single-projection plane consisting of 32 scintillation strips are presented.\n\nhttps://indi co.nevod.mephi.ru/event/9/contributions/245/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/245/ END:VEVENT BEGIN:VEVENT SUMMARY:The possibility of detecting TeV electrons and positrons of galact ic cosmic rays using the Earth's magnetic field DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-262@indico.nevod.mephi.ru DESCRIPTION:Speakers: Alexandr Stuzhin ()\nVarious mechanisms for the prod uction and acceleration of positrons to energies of ∼ 10 GeV and above h ave been actively discussed since their excess in the PAMELA experiment wa s first detected. To test these theoretical models\, measurements of posit ron flux at energies of ∼ 1 TeV and above are necessary. However\, moder n methods of registering cosmic rays do not provide an opportunity to regi ster the fluxes of positrons and electrons separately. A promising techniq ue is to use synchrotron radiation of positrons and electrons in the Earth 's magnetic field to detect them. In this work we modeled the process of d etection of positrons and electrons by this technique in the TeV energy ra nge. Estimated registration efficiency for polar latitudes are 5-35% highe r than for equatorial latitudes. Using the experimental data of CALET\, DA MPE and FERMI on the total electron-positron flux of galactic cosmic rays\ , the expected integral detector count rate for the ROSS(Russian Orbital S ervice Station) and ISS(International Space Station) orbit in the energy r ange of 1-4.5 TeV was obtained. The high-latitude ROSS orbit provides a hi gher count rate. The possibility of measuring positron energies by registe ring synchrotron photons emitted by them was also investigated. The energy resolution was 35-45% depending on the positron energy and the minimum nu mber of detected photons.\n\nhttps://indico.nevod.mephi.ru/event/9/contrib utions/262/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/262/ END:VEVENT BEGIN:VEVENT SUMMARY:Tunka-Grande and TAIGA-Muon experiments: status\, results and pros pects DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-256@indico.nevod.mephi.ru DESCRIPTION:Speakers: Roman Monkhoev (API ISU)\nThe Tunka-Grande and TAIGA -Muon scintillation arrays are part of the TAIGA astrophysical complex. Th is complex is located in the Tunka Valley\, 50 km from Lake Baikal and is aimed at solving fundamental problems of cosmic ray physics and gamma-ray astronomy in the energy range 10 TeV - 1 EeV.\nIn report we present descri ption and status of arrays\, scientific programs and the main results of t he Tunka-Grande array based on 7 seasons of operation: CR energy spectrum and limit on the flux of the diffuse gamma rays in the energy range 10 PeV - 1000 PeV. In addition\, we provide the results of test operation of the first 3 clusters of the TAIGA-Muon array.\n\nhttps://indico.nevod.mephi.r u/event/9/contributions/256/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/256/ END:VEVENT BEGIN:VEVENT SUMMARY:A new method for searching for VHE muons in data from Cherenkov wa ter neutrino telescopes DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-232@indico.nevod.mephi.ru DESCRIPTION:Speakers: Mikhail Lisitsin ()\nMeasuring the energy spectrum o f very high-energy muons (VHE-muons) solves many problems of cosmic rays p hysics and nucleus-nucleus interactions. The most promising facilities for solving this problem are gigaton neutrino telescopes (IceCube\, Baikal-GV D and KM3NeT). However\, VHE-muons (E > 30-100 TeV) come into the detector accompanied by muon bundles of various multiplicities. In this case\, it is difficult to distinguish muon bundles of large multiplicity from muon b undles of small multiplicity with a high-energy muon. The report is devote d to the development of a new method for distinguishing such events.\n\nTh e essence of the developed method is the analysis of the longitudinal prof ile of energy loss and the selection of events according to the exponent i ndex of the fitting function and the magnitude of fluctuations in energy l oss. \nTo develop and adjust the method\, simulations of the energy spectr um with a power index of 2.7 were performed in the energy range of 10^14 – 10^20 eV via the CORSIKA program. The spectrum of EAS muons was obtain ed. The energy losses of EAS muons and single VHE-muons with fixed energie s 10\, 31\, 100\, 316\, 1000 TeV were simulated in the PROPOSAL software p ackage. An algorithm has been developed for the muon bundles assembling ba sed on the spectrum of EAS muons.\n\nVarious criteria for distinguishing e vents based on combinations of the exponent index of the longitudinal prof ile of the energy loss and the residual sum of squares are discussed in th e report. The results of separating events with various bins in the longit udinal profile of the energy loss of the EAS muon component are shown.\n\n https://indico.nevod.mephi.ru/event/9/contributions/232/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/232/ END:VEVENT BEGIN:VEVENT SUMMARY:Reconstruction of parameters of extensive air showers registered b y the NEVOD-EAS array DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-209@indico.nevod.mephi.ru DESCRIPTION:Speakers: Elena Yuzhakova (MEPhI)\nThe talk is devoted to the methods of reconstruction of parameters of extensive air showers based on the response of the NEVOD-EAS array. The NEVOD-EAS array is located in MEP hI and allows measuring deposited energy and arrival time of EAS particles . The development of reconstruction method is carried out using simulation s produced by means of the CORSIKA program with the QGSJET-II-04 + FLUKA 2 020.0.3 hadron interaction models. In total\, we have analysed 1 200 000 s howers initiated by primary protons and iron nuclei in the energy range 10 ^15 - 10^17 eV.\nTo reconstruct the parameters of the EAS\, we have applye d two methods: least squares and maximum likelihood. The accuracy of recon struction of the EAS core position\, the age and the shower size is discus sed. Results of estimation of the effective area of the array using variou s cuts are presented\, and the accuracy of reconstruction of the shower si ze spectrum for different types of primary particle spectra is considered. \n\nhttps://indico.nevod.mephi.ru/event/9/contributions/209/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/209/ END:VEVENT BEGIN:VEVENT SUMMARY:The data acquisition system of the coordinate-tracking detector TR EK DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-207@indico.nevod.mephi.ru DESCRIPTION:Speakers: Evgeniy Khomchuk (National Research Nuclear Universi ty MEPhi)\nThe large-scale coordinate-tracking detector TREK is being cons tructed at the Experimental Complex NEVOD (MEPhI\, Moscow). It is designed to detect high-density muon bundles of inclined extensive air showers. It will significantly expand the capabilities of the experimental complex an d ensure the progress in solving the «muon puzzle».\nThe main elements o f the coordinate-tracking detector TREK are: the drift chambers (DCs)\, th e time-to-digital converters (TDCs)\, and a control computer\, running DAQ software. The detector consists of two coordinate planes including 132 DC s each. The total area of the coordinate plane is 250 sq. meters. The cham bers of each plane are divided into 18 clusters. Each cluster is served by its own TDC ensuring precise measurement of DC hit times\, as well as per iodic noise measurements. To provide synchronous operation and triggering of TDCs\, the registering system of the TREK detector is connected to the System of Global Time Synchronization of the Complex\, as well as to the t riggering system of the NEVOD-DECOR-CTS experiment. The control and monito ring of the DAQ system\, as well as TDC data read-out and storing are perf ormed by the specially developed software.\nIn the talk\, we describe the structure and operation principals of the TREK detector DAQ system\, as we ll as the architecture and features of its software.\n\nhttps://indico.nev od.mephi.ru/event/9/contributions/207/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/207/ END:VEVENT BEGIN:VEVENT SUMMARY:Extensive air showers of highest energies registered at the Yakuts k array DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-201@indico.nevod.mephi.ru DESCRIPTION:Speakers: Stanislav Knurenko ()\nThe article considers showers produced by primary particles with energies E0 ≥ 100 EeV. The showers w ere registered in the course of continuous long-term observations at the Y akutsk array of extensive air showers. In the present work\, the mathemati cal processing of showers was repeated and the phenomenology of the charge d component\, muons with threshold thr\,  1 GeV and radio emission i n the region of highest energies was refined. The characteristics of cosmi c rays are analyzed: the energy spectrum and mass composition determined f rom the Cherenkov\, muon components and radio emission in the energy range 50 – 200 EeV.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/20 1/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/201/ END:VEVENT BEGIN:VEVENT SUMMARY:Monte Carlo simulation of the OLVE-HERO detector DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-223@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ilyas Satyshev (JINR)\nA project of the OLVE-HERO sp ace detector is proposed for CR measurement in the range 1012-1016 eV\, wh ich will include a large ionization-neutron 3D calorimeter with a high gra nularity and geometric factor of ~16 m2٠sr. Current OLVE-HERO main detect or is expected to be an image calorimeter of a boron loading of plastic sc intillator with a tungsten absorber. Such a calorimeter allows one to meas ure an additional neutron signal which will improve the energy resolution of the detector and mainly the rejection power between electromagnetic and nuclear CR components will be increased by factor 30-50. Preliminary resu lts of modeling the threshold sensitivity from the energy of CR particles for a simplified version of the detector are presented\, where the thresho ld value is defined by the thermal neutron number in the detector.\n\nhttp s://indico.nevod.mephi.ru/event/9/contributions/223/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/223/ END:VEVENT BEGIN:VEVENT SUMMARY:New approach of explaining the missing sources of UHE neutrinos as an effect of approaching Planck length DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-192@indico.nevod.mephi.ru DESCRIPTION:Speakers: Abdullah Shehada (Chechen State Pedagogical Universi ty )\nIn this paper a new effect have been taken into account which has ev er been\nused before in physics\, this effect related to two different eld s\, Quantum physics and General Relativity. This effect takes name: Time D ilatation as an Effect of Approaching Planck Length\, this effect is compl etely different from the gravitational time dilatation in general relativi ty and time dilatation due to closing to the speed of light in special rel ativity. The new effect becomes obvious and strong for the particles that have very high energies. Experiments in particle physics and astrophysics had got conclusion that the particles may travel faster than the speed of light in vacuum\, such as MINOS experiment and Fermilab1979 in particle ex periments and supernova SN1987A and Gamma Ray Bursts (GRBs) in astronomy f ield. And that seems violating the theory of relativity\, but this theory can explain all these unusual observations easily and doesn't violating th e theory of relativity.\n\nhttps://indico.nevod.mephi.ru/event/9/contribut ions/192/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/192/ END:VEVENT BEGIN:VEVENT SUMMARY:Local interstellar spectra of electrons and positrons by demodulat ing fluxes from the PAMELA experiment DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-252@indico.nevod.mephi.ru DESCRIPTION:Speakers: Pavel Mukhin ()\nOn entering the Solar System\, gala ctic cosmic rays undergo solar modulation\, which can be described with a modulation parameter defined by proton fluxes from neutron monitors. In pa rticular\, the modulation considerably distorts the fluxes of galactic cos mic-ray electrons and positrons with energies below 10 GeV. Taking into ac count known modulation potential\, which also depends on the solar activit y\, there is a possibility of restoring the local interstellar spectra by demodulating fluxes from satellite experiments.\nThis work presents primar y electron and positron fluxes obtained by the PAMELA experiment at 1 AU f or different solar activity phases in 2006–2016 using machine learning m ethods. Also\, by demodulating these spectra\, the local interstellar spec tra of electrons and positrons have been restored.\n\nhttps://indico.nevod .mephi.ru/event/9/contributions/252/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/252/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for particle excess from the Cygnus Cocoon region dire ction during a hypothetical flare detected in the Bаksan Crapet-2 exper iment DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-239@indico.nevod.mephi.ru DESCRIPTION:Speakers: Lyubov Sveshnikova (MSU)\nSources of PeV cosmic rays (so called Pevatrons) can be identified by gamma and neutrino radiatio n with energy more than 100 TeV due to not destroyed trajectories by interstellar and galactic magnetic fields. In particular\, one of such po tential sources areas is considered to be the region of the double source PSR J2032+4127 in the Cocoon nebula in the constellation Cygnus. The neut rino event with energy 150 TeV was recorded in the Ice Cube experiment in November\, 2020 from the Cygnus Cocoon direction. In the Capet 2 exper iment (located in Baksan gorge)\, there was registered a sharp increase o f photon fluxes with an energy of more than 300 TeV from the same directio n as Ice Cube neutrino and temporal coincidence. This flux exceeds by 4 orders of magnitude the expected intensity obtained in gamma-ray astronomi cal experiments and it is comparable to the EAS hadron background.\nIn th e TAIGA astrophysical experiment\, the HiSCORE wide-angle Cherenkov instal lation (with an area of about 1 km2 at present) is aimed at registering ga mma quanta with an energy of more than 50 TeV with an angular resolution o f at least 0.2 degrees. One can expect that such a powerful flare should be registered by HiSCORE array. \n To check this hypothesis we have analyzed EAS events registered by HiSCORE array during 20 hr in Octob er- November 2020 yr from the Cygnus Cocoon direction. The intensity of g amma-like particles with energy more than 200 TeV has been compared with an intensity of the nearest background region around the source. The uppe r limit of the expected excess flux will be presented.\n\nhttps://indico.n evod.mephi.ru/event/9/contributions/239/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/239/ END:VEVENT BEGIN:VEVENT SUMMARY:Extraction of signals from EAS neutrons detected by the URAN setup DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-234@indico.nevod.mephi.ru DESCRIPTION:Speakers: Dmitriy Chernov (National Research Nuclear Universit y MEPhI (Moscow Engineering Physics Institute))\nOn the basis of the Exper imental Complex NEVOD\, the URAN setup has been deployed which serves to d etect the electron-neutron component of extensive air showers (EAS). This setup includes 72 scintillation detectors and covers an area of ~10^3 m^2. Registration of the neutron component by detectors is possible due to the ZnS(Ag) + B2O3 scintillator\, where the content of the 10B isotope is 18% . When a neutron is captured by the boron isotope (10B)\, two charged part icles are born\, which cause luminescence flashes in ZnS(Ag) scintillator recorded by a photomultiplier. \nOne of the important problems is the sepa ration of signals caused by neutron capture in a scintillator from noise p ulses. The paper presents a new algorithm for selecting signals caused by EAS neutrons capture. The algorithm makes it possible to reduce the contri bution of noise pulses and increase the efficiency of neutron detection by the URAN setup.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/23 4/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/234/ END:VEVENT BEGIN:VEVENT SUMMARY:A technique of the calibration of optical modules inside the volum e of Cherenkov water detector NEVOD DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-205@indico.nevod.mephi.ru DESCRIPTION:Speakers: Tatyana Karetnikova (National Research Nuclear Unive rsity "MEPhI")\nIn recent decades\, Cherenkov water (ice) telescopes such as IceCube\, Baikal-GVD and KM3Net are being actively developed for resear ch in the field of neutrino physics and astrophysics. Optical modules are the main detecting elements of such neutrino telescopes.\nCalibration of o ptical modules of different neutrino telescopes under the same conditions is one of the important experimental problems. Such a calibration can be c arried out at the Experimental complex NEVOD. Scientific installations of the complex make it possible to identify tracks of single near-vertical an d near-horizontal muons\, as well as to detect events with large energy de posits and to study the response of the optical modules being tested to th ese events.\nIn the report\, we discuss the software and hardware complex for calibrating optical modules of Cherenkov neutrino telescopes at the Ex perimental complex NEVOD\, as well as the possibility of its implementatio n for studying the characteristics of the Baikal-GVD optical module.\n\nht tps://indico.nevod.mephi.ru/event/9/contributions/205/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/205/ END:VEVENT BEGIN:VEVENT SUMMARY:Spectrum of cosmic rays variations in 2011-2021 according to AMS-0 2 magnetic spectrometer onboard the ISS DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-258@indico.nevod.mephi.ru DESCRIPTION:Speakers: Vasilina Slastnaya ()\nSince the middle of the last century\, cosmic ray variations have been studied using data from a ground -based network of neutron monitors. To determine the energy spectrum of co smic rays at the boundary of the magnetosphere\, knowledge of the shape of the variation spectrum is required. In this work\, to determine the spect rum of proton flux variations\, we used the recently published precision A MS-02 daily proton data obtained from 05/2011 on board the ISS. To approxi mate the spectrum of variations υ(R)= -δJ/J as function of rigidity R\, the Ellison-Ramaty formula was used. Fitting parameters were obtained on t he daily basis and compared with indexes of solar activity. No transforma tion of the spectrum was found during the polarity of the solar magnetic f ield reversal period. There is an anticorrelation between the fitting para meters and the number of sunspots. Alternative ways of studying the spectr um of variations are considered. At the 2nd moment there are annual quasi- periodic fluctuations. Connection of the 3rd moment with solar flares is o bserved.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/258/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/258/ END:VEVENT BEGIN:VEVENT SUMMARY:Cutoff rigidity in the Galactic magnetic field DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-251@indico.nevod.mephi.ru DESCRIPTION:Speakers: Rustam Yulbarisov (NRNU MEPhI)\nMore than 80 years a fter the discovery of UHECRs\, many questions remain about possible source s\, mechanisms of acceleration\, propagation\, and so on. An important asp ect of research is the analysis of their motion in the magnetic field of t he Galaxy\, which implies\, first of all\, model calculations. New works d evoted to such an analysis appear with the accumulation of experimental ob servations of the field and the development of the corresponding models.\n The current work is devoted to the calculation of the magnetic cutoff rigi dity of cosmic rays in the Galactic field. We calculate the movement of ch arged particles in the Milky Way using the toolkit developed by our scient ific group. The calculation is performed in a modified JF12 model. We inve stigate the residence time of particles with different energies in the gal actic disk and construct a map of the magnetic cutoff for an observer on t he Earth. The influence of the simulated sizes of turbulent inhomogeneitie s on the result is considered.\n\nhttps://indico.nevod.mephi.ru/event/9/co ntributions/251/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/251/ END:VEVENT BEGIN:VEVENT SUMMARY:Extending of the capabilities of the PRISMA-36 array through the i ntroduction of a recording channel for studying neutron variations DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-246@indico.nevod.mephi.ru DESCRIPTION:Speakers: Dmitry Gromushkin (National Research Nuclear Univers ity MEPhI (Moscow Engineering Physics Institute))\nSince 2012 in the Exper imental Complex NEVOD (MEPhI\, Moscow)\, the PRISMA array for studying ext ensive air showers by detecting neutrons has been operated. In the array t he en-detectors are used to detect neutrons. The detector consists of a th in (~ 30 mg/cm^2) inorganic scintillator ZnS(Ag)+6^LiF (the enrichment of Li with 6^Li isotope is 90%) and photomultiplier FEU-200\, which are insta lled inside a light-isolating cylindrical housing (heights of 570 mm and d iameter of 740 mm). In 2023\, it is planned to upgrade the array by replac ing the photomultipliers\, integrating amplifiers\, digitizing electronics and high-voltage power supply system. Also during the array upgrade\, a s eparate recording channel will be added in the detectors to study variatio ns of the neutron background and processes affecting these variations. In the report we discuss the results of studying the applicability of the hem ispherical photomultipliers EMI 9350 and D642 for the PRISMA-36 array\, as well as the scheme and operating principals of the new recording channel. \n\nhttps://indico.nevod.mephi.ru/event/9/contributions/246/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/246/ END:VEVENT BEGIN:VEVENT SUMMARY:Forbush decreases associated with coronal holes\, coronal mass eje ctions from active regions\, and filament eruptions: a comparison in solar cycles 23 and 24 DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-224@indico.nevod.mephi.ru DESCRIPTION:Speakers: Maria Abunina (IZMIRAN)\nThe paper investigates the similarities and differences between Forbush decreases in solar cycles 23 and 24. The analysis was carried out for groups of events associated with different types of solar sources: coronal mass ejections from active regio ns accompanied by solar flares (CME1 group)\; filament eruptions outside a ctive regions (CME2 group)\; high-speed streams from coronal holes (CH gro up). The distributions and relationships of various parameters were studie d: the amplitude of Forbush decreases\; the maximum values of the hourly d ecrease in the cosmic ray density\, the cosmiv ray equatorial anisotropy\, the solar wind velocity\, the magnetic field intensity during an event\, as well as the values of the solar wind velocity and the magnetic field in tensity one hour before the Forbush decrease onset. The results showed tha t the number of events\, parameter values and their relationships depend o n the phase and cycle of solar activity. In the 24th cycle\, the number of events in the CME1 group decreased\, did not change in CME2\, and increas ed in CH. The values of the parameters and the difference between them in different groups of events are higher in cycle 23. The magnitude of the Fo rbush decreases in the CME1 group in cycle 23 depends more strongly on the solar wind velocity\, and in cycle 24 - on the magnetic field strength\, as in the CME2 group in both solar cycles.\n\nhttps://indico.nevod.mephi.r u/event/9/contributions/224/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/224/ END:VEVENT BEGIN:VEVENT SUMMARY:The indication for 40K geo-antineutrino flux with Borexino phase-I II data DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-216@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ivan Karpikov (INR RAS)\nWe provide the indication o f high flux of 40K geo-antineutrino and geo-neutrino (40K-geo-(ν¯+ν)) w ith Borexino Phase III data. This result was obtained by introducing a new source of single events\, namely 40K-geo-(ν¯+ν) scattering on electron s\, in multivariate fit analysis of Borexino Phase III data. Simultaneousl y we obtained the count rates of events from 7Be\, pep and CNO solar neutr inos. These count rates are consistent with the prediction of the Low meta llicity Sun model SSM B16-AGSS09. MC pseudo-experiments showed that the ca se of High metallicity Sun and absence of 40K-geo-(ν¯+ν) can not imitat e the result of multivariate fit analysis of Borexino Phase III data with introducing 40K-geo-(ν¯+ν) events. We also provide arguments for the hi gh abundance of potassium in the Earth.\n\nhttps://indico.nevod.mephi.ru/e vent/9/contributions/216/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/216/ END:VEVENT BEGIN:VEVENT SUMMARY:The module for positron detecting of the solid-state antineutrino detector DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-188@indico.nevod.mephi.ru DESCRIPTION:Speakers: Dmitry Gromushkin (National Research Nuclear Univers ity MEPhI (Moscow Engineering Physics Institute))\nIn the report we presen t the data on the development of a prototype of module for a solid-state d etector of electron antineutrinos\, which is based on a plastic scintillat or for detecting positrons from the inverse beta decay (IBD) reaction. It is assumed that the complex of scintillation modules\, supplemented with s creens for detecting neutrons from IBD reaction using the ZnS(Ag)-6LiF (or ZnS(Ag)-B2O3) scintillation composition\, will make it possible to constr uct large-scale detectors for monitoring antineutrino fluxes generated in a fission chain reaction. The practical application of such detectors is c onnected with the remote monitoring of nuclear power plant reactors\, smal l modular reactors\, including floating power plants\, as well as with the solution of nonproliferation problems.\n\nhttps://indico.nevod.mephi.ru/e vent/9/contributions/188/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/188/ END:VEVENT BEGIN:VEVENT SUMMARY:Application of coupling functions to analyze energy characteristic s of Forbush decreases according to URAGAN muon hodoscope data DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-220@indico.nevod.mephi.ru DESCRIPTION:Speakers: Polina Sukhova (NRNU MEPhI)\nThe purpose of the work is to investigate energy characteristics of Forbush decreases using coupl ing functions according to muon hodoscope URAGAN data. A coupling function shows relative contribution of primary cosmic rays with different energie s to a count rate observed by a particular detector\, so it is a basic too l to study energy characteristics of various modulation phenomena\, such a s Forbush effects. \nA coupling function of a real detector depends on an integral multiplicity of secondary particles\, effective area of the detec tor and the spectrum of primary particles. The muon multiplicity was deter mined by simulations in CORSIKA software package using FLUKA and QGSJET II models. \nAn algorithm for determining amplitudes of Forbush decreases wa s developed. In the work we present results of calculations of the muon ho doscope effective energies using coupling functions. Methods for determini ng spectral indices of Forbush decreases by relative variations\, as well as by effective energies\, are implemented.\n\nhttps://indico.nevod.mephi. ru/event/9/contributions/220/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/220/ END:VEVENT BEGIN:VEVENT SUMMARY:Analysis of joint events by means of the ProtoTREK and the NEVOD-E AS data DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-235@indico.nevod.mephi.ru DESCRIPTION:Speakers: Diana Gazizova (NRNU MEPhI)\nThe Experimental Comple x NEVOD includes a number of large-scale facilities for detection of high energy cosmic rays\, including the ProtoTREK and the NEVOD-EAS detectors. The coordinate detector ProtoTREK consists of 14 multiwire drift chambers with a total area of 13 $m^2$ and makes it possible to register and to rec onstruct tracks of charged particles of extensive air showers (EAS). The N EVOD-EAS facility is an array of surface scintillation detectors covering an area of $10^4$ $m^2$ which are grouped in 9 clusters\; the setup regist ers the electron-photon component of the EAS. These detectors work indepen dently\, in particular\, they have different internal clocks. The ProtoTRE K is located between the detector stations of the 5th cluster of the NEVOD -EAS\, therefore\, the events that are registered in this cluster are cons idered. The work presents results of the analysis of joint events. The ori ginal method for selection of events was developed. 4814 joint events on J une 10 and June 11\, 2021 were found and analyzed by the difference of the angles between reconstructed directions of the EAS. Thereby\, the most pr obable angle between the reconstructed by two setups EAS arrival direction s is 3.4°.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/235/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/235/ END:VEVENT BEGIN:VEVENT SUMMARY:The project of the hardware and software system for storage and an alysis of large amounts of data of the scientific facilities of the Experi mental Complex NEVOD DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-206@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ivan Shulzhenko (National Research Nuclear Universit y MEPhI)\, Evgeniy Khomchuk (National research nuclear university)\nTo dat e\, cosmic rays are the only tool that allows one to study nucleus-nucleus interactions at energies of hundreds of TeV in the center-of-mass system. Investigations of high-energy CR are carried out by detection of secondar y particles of extensive air showers (EAS) formed in interactions of prima ry particles with the Earth's atmosphere.\nEarlier studies of EAS revealed a number of unusual phenomena in the interactions of particles of high an d ultra-high energies: in the measured energy spectrum of cosmic rays a nu mber of features that today cannot be explained within the framework of a single model are observed. The key to explaining these phenomena may be th e results of multicomponent studies of EAS carried out in frames of the co mplementary approach to the experimental data analysis.\nSuch studies and such an approach can be implemented at the Experimental Complex (EC) NEVOD . The complex combines six scientific facilities (NEVOD\, DECOR\, CTS\, NE VOD-EAS\, PRISMA-32 and URAN) which are launched in operation and allow on e to study the same events using three components at once: electron-photon \, muon and hadronic ones.\nAs a result of the operation of the facilities \, a volumetric data stream is formed. It contains topological\, trigger\, coordinate\, amplitude and time information about recorded events. At the same time\, to solve various computational problems in order to verify th e obtained experimental results and develop new methods\, an impressive ba nk of simulated EAS and facility responses obtained using the Geant4 and C ORSIKA software packages is required.\nTherefore\, for storing and efficie nt analysis of experimental and simulated events of the facilities of the Complex\, a hardware and software system for storage and analysis of large amounts of data is being created. This system will be deployed on the bas is of the EC NEVOD data processing center providing all the necessary oper ating conditions\, including a backup power system\, and integration into the EC NEVOD local area network. Modern DBMS will make it possible to effe ctively select from the total amount of events (both experimental and simu lated) only those ones that satisfy certain criteria and are suitable for solving specific physical problems.\nIn the report\, we describe the hardw are and software architecture\, features of the system for storage and ana lysis of large amounts of data of the scientific facilities of the Experim ental Complex NEVOD. We also present the structures of the databases for s toring data of experimental events which are already implemented and used for analysis. The prospects of the further development of the system are d iscussed.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/206/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/206/ END:VEVENT BEGIN:VEVENT SUMMARY:Features of Forbush decreases obtained by satellite and ground-bor n detectors DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-241@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ilya Lagoida (NRNU MEPhi)\nThe Forbush decreases (FD s) are known as sharp drops in cosmic ray intensity\, registered by differ ent scientific equipment on Earth and interplanetary space. These events c orrelate with solar activity\, mainly with coronal mass ejections (CMEs). CMEs spreads into interplanetary space and swap out the cosmic ray particl es from the modulation region. The main features of FDs are the intensity drop amplitude and the recovery time to its undisturbed level. These param eters are characterized by a large variability of the measured values. The reasons for this variability are connected to the scale of the CMEs and w ith the structure and velocity of ejected solar mass in place of measureme nt. Also\, they depend on the detector type used for observing FDs. The sa tellite detectors register primary cosmic rays in a wide energy range and effectuate the direct measurements of the phenomenon\, whereas ground-base d detectors measure the secondary cosmic rays born in the Earth's atmosphe re. Ground-based detectors have larger statistics with respect to satellit e experimentation but are less sensitive to different variations of cosmic rays intensity as well as FDs. To study FDs properties we use the primary flux data of CR cosmic ray particles recorded by the PAMELA and AMS-2 spe ctrometers for the time period from 2006 to 2019 in the rigidity range fro m 0.8 to 50 GV. The amplitudes and recovery time behaviors during FD pheno mena were the subject of our study. The data from SOHO coronagraphs were t aken for searching the CMEs responsible for the observed FDs. The amplitud e values of FDs and the behavior of their recovery times were followed wit h respect to some parameters of solar activity and interplanetary space. T he obtained results of the satellite instruments were compared with data f rom several neutron monitors.\n\nhttps://indico.nevod.mephi.ru/event/9/con tributions/241/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/241/ END:VEVENT BEGIN:VEVENT SUMMARY:Dynamics of high-energy proton fluxes in the South Atlantic Anomal y region according to ARINA and VSPLESK satellite experiments DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-236@indico.nevod.mephi.ru DESCRIPTION:Speakers: Sergey Aleksandrin (National Research Nuclear Univer sity “MEPhI”)\nThis paper studies the dynamics of proton flux in the S outh Atlantic Anomaly (SAA) region according to ARINA (was operated on the Resurs-DK1 satellite from 2006 to 2015) and VSPLESK (which was mounted on the ISS from 2008 to2013) satellite experiments. Both spectrometers have the same scheme.\nThe SAA drift is determined by the position of the maxim um flux of high-energy protons with energies in the range from 30 to 100 M eV at the altitude of the Resurs-DK1 satellite (about 350-600 km) and the ISS (380-420 km). Part of the time the instruments operated simultaneously .\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/236/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/236/ END:VEVENT BEGIN:VEVENT SUMMARY:Ultrahigh-energy neutrino-nucleon deep-inelastic scattering and th e Froissart bound violation DTSTART;VALUE=DATE-TIME:20230627T134500Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-211@indico.nevod.mephi.ru DESCRIPTION:Speakers: Anatoly Kotikov ()\nA simple formula for the total c ross section \\sigma_{\\nu N} of neutral- and charged-current deep-inelast ic scattering of ultrahigh-energy neutrinos on isoscalar nuclear targets i s presented. The cross section \\sigma_{\\nu N} is proportional to the str ucture function F_2^{\\nu N}(M^2_V/s\,m_V^2) (M_V is the intermediate-bos on mass and s is the square of the center-of-mass energy) with an addition al coefficient\, which depends on the asymptotic low-x behavior of F_2: it contains an additional \\ln s term if F_2 scales with a power of \\ln(1/x ). Hence\, an asymptotic low-x behavior F_2 \\sim \\ln^2(1/x)\, which is frequently assumed in the literature\, already leads to a violation of the Froissart bound on \\sigma_{\\nu N}.\n\nhttps://indico.nevod.mephi.ru/eve nt/9/contributions/211/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/211/ END:VEVENT BEGIN:VEVENT SUMMARY:Thermal neutron background variations monitoring using en-detector s DTSTART;VALUE=DATE-TIME:20230627T134000Z DTEND;VALUE=DATE-TIME:20230627T140000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-199@indico.nevod.mephi.ru DESCRIPTION:Speakers: Kirill Kyrinov (INR RAS)\nLong-term variations of th ermal neutron background in Moscow\, where EAS array ENDA-INR is running\, are studied using en-detectors (developed in the INR RAS). EN-detectors b ased on the inorganic scintillation compound ZnS(Ag) + B2O3 with unenforce d boron. The paper provides information about detectors stability and ther mal neutron background variations including seasonal and weather effects.\ n\nhttps://indico.nevod.mephi.ru/event/9/contributions/199/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/199/ END:VEVENT BEGIN:VEVENT SUMMARY:Coulomb pulsars are sources of cosmic rays with energies greater t han 10 TeV DTSTART;VALUE=DATE-TIME:20230627T133000Z DTEND;VALUE=DATE-TIME:20230627T134500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-229@indico.nevod.mephi.ru DESCRIPTION:Speakers: Phiilipp Vysikaylo (MRSU)\nIn a new capacity\, Einst ein's idea of the equivalence of mass and energy is confirmed. The equival ence manifests itself in similar functionality in the processes of pulsati ons (focusing and bounce) of "excess" energy in the generalized 2D Kepler problem and "excess" mass in the 3D Vysikaylo-Chandrasekhar problem of cum ulation and dissipation of de Broglie waves in quantum stars (pulsating ac cretion of quantum stars) with a mass greater than Chandrasekhar's (~ 1.46 solar masses). Such pulsations of quantum stars are due to differences in the de Broglie wavelengths of electrons and ions. This difference leads t o quantum separation of charge during the collapse of a quantum star and t he formation of an electric field shock wave. A new mechanism (type) of a thermonuclear reactor near the surface of charged quantum stars and dense cores of ordinary stars and planets is proposed. Acceleration of protons a nd electrons up to energies above 10 TeV in electric field shock waves in the nuclei of giant plasmoids – quantum stars – and their transmutatio n into neutrons in reactions with each other are the basis of such a mecha nism. Rotation\, which reveals cumulation and dissipation and structurally promotes the transfer of energy from all degrees of freedom into rotation and pulsations during cumulation\, is not the only true sign of cumulatio n and structural spiral turbulence with hierarchical cascades of structure s with energy-mass-momentum flows. The same sign of cumulation is the viol ation of electrical neutrality.We prove that\, just as in the case of rota tion\, it is possible under certain conditions to form space charge jumps (shock waves of the electric field discovered by Rutherford in atomic nucl ei\, Gunn in semiconductors and Vysikaylo in gas-discharge plasma\, see [1 ] for more details) and the transformation of all types of energy into ele ctrical energy (electric field). In this case\, the violation of electrica l neutrality is very small\, but its role in the organization of the struc ture of the Coulomb quantum pulsar is enormous. It is a weak violation of electrical neutrality at a level of 10**-36 that stops the gravitational c umulation of protons into stars (and even into black holes) and leads to t he generation of proton or ion winds from stars [2] and even from black ho les [1]. The violation of electrical neutrality at the level of 10**-18 le ads to the suppression of gravitational forces\, and at the level of 10**- 12 - to the formation of Cosmic rays with energies up to 3·10**20 eV [1]. Simultaneous excitation in complex hierarchical dynamical systems of rota tion\, pulsations and violation of electrical neutrality leads to the gene ration of the third degree of freedom - a magnetic field. There is no need to invent a "mysterious" magnetic dynamo\, but one should involve the int erference of rotation and violation of electrical neutrality. The author a rgues that the presence of a magnetic field is an indirect\, convincing si gn of a violation of electrical neutrality and rotation\, and\, consequent ly\, cumulation.\n[1] Vysikaylo P.I. Detailed Elaboration and General Mod el of the Electron Treatment of Surfaces of Charged Plasmoids (from Atomic Nuclei to White Dwarves\, Neutron Stars\, and Galactic C ores): Self_Condensation (Self_Constriction) and Classification of Charged Plasma Structures–Plasmoids. Part I-3. General Analysis of the Convecti ve Cumulative–Dissipative Processes Caused by the Violation of Neutralit y: Metastable Charged Plasmoids and Plasma Lenses. Surface Engineering and Applied Electrochemistry. 2012\, 48(1)\, 11–21.\n[2] Vysikaylo P.I. Qu antitative Investigation Nonequilibrium Inhomogeneous Plasma of the Helios phere with Runaway Electrons IEEE Transactions on Plasma Science 2022\, V. 50\, Issue 4\, pp. 810-816. DOI: 10.1109/TPS.2022.3160189\n\nhttps://indic o.nevod.mephi.ru/event/9/contributions/229/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/229/ END:VEVENT BEGIN:VEVENT SUMMARY:Mass composition of cosmic rays with energies above 3*10^15 eV acc ording to the data of the small Cherenkov array DTSTART;VALUE=DATE-TIME:20230627T131500Z DTEND;VALUE=DATE-TIME:20230627T133000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-230@indico.nevod.mephi.ru DESCRIPTION:Speakers: Valentina Mokhnachevskaya (SHICRA SB RAS)\, Stanisla v Knurenko (SHICRA SB RAS)\nAccording to the long-term registration data f rom the small Cherenkov array of integral and Cherenkov differential detec tors obtained the characteristics of air showers with energies above 3*10^ 15 eV\, including of the maximum of the development of the Xmax. The depen dence of Xmax on the shower energy found and the characteristics of air sh owers compared with the QGSjetII-04 model. From a comparison of Xmax with calculations based on the QGSetII-04 model for a proton and an iron nucleu s\, a conclusion obtained on the mass composition of cosmic rays in the en ergy range 3*10^15 – 2*10^18 eV.\n\nhttps://indico.nevod.mephi.ru/event/ 9/contributions/230/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/230/ END:VEVENT BEGIN:VEVENT SUMMARY:Modernization of mechanical attachements point DTSTART;VALUE=DATE-TIME:20230627T130000Z DTEND;VALUE=DATE-TIME:20230627T131500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-242@indico.nevod.mephi.ru DESCRIPTION:Speakers: Aleksandr Blinov ()\nIACT's are one of the key parts of the TAIGA observatory and design for study of gamma rays and charged c osmic rays in the energy range of 1013-1018 eV. One of crucial components of IACT is mechanical attachment point of mirror. It's consist of: mirror\ , heating cable and mirror alignment actuators. This poster will present t he results of the modernization of the mechanical attachment point of mirr ors\, such as: replacement of the heat cable with a heater\, that covers t he back surface of the mirror\, mirror alignment automation and the produc tion of mirrors.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/24 2/ LOCATION:National Research Nuclear University MEPhI Hall of B-100 Lecture Room URL:https://indico.nevod.mephi.ru/event/9/contributions/242/ END:VEVENT BEGIN:VEVENT SUMMARY:Astrophysical aspects of multiple fragmentation of nuclei in nucle ar emulsion DTSTART;VALUE=DATE-TIME:20230629T100000Z DTEND;VALUE=DATE-TIME:20230629T101500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-186@indico.nevod.mephi.ru DESCRIPTION:Speakers: Andrei Zaitsev (JINR)\nThe BECQUEREL experiment is a imed at solving topical problems in nuclear clustering physics [1]. The us ed method of nuclear track emulsion (NTE) makes it possible\, due to its u nique sensitivity and spatial resolution\, to study in a unified approach multiple final states arising in dissociation of relativistic nuclei. The ideas about nuclear clustering obtained in high-energy physics are importa nt for applications in nuclear astrophysics\, cosmic ray physics\, nuclear medicine\, and perhaps even nuclear geology. Currently\, a research focus is on the theoretical concept of alpha particle Bose-Einstein condensate (αBEC) - the ultra cold state of several S-wave alpha particles near coup ling thresholds. The unstable 8Be nucleus is described as 2αBEC\, and the C-12 Hoyle state (HS) as 3αBEC. Confirmation of the existence of more co mplex forms of αBEC could provide a basis for expanding scenarios for the synthesis of medium and heavy nuclei in nuclear astrophysics.\nThe consid eration of αBEC as an invariant phenomenon indicates possibility of its s earch in the relativistic fragmentation. A practical alternative is provid ed by NTE layers longitudinally exposed to relativistic nuclei. The invari ant mass of ensembles of He and H fragments can be determined from emissio n angles in the approximation of conservation of momentum per nucleon of a parent nucleus [2]. Owing to extremely small energies and widths\, the Be -8 and HS decays\, are identified in fragmentation of light nuclei by an u pper constraint on the invariant mass. Having been tested\, this approach has been used to identify Be-8 and HS and search for more complex states o f αBEC in fragmentation of medium and heavy nuclei. Recently\, based on t he statistics of dozens of Be-8 decays\, an enhancement in probability of detecting Be-8 in an event with an increase in number of relativistic alph a particles was found [3]. A preliminary conclusion is drawn that contribu tions of B-9 and HS decays also increase. The exotically large sizes and l ifetimes of Be-8 and HS allowing suggesting possibility of synthesizing α BEC by successively connecting the emerging alpha particles.\nThe main tas k of the forthcoming stage of the project is to clarify the relation betwe en the appearance of Be-8 and HS and alpha multiplicities and search on th is basis for decays of the 4αBEC [4]. In this regard\, the BECQUEREL expe riment aims to measure multiple channels of Kr-84 fragmentation below 1 Ge V per nucleon in GSI (Darmtadt). There are a sufficient number of NTE laye rs\, transverse scanning of which on the motorized microscope Olympus BX63 makes it possible to achieve required statistics. However\, the low energ y complicates the identification of HS and 4αBEC. NTE layers exposed to h eavy nuclei at several GeV per nucleon will make it possible to apply well -established approaches to analysis. The acceleration of Xenon nuclei up t o 3.8 GeV per nucleon and the extraction of their beam in the recent run o f the NICA accelerator chain made it possible to take practical steps towa rds nuclear emission irradiation near the accelerator and in the area of t he flagship BM@N experiment.\n\n\n[1] P.I. Zarubin\, Lect. Notes in Phys . 875\, Clusters in Nuclei\, Volume 3. Springer Int. Publ.\, 51 (2013)\; a rXiv:1309.4881.\n[2] D.A. Artemenkov et al.\, Eur. Phys. J. A 56 (2020) 250\; arXiv: 2004.10277.\n[3] A.A. Zaitsev et al.\, Phys. Lett. B 820 (2 021) 136460\; arXiv: 2102.09541.\n[4] D.A. Artemenkov et al.\, Phys. At. Nucl.\, 85\, 528 (2022)\; arХiv: 2206.09690.\n\nhttps://indico.nevod.mep hi.ru/event/9/contributions/186/ LOCATION: URL:https://indico.nevod.mephi.ru/event/9/contributions/186/ END:VEVENT BEGIN:VEVENT SUMMARY:Forecast of strong geomagnetic storms in February-March 2023 based on measurements of fluctuations in the intensity of galactic cosmic rays DTSTART;VALUE=DATE-TIME:20230629T094500Z DTEND;VALUE=DATE-TIME:20230629T100000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-225@indico.nevod.mephi.ru DESCRIPTION:Speakers: Petr Gololobov (Yu.G. Shafer Institute of Cosmophysi cal Research and Aeronomy SB RAS)\nIn order to develop methods for space w eather forecasting\, the dynamics of fluctuations (variations with periods from several minutes to 2-3 hours) of the intensity of galactic cosmic ra ys (CR) during the events of strong geomagnetic storms on February 26 and March 23\, 2023\, which are characterized by the values Dst < -100 nT. To do this\, we use 1-minute pressure-corrected registration data from the ne utron monitors of the Yakutsk and Tixie Bay CR stations\, 1-minute data fr om direct observations of the parameters of the interplanetary magnetic fi eld (IMF) and solar wind (SW) onboard the ACE and DSCOVR spacecraft. To st udy the properties of CR fluctuations and SW turbulence\, digital filterin g methods and Blackman-Tukey spectral analysis with the Tukey spectral win dow are used. In this case\, the maximum values of the coherence coefficie nts in the frequency range 1.23·10-4 - 1.67·10-2 Hz are used as the inde x of CR and SW fluctuations. Note that the coherence coefficient is a gene ralization of the correlation function to the frequency domain. Its use is due to the fact that\, in contrast to fluctuation spectra\, the level of which varies by orders of magnitude depending on the state of the interpla netary medium\, coherence takes values ranging from 0 to 1\, regardless of the level of solar activity.\nIt is shown that in the event in February\, in contrast to the event in March\, significant coherent CR fluctuations of large magnitude (about 0.8) are observed about 2 days before the start of the geomagnetic storm. An analysis of data from direct measurements of SW parameters shows that the geomagnetic storm on February 26 was caused b y the passage of an interplanetary shock wave\, and on March 23\, by a cor onal mass ejection with a magnetic cloud moving at a speed not exceeding t he background SW velocity. A more detailed analysis leads to the conclusio n that the presence of CR fluctuations in February is due to the presence in the SW of fast magnetosonic waves of noticeable amplitude\, which can b e generated by energetic storm particle flows in the region ahead of the i nterplanetary shock wave front. While in March 2023 the contribution of th ese waves to the observed IMF turbulence spectrum d id not exceed 50%\, a nd before the onset of the geomagnetic storm\, no coherent CR intensity fl uctuations were observed. At the same time\, high coherence values of CR f luctuations were observed in both events in the region of the disturbance itself\, which may indicate an increased level of magnetosonic turbulence of the solar wind in the region of the SW disturbance itself. The results obtained here are in good agreement with the physical picture of the occur rence of CR intensity fluctuations that we have previously constructed\, b ut further research is required to develop a method for predicting geomagn etic storms based on measurement data from neutron monitors.\nWe thank the NOAA and ACE Science Centers for providing the DSCOVR and ACE spacecrafts data. The work was performed using the equipment of the Unique Scientific Facility "Russian National Ground-Based Network of Cosmic Ray Stations" ( https://ckp-rf.ru/catalog/usu/433536) with the support of the Russian Scie nce Foundation (grant no. 22-22-20045).\n\nhttps://indico.nevod.mephi.ru/e vent/9/contributions/225/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/225/ END:VEVENT BEGIN:VEVENT SUMMARY:Acceptance vectors of muon hodoscope URAGAN DTSTART;VALUE=DATE-TIME:20230629T093000Z DTEND;VALUE=DATE-TIME:20230629T094500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-217@indico.nevod.mephi.ru DESCRIPTION:Speakers: Polina Kuzmenkova (National Research Nuclear Univers ity MEPhI)\nCosmic ray variations observed with ground-based detectors inc lude variations of extraterrestrial origin\, atmospheric\, magnetospheric\ , apparatus variations\, and statistical fluctuations. The method of accep tance vectors allows us to determine cosmic ray anisotropy out of the magn etosphere for studying physics of solar-terrestrial relations. The basis o f the technique are coupling function method\, calculations of particle tr ajectories in the terrestrial magnetic field\, and spherical analysis. \n\ nThe work presents preliminary results of muon hodoscope URAGAN acceptance vectors computing. Furthermore\, the comparison of muon data with the Glo bal Survey Method for neutron monitor network is discussed. Finally\, the application of the method to investigate geoeffective events by cosmic ray data is considered.\n\nhttps://indico.nevod.mephi.ru/event/9/contribution s/217/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/217/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic ray variations of magneospheric and atmospheric origin in S eptember 2017 DTSTART;VALUE=DATE-TIME:20230629T091500Z DTEND;VALUE=DATE-TIME:20230629T093000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-203@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ivan Kovalev (Institute of Solar-Terrestrial Physics SB RAS)\nUsing data of ground level cosmic ray observations on neutron mo nitor world network\, Yakutsk muon telescope complex and URAGAN muon hodos cope (Moscow)\, we carried out a research of magnetospheric and atmospheri c cosmic ray variations over September 2017 by a modified spectrographic g lobal survey method. We obtained time dependence of changes in the planeta ry system of rigidities of geomagnetic cutoff (RGC) and average mass tempe rature over the muon detector sites. Based on the data on the planetary sy stem of RGCs\, we calculated the parameters of certain magnetospheric curr ent systems during the geomagnetic disturbances of September 2017 within a n axial symmetric model of a bounded magnetosphere.\n\nhttps://indico.nevo d.mephi.ru/event/9/contributions/203/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/203/ END:VEVENT BEGIN:VEVENT SUMMARY:Selection of the solar-diurnal anisotropy of cosmic rays by local and global methods DTSTART;VALUE=DATE-TIME:20230629T090000Z DTEND;VALUE=DATE-TIME:20230629T091500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-193@indico.nevod.mephi.ru DESCRIPTION:Speakers: Nataly Shlyk (IZMIRAN)\nAccording to the Moscow neut ron monitor (NM MOSC) data\, using harmonic analysis\, the characteristics of the solar-diurnal anisotropy of cosmic rays (CR) on quiet days were ob tained for a long period from 1965 to 2020. It has been established that t he average daily CR variations at NM MOSC are almost completely described by two harmonics of the solar-diurnal anisotropy and does not contain sign s of other influences. Comparison with the average daily characteristics o f the equatorial component of the CR vector anisotropy\, obtained from the data of the global NM network using the global survey method\, showed goo d agreement between the results of the two methods. From a comparison of l ocal and global results\, estimates of the coupling coefficients of the fi rst harmonic of CR anisotropy for NM MOSC was done and a new experimental method for calculating the coupling coefficients of individual detectors i s proposed.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/193/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/193/ END:VEVENT BEGIN:VEVENT SUMMARY:Reconstruction of the characteristics of a high-energy event detec ted by the Carpet-2 array in association with the GRB 221009A gamma-ray bu rst DTSTART;VALUE=DATE-TIME:20230629T081500Z DTEND;VALUE=DATE-TIME:20230629T083000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-215@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ivan Karpikov (INR RAS)\nThe Carpet-2 collaboration reports on the observation and analysis of an event with a low muon conten t coincident with the gamma-ray burst GRB 221009A and the transient Swift J1913.1+1946. This bright transient was observed by numerous instruments i n the optical\, X-ray and gamma-ray energy ranges. The redshift of this GR B is z=0.1505 (measured from afterglow observations).\nThe Carpet-2 array detected an extensive air shower at 14:32:35 UT (1338 s after the SWIFT tr igger and 4536 s after the GBM trigger) with the reconstructed arrival dir ection (RA=289.51°\, Dec=18.44°) \, which is 1.78° from the direction t owards GRB 221009A\, well within the angular resolution of Carpet-2 (\\app rox 4.7°). This event produced zero hits in the 175 m^{2} muon detector o f the Carpet-2 array. The reconstructed energy of the primary particle is in the range of 200-250 TeV. We estimate of the probability of the type o f particle (photon or proton)\, its energy and detection efficiency.\n\nht tps://indico.nevod.mephi.ru/event/9/contributions/215/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/215/ END:VEVENT BEGIN:VEVENT SUMMARY:The study of cosmic rays with energies greater than 5 EeV by radio method DTSTART;VALUE=DATE-TIME:20230629T080000Z DTEND;VALUE=DATE-TIME:20230629T081500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-202@indico.nevod.mephi.ru DESCRIPTION:Speakers: Igor Petrov (Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy)\nSince 1986\, regular measurements of radio emissi on generated by air shower relativistic particles have been started at the Yakutsk array. As a result of studying the noise background on the array region\, a frequency of 30-35 MHz was chosen with minimal radio noise. Sho wers with energies greater than 10 EeV were registered at the array. For t he first time\, radio emission in showers with energies greater than 100 E eV was registered at the Yakutsk array. A joint study of charged particles \, Cherenkov light\, and radio emission showed that the amplitude of the r adio signal is proportional to the energy of the shower\, and the shape of the spatial distribution of radio emission at sea level is associated wit h the maximum development of the shower particle cascade. Based on these c haracteristics\, using calculations of the QGSjetII-04 model\, an estimate was made of the atomic weight of primary particles that produced air show ers with highest energies.\n\nhttps://indico.nevod.mephi.ru/event/9/contri butions/202/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/202/ END:VEVENT BEGIN:VEVENT SUMMARY:Systematic uncertainties of the primary astroparticle energy estim ation vs zenith angle distribution of EAS event rate measured with surface array DTSTART;VALUE=DATE-TIME:20230629T074500Z DTEND;VALUE=DATE-TIME:20230629T080000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-191@indico.nevod.mephi.ru DESCRIPTION:Speakers: Anatoly Ivanov (Shafer Institute for Cosmophysical R esearch and Aeronomy)\nSystematic uncertainties in the energy estimation o f EAS primaries are a source of headache for physicists and lead to elusiv e discrepancies in the energy spectra of cosmic rays measured with differe nt arrays. We have found the zenith angle distribution of EAS event rate t o be sensitive to these systematic uncertainties. It gives an opportunity to test different algorithms for the primary astroparticle energy estimati on\, to find the best of them\, and tune the parameters in the model indep endent way. We have compared several algorithms that were in use in the Ya kutsk array group\, discard some of them\, and derived the proper paramete rs assuming isotropic arrival directions of cosmic rays.\n\nhttps://indico .nevod.mephi.ru/event/9/contributions/191/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/191/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct comparison of muons in ultrahigh energy EASs between Yakuts k array and Auger experiment data DTSTART;VALUE=DATE-TIME:20230629T073000Z DTEND;VALUE=DATE-TIME:20230629T074500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-226@indico.nevod.mephi.ru DESCRIPTION:Speakers: Leonid Ksenofontov (Yu.G. Shafer Institute of Cosmop hysical Research and Aeronomy SB RAS)\nThe results of direct measurements of the muon density in extensive air showers (EAS) with zenith angles $\\t heta \\leq 45^\\circ$ and energies $Е_0\\geq 10^{17}$ eV obtained in the Auger experiment and at the Yakutsk array are considered. In both cases mu ons were registered by underground scintillation detectors with the same t hreshold energy $Е_{\\mu}\\approx 1.0 \\times \\sec \\theta$ GeV. The mea sured values are compared with the theoretical values calculated within th e framework of QGSjet-II-04 hadron interaction model using the CORSIKA cod e. They differ from each other by the factor of 1.53 ± 0.13(stat). It is shown that this difference is due to the muon density overestimation by a factor of 1.22 and the primary energy underestimation by a factor of 1.25 in the Auger experiment.\n\nhttps://indico.nevod.mephi.ru/event/9/contribu tions/226/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/226/ END:VEVENT BEGIN:VEVENT SUMMARY:Studying muon bundles of inclined air showers in the NEVOD-DECOR e xperiment DTSTART;VALUE=DATE-TIME:20230629T071500Z DTEND;VALUE=DATE-TIME:20230629T073000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-228@indico.nevod.mephi.ru DESCRIPTION:Speakers: Aleksei Bogdanov (MEPhI)\nNEVOD-DECOR is the unique experiment where systematic studies of cosmic ray muon bundles in a wide r ange of zenith angles and\, accordingly\, the energies of primary cosmic r ays are carried out. Impressive experimental material (more than 100 thous and events) has been accumulated over a long time period from May 2012 to December 2022. The earlier developed method of local muon density spectra allows us to compare experimental data on muon bundles with the results of the EAS muon component simulations. The analysis showed that the observed intensity of muon bundles at primary cosmic ray energies of about 1 EeV a nd higher can be compatible with the expectation (in frame of widely used hadron interaction models) only under the assumption of an extremely heavy mass composition. It is consistent with data of several other experiments on investigations of air shower muon content\, but contradicts the availa ble measurements of the depth of the shower maximum in the atmosphere by m eans of fluorescent technique\, which favor a light mass composition at th ese energies. This probably leads to the need to revise the existing model s of hadronic interactions.\n\nhttps://indico.nevod.mephi.ru/event/9/contr ibutions/228/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/228/ END:VEVENT BEGIN:VEVENT SUMMARY:Current status of the TREK detector for studies of cosmic ray muon bundles at large zenith angles DTSTART;VALUE=DATE-TIME:20230628T150000Z DTEND;VALUE=DATE-TIME:20230628T151500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-249@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ivan Troshin (MEPhI)\nAt National Research Nuclear U niversity MEPhI\, a large-scale coordinate-tracking detector TREK for the study of muon bundles at large zenith angles is under construction. The de tector has an area of 250 $m^2$ and consists of two planes of multi-wire d rift chambers.\n\nIn joint operation with the Cherenkov water detector of 2000 tons of distillated water\, the TREK detector will provide on unprece dented investigation of near-horizontal flux of muon bundles generated in the interactions of ultra-high-energy cosmic rays. This research will cont ribute to resolving the «muon puzzle» concerning the origin of the exces s of cosmic ray muons\, which has been observed in such experiments as NEV OD-DECOR\, IceCube and the Pierre Auger Observatory. The report presents t he results of assembling and launching the inner plane of the TREK detecto r\, the results of the gas mixture purging\, the results of testing and pa ssportization of drift chambers on the testbench. The estimates of the eff iciency and the accuracy of track reconstruction will be discussed.\n\nhtt ps://indico.nevod.mephi.ru/event/9/contributions/249/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/249/ END:VEVENT BEGIN:VEVENT SUMMARY:Kinematic description of alignment in the Pamir experiment DTSTART;VALUE=DATE-TIME:20230628T144500Z DTEND;VALUE=DATE-TIME:20230628T150000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-222@indico.nevod.mephi.ru DESCRIPTION:Speakers: Aleksei Nikolskii (BLTP JINR)\nThe report is devoted to the geometric and kinematic description of the azimuthal correlation o f photon and hadron families\, which was observed by the Pamir collaborati on in emulsion experiments with cosmic rays. This effect is called «align ment»\, because quantitatively this feature demonstrates a deviation from the straight line of points on the emulsion film plane used for particles detection. In our approach\, it is shown that a high degree of alignment is a consequence of the selection procedure for the most energetic cluster s\, i.e. the existence of a lower energy threshold of the gamma component in the interaction products of the target nuclei and cosmic radiation toge ther with the law of conservation of their transverse momentum. The obtain ed results correct describe the maximum degree of alignment for the three points and are also close to the measurements in the Pamir experiment for the case of four and five clusters\, so the proposed method looks very pro mising for interpretation the alignment phenomenon.\n\n1. Pamir Collaborat ion\, A. Borisov et al.\, in Proceedings of 4th International Symposium on Very High Energy Cosmic Ray Interactions\, Beijing\, ed. by D. Linkai (1 986)\, p. 4\; \n2. I.P. Lokhtin\, A.V. Nikolskii\, \, A.M. Snigirev\, Eur . Phys. J. C 83\, 324 (2023)\, arXiv: 2301.07975\; \n3. I.P. Lokhtin\, A .K. Managadze\, A.M. Snigirev\, Phys. Atom. Nuclei 76\, 602–606 (2013)\; \n4. I.P. Lokhtin\, A.K. Managadze\, L.I. Sarycheva\, A.M. Snigirev\, Eur . Phys. J. C 44\, 51 (2005)\, arXiv: hep-ph/0502230\; s\n5. R.A. Mukhameds hin\, Eur. Phys. J. C 82\, 155 (2022)\, arXiv: 2207.13558.\n\nhttps://indi co.nevod.mephi.ru/event/9/contributions/222/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/222/ END:VEVENT BEGIN:VEVENT SUMMARY:Hadronization as a key to the muon puzzle DTSTART;VALUE=DATE-TIME:20230628T143000Z DTEND;VALUE=DATE-TIME:20230628T144500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-212@indico.nevod.mephi.ru DESCRIPTION:Speakers: Roman Nikolaenko ()\nThe excess of muons in ultra-hi gh energy cosmic rays (UHECR) in comparison with the results of Monte-Carl o simulations that grows with the primary particle energy is known as the muon puzzle. Since the LHC data became available\, many improvements have been done to the models of hadronic interactions used in extensive air sho wers (EAS) simulation tools. Yet the noticeable deviation from experimenta l data is observed for both so-called post-LHC models: EPOS LHC and QGSJET -II-04. The focus of theoretical works that try to solve this puzzle has s hifted towards the process of hadronization\, i. e. when partons produced in high-energy collisions combine into final state hadrons. Some attempts were made to improve the description of particle production like core-coro na effect in EPOS. But for the complete solution\, further changes are req uired.\n\n This study presents the detailed overview of models of h adronization used in several modern high-energy hadron interaction models: PYTHIA 8.3\, EPOS LHC and QGSJET-II-04. The connection to the EAS simulat ions and muon puzzle is considered. Different possibilities for further im provements of the models are discussed.\n\nhttps://indico.nevod.mephi.ru/e vent/9/contributions/212/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/212/ END:VEVENT BEGIN:VEVENT SUMMARY:Bose–Einstein condensation and muon production in ultra-high ene rgy cosmic ray particle collisions DTSTART;VALUE=DATE-TIME:20230628T141500Z DTEND;VALUE=DATE-TIME:20230628T143000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-210@indico.nevod.mephi.ru DESCRIPTION:Speakers: Vitalii Okorokov (National Research Nuclear Universi ty MEPhI)\nCollisions of cosmic ray particles with ultra-high initial ener gies larger than 0.1–1 EeV with nuclei in the atmosphere lead to creatio n a strongly interacting matter under extreme conditions and open a wide r oom for appearing of the novel dynamical features for production of second ary particles. In particular\, the estimations obtained for the space dens ity of charged particles at freeze-out and its critical value within the m odel of certain ring diagrams allow the possibility of lasing behavior for secondary pions at least for nuclear interactions with ultra-high energy cosmic ray (UHECR) particles. The pion-lasing behavior results in the shif t to larger multiplicities and\, as consequence\, can provide\, in general \, the enhanced yield of cosmic muons. The Muon puzzle is a well-known pro blem in the physics of high-energy cosmic rays one of the aspects of which is the muon bundle excess compared to simulations within available phenom enological models. In the present work critical value of the space particl e density for onset of Bose–Einstein condensation of the boson wave-pack ets into the same wave-packet state is estimated with help of the improved formula obtained within model of multiparticle symmetrization for UHECR e nergy domain. Energy dependence of mean multiplicity of pions is evaluated for the cases of absent of the Bose–Einstein effects and for presence o f laser-like behavior for pions. The possible influence of the Bose–Eins tein condensation is discussed for the muon production in UHECR particle c ollisions with the atmosphere.\n\nhttps://indico.nevod.mephi.ru/event/9/co ntributions/210/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/210/ END:VEVENT BEGIN:VEVENT SUMMARY:CMS Measurements and UHECR DTSTART;VALUE=DATE-TIME:20230628T140000Z DTEND;VALUE=DATE-TIME:20230628T141500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-218@indico.nevod.mephi.ru DESCRIPTION:Speakers: Lev Kheyn (SINP MSU)\nCMS measurementsm valuable for tuning CR generators are discussed.\n\nhttps://indico.nevod.mephi.ru/even t/9/contributions/218/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/218/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic ray accelerator in the inhomogeneous heliosphere and its im pact on the inhabitants of the Earth DTSTART;VALUE=DATE-TIME:20230628T124500Z DTEND;VALUE=DATE-TIME:20230628T130000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-237@indico.nevod.mephi.ru DESCRIPTION:Speakers: Phiilipp Vysikaylo (MRSU)\nUsing the helio-sphere as an example\, we have investigated the hypothesis that stellar winds or co smic rays originate in stars and accelerate in their star spheres in elect ric field shock waves. We have proved that a nonequilibrium inhomogeneous giant gas discharge occurs in the helio-sphere at large values of the para meter E/N\, which determines the electron temperature. This quasi-stationa ry discharge determines the main parameters of the slow solar wind (SW) in the helio-sphere. In connection with the development of space technologie s and the exit of man into outer space\, the problem of the nature of SW i s acute. The Pannekoek-Rosseland-Eddington model does not take into accoun t the important role of high-energy runaway (from the Sun) electrons and\, accordingly\, the duality of electron flows in the helio-sphere (from the Sun and towards the Sun). According to the alternative model formulated b y us\, high-energy (running away from the positively charged Sun) electron s leave the Sun and the helio-sphere\, and low-energy\, unable to leave th e Coulomb potential well - the positively charged Sun and the helio-sphere \, return to the positively charged Sun. The weak difference between the c ounter currents of high-energy (running away from the Sun) electrons and l ow-energy (returning to the Sun) electrons is compensated by the current o f positive ions and protons from the Sun - SW. These dynamic processes mai ntain a quasi-constant effective dynamic charge of the Sun and the entire helio-sphere. Quasi-neutrality on the Sun and the helio-sphere is well per formed up to 10*-36. According to experiments and analytical calculations based on our model [1]: 1) the plasma in the corona is non-equilibrium\; 2 ) maximum electron temperature Te ~ 1-2 million degrees\; 3) Te increases from 1000 km from the Sun and 4) the role of high-energy electrons emitted from the plasma leads to a significant increase in the effective: solar c harge and electric fields in the helio-sphere in relation to the Pannekoek -Rosseland-Eddington model. This is due to the absence of a compensation l ayer screening the effective solar charge. It does not form due to the run away of high-energy electrons from the entire helio-sphere with high tempe ratures above the surface of the Sun. The runaway process of high-energy e lectrons forms the internal EMF of the entire helio-sphere and a giant acc elerator of protons and α-particles in the SW. This process manifests its elf in the generation of two counter streams of particles: 1) neutral or w ith a small charge (toward the Sun) and 2) in the form of high-energy elec trons (escaping from a positively charged Sun) and 3) the formation of a s olar wind with positively charged ions with Z/M ≥ 0.107 (from the positi vely charged Sun). The calculated values of the ion parameters in the sola r wind are compared with experimental observations. The velocities of prot ons in the SW are determined by their birthplace in the helio-sphere and c an exceed 1200 km/s. The influence of SW protons on the well-being of the inhabitants of the Earth is discussed.\n[1] Vysikaylo P.I. Quantitative I nvestigation Nonequilibrium Inhomogeneous Plasma of the Helio-sphere with Runaway Electrons IEEE Transactions on Plasma Science 2022\, V.50\, Issue 4\, pp. 810-816. DOI: 10.1109/TPS.2022.3160189\n\nhttps://indico.nevod.mep hi.ru/event/9/contributions/237/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/237/ END:VEVENT BEGIN:VEVENT SUMMARY:High-energy magnetospheric electron flux enhancements and the para meters of interplanetary and near-Earth medium DTSTART;VALUE=DATE-TIME:20230628T123000Z DTEND;VALUE=DATE-TIME:20230628T124500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-213@indico.nevod.mephi.ru DESCRIPTION:Speakers: Olga Kryakunova (Institute of Ionosphere)\nBased on the data of 35-year (1987-2021) measurements of magnetospheric electron fl uxes with energy >2 MeV in geostationary orbits\, solar wind speed and geo magnetic activity\, a catalog of electron flux enhancements was compiled i n which the electron fluence exceeds $10^8$ $cm^{-2} sr^{–1} day^{–1}$ . The epoch superposition method performed using the GOES-13 spacecraft da ta shows that large electron flux enhancements are preceded by a significa nt increase in the solar wind velocity and the Ap index of geomagnetic act ivity\, and immediately before the increase the relativistic electron flux decreases. Based on the calculated mean values of the electron fluences\, solar wind velocity\, and Ap-index of geomagnetic activity on the day of electron enhancement and on previous days\, a typical behavior of these pa rameters during and before an electron flux enhancement was obtained. The average characteristics of electron flux enhancements and the parameters o f interplanetary and near-Earth medium are calculated before large electro n flux enhancements. It is shown that the greater the increase in solar wi nd velocity and geomagnetic activity the larger the subsequent electron fl ux enhancement. The density and vector anisotropy of galactic cosmic rays for 453 events of high-energy magnetospheric electron flux enhancements ov er the period 1996-2020 were calculated by the Global Survey Method (GSM). Some examples of these events\, which are characteristic of different cla sses of solar sources\, are considered.\n\nhttps://indico.nevod.mephi.ru/e vent/9/contributions/213/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/213/ END:VEVENT BEGIN:VEVENT SUMMARY:Testing the mezofractal power spectrum for ISM by comparing with n umerical MHD calculations DTSTART;VALUE=DATE-TIME:20230628T121500Z DTEND;VALUE=DATE-TIME:20230628T123000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-260@indico.nevod.mephi.ru DESCRIPTION:Speakers: Ilya Kozhemyakin (Ulyanovsk State University)\nFor u nderstanding cosmic ray propagation through the interstellar medium (ISM)\ , an adequate model for the latter is needed. The ordinary diffusion appro ach\, leading to the Brownian motion\, assumes independence of ISM local i nhomogeneities\, such as molecular clouds and magnetic fluctuations. The l ong-range turbulent correlations created by magnetic force lines and gravi tation forces require a special representation of these ISM properties. Pu re power kind turbulent spectra occur to be too poor for this aim\, and mo reover\, do not show acceptable agreement with last MHD calculation result s. A more perspective spectra is obtained on the basis of statistical mech anics and promises to be more efficient. These include the Uchaikin-Zolota rev four-parameter mesofractal power spectrum [1]\, obtained by solving th e Ornstein-Zernike equation using three-dimensional stable Levi-Feldheim d istributions. These parameters provide its flexibility (the ability to app roximate well the numerical results of various calculations) and are easil y amenable to kinetic interpretation within the framework of the concept o f Markov breaking chains [2].\nThe report shows successful applications of this spectrum to the approximation of the numerical results of two MHD ca lculations [3\,4].\n\nReferences:\n\n1. Uchaikin\, V.V.\; Zolotarev\, V.M. Chance and Stability. Stable Distributions and Their Applications\, VSP\, Utrecht\, 1999.\n2. Uchaikin\, V.V.\; Kozhemyakin\, I.I. A Mesofractal Mo del of Interstellar Cloudiness. Universe. 2022\; 8(5):249. \n3. Burkhart\, B.\; Lazarian\, A.\; Ossenkopf\, V.\; Stutzki\, J. The turbulence power s pectrum in optically thick interstellar clouds. Astrophys. J. 2013\, 771\, 123.\n4. Falceta-Gonçalves\, D.\, Kowal\, G.\, Falgarone\, E.\, & Chian\ , A. L. (2014). Turbulence in the interstellar medium. Nonlinear Processes in Geophysics\, 21(3)\, 587-604.\n\nhttps://indico.nevod.mephi.ru/event/9 /contributions/260/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/260/ END:VEVENT BEGIN:VEVENT SUMMARY:Calculation of geomagnetically trapped proton flux from the PAMELA experimental data. DTSTART;VALUE=DATE-TIME:20230628T120000Z DTEND;VALUE=DATE-TIME:20230628T121500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-196@indico.nevod.mephi.ru DESCRIPTION:Speakers: Vitaly Malakhov (NRNU MEPhI)\nThe special interest t o the estimation of trapped proton intensities in low-altitude region of t he near-terrestrial space environment concerns their effects on numerous r obotic and manned missions. The main part of radiation exposure comes from the space region where the trajectory of mission orbit pass through the S outh Atlantic anomaly (SAA).\nAt present time\, the nature of long-term ma gnetic trapping of protons is well established. The main sources of trappe d protons are cosmic ray albedo neutron decay (CRAND) and injected solar p rotons. The contribution from solar protons prevail at energies <100 MeV a nd L>1.3\, while the influence of CRAND dominates otherwise. Inelastic nuc lear scattering\, energy transfer to plasma electrons and ionization of th e neutral atmosphere\, provides the losses.\nRecently the measurements of the geomagnetically trapped proton fluxes for the kinetic energy interval ranging from 80 MeV to the highest trapping energies (2 GeV) were fulfille d by the PAMELA mission at low Earth orbits (350 ÷ 610 km). Protons flux properties were investigated in detail\, providing a full characterization of the particle radiation in the SAA region\, including locations\, energ y spectra\, and pitch angle distributions. To analyze data the standard ap proach developed in 1995 by SAMPEX team was introduced. To reconstruct the intensities of trapped particles\, the effective areas\, averaged over gy ro phase angle\, are calculated as function of pitch angle for different i nstrument orientations respective geomagnetic field vector. Therefore\, th e numerous simulations are fulfilled varying pitch angle and telescope axi s orientation angles in steps (energy bins varying is separate point).\nIn this report\, we propose another variant of trapped particles intensity r econstruction. Instead of multiple effective area calculations\, the value of effective acceptance is estimated for fixed instrument orientation and pitch angle from one simulation sample (for given energy bin) of data in ordinary way with isotropic flux incidence. In this procedure\, the additi vity of acceptance for different regions of allowed directions is used.\n\ nhttps://indico.nevod.mephi.ru/event/9/contributions/196/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/196/ END:VEVENT BEGIN:VEVENT SUMMARY:The modeling of the cosmic ray particles interaction with the Eart h's atmosphere during the GLE events DTSTART;VALUE=DATE-TIME:20230628T114500Z DTEND;VALUE=DATE-TIME:20230628T120000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-250@indico.nevod.mephi.ru DESCRIPTION:Speakers: Evgenii Maurchev (IZMIRAN)\nThe work presents the re sults of calculations of the cosmic ray protons propagation through the Ea rth's atmosphere using the Monte Carlo method. We developed the model for this modeling with the GEANT4 software development toolkit. It uses the st andard QGSP_BERT_HP class to describe the physics of the particle interact ions with matter. The general results are a quantitative estimated seconda ry particle fluxes (neutrons\, muons\, electrons\, positrons and photons i n the wide energy region)\, as well as the ionization count rate in compar ison only with the galactic cosmic rays. In this work we have considered t hree GLE events (№ 65\, № 69 and № 70). Moreover\, it is taken into account that there are two components in the spectrum of primary cosmic ra ys\, prompt and delayed (in accordance with the work on assessing the feat ures of the spectrum of relativistic solar protons using the GLE modeling technique).\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/250/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/250/ END:VEVENT BEGIN:VEVENT SUMMARY:Formation of a Forbush decrease in a magnetic cloud by the electro magnetic mechanism DTSTART;VALUE=DATE-TIME:20230628T113000Z DTEND;VALUE=DATE-TIME:20230628T114500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-208@indico.nevod.mephi.ru DESCRIPTION:Speakers: Anastasia Petukhova (Yu.G. Shafer Institute of Cosmo physical Research and Aeronomy)\nWe calculate cosmic ray intensity and ani sotropy using the model of the Forbush decrease formation in a magnetic cl oud by the electromagnetic mechanism for three events. The properties of t he Forbush decrease are determined by solving the Boltzmann kinetic equati on without particle scattering. Geometrical parameters of the magnetic clo ud\, such as velocity\, velocity gradient\, cross-section area\, and angul ar sizes\, are based on the kinematic model. The magnetic field properties and the type of helical structure near the Sun are based on the Miller an d Turner toroidal model. In interplanetary space\, magnetic field componen ts are determined by the frozen-in condition. The model properties of the velocity\, velocity gradient\, magnetic field components\, and characteris tics of the Forbush decrease roughly agree with measurements in three even ts. There are no free parameters in the Forbush decrease formation model.\ n\nhttps://indico.nevod.mephi.ru/event/9/contributions/208/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/208/ END:VEVENT BEGIN:VEVENT SUMMARY:Study of anomalous events in the TUS experiment DTSTART;VALUE=DATE-TIME:20230628T100000Z DTEND;VALUE=DATE-TIME:20230628T101500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-253@indico.nevod.mephi.ru DESCRIPTION:Speakers: Aleksandr Blinov ()\nThe TUS experiment was the firs t detector to measure the fluorescence and Cherenkov radiation of extensiv e air showers (EAS) in the Earth's atmosphere from space orbit. The main g oal of the TUS experiment was to search for and study ultra high-energy co smic rays with energies E > 70 EeV. The TUS detector registered a number o f unusual events\, the origin of which is unclearwith an anomalously large number of active pixels . To clarify the nature of these events\, a more detailed analysis has been carried out and preliminary results are present ed.Various variants of the nature of the appearance of anomalous events ar e discussed: cosmological gamma-ray bursts (GRB)\, synchrotron radiation o f galactic electrons in the geomagnetic field\, as well as reflection in t he solar panels of the satellite of fluorescent and Cherenkov radiation of out-of-aperture EASs\, accompanied by lightning discharges in the atmosph ere.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/253/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/253/ END:VEVENT BEGIN:VEVENT SUMMARY:Investigation of the large-scale distribution of the arrival point s of 1-100 PeV EAS detected at the Tien Shan cosmic ray installation DTSTART;VALUE=DATE-TIME:20230628T094500Z DTEND;VALUE=DATE-TIME:20230628T100000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-214@indico.nevod.mephi.ru DESCRIPTION:Speakers: Alexander Shepetov (Lebedev Physical Institute)\, Vl adimir Ryabov (Lebedev Physical Institute)\nA set of eight scintillators w ith the reduced to (50-70)ns width of their output pulse signals is applie d for determination of the arrival directions of extensive air showers whi ch are effectively detected by the Tien Shan shower installation in the en ergy range between 1 and 100 PeV. Up to the present time\, about ~$10^6$ s hower events applicable for deducing their directional angles were collect ed in 2021-2023 during the ~5500h of the installation operation life time. Here\, the statistical characteristics of these events are presented whic h confirm the functioning correctness of the electronic hardware and mathe matical algorithms applied for the treatment of the initial measurement da ta. Further on\, the newly obtained information on the angular distributio n of the EAS arrival points is supposed to be used for a study of the larg e-scale anisotropy of the PeV cosmic rays on the celestial sphere by appli cation of the difference method which has been earlier developed for this purpose in the LPI.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions /214/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/214/ END:VEVENT BEGIN:VEVENT SUMMARY:On the nature of cosmic ray transport nonlocality DTSTART;VALUE=DATE-TIME:20230628T093000Z DTEND;VALUE=DATE-TIME:20230628T094500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-194@indico.nevod.mephi.ru DESCRIPTION:Speakers: Vladimir Uchaikin (Ulyanovsk State University)\nThe commonly accepted CR transport theory is based on the diffusion equation\, which in turn follows from the Boltzmann kinetic equation. The latter was derived for multiple collisions of particles with local formations (atoms \, molecules) under the assumption of their statistical independence\, mor e precisely\, of the Poisson nature of the ISM ensemble. It is this proper ty that is responsible for the appearance of local operators in diffusion- type equations. However\, the interstellar cloud structure\, coupled with its turbulent nature\, is an example of a strongly correlated medium whose motion cannot be described in terms of perturbation theory. To describe i t\, the author proposed a generalization of the Ornstein-Zernike integral equation for the ISM correlation function (in terms of cloud concentration )\, which is consistent with the results of numerical MHD calculations and observation data. The important mathematical tool connecting two dynamica l systems (CR and ISM) is a new 4-parameter approximation of the power spe ctrum of turbulent fluctuations. It is consistent with the classical power forms in the inertial interval and gives a smooth transition beyond its l imits.\n\nThe report unfolds the logic of the appearance on the stage of n on-local operators (fractional derivatives)\,\nconcept of fractals and mul tifractals. The latter also includes the mesofractal ISM model discussed i n the report\, which demonstrates fractal properties on small scales and t ransforms into a homogeneous medium upon transition to large scales. In ot her words\, this model has asymptotic locality\, and one can speak of a lo cality horizon beyond which the usual transfer theory becomes valid.\n\nht tps://indico.nevod.mephi.ru/event/9/contributions/194/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/194/ END:VEVENT BEGIN:VEVENT SUMMARY:Where are the pevatrons that form the knee in the spectrum of the cosmic ray nucleon component around 4 PeV? DTSTART;VALUE=DATE-TIME:20230628T091500Z DTEND;VALUE=DATE-TIME:20230628T093000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-255@indico.nevod.mephi.ru DESCRIPTION:Speakers: Nikolay Volkov (Altai State University)\nThe paper d iscusses an approach that made it possible to estimate the distance to the nearest pevatrons\, which form a break in the spectrum of the cosmic ray nucleon component of about 4 PeV. It is based on the spectra of nucleons a nd electrons obtained by the authors in the framework of the superdiffusio n model of nonclassical CR diffusion\, which have a break\, on the assumpt ion that nucleons and electrons are accelerated by the same sources and th eir propagation in an inhomogeneous turbulent galactic medium is character ized by the same diffusion coefficient\, and also on the break in the spec trum of the electronic component in the region of 0.9 TeV\, established in the DAMPE experiment.\n\nIt is shown that pevatrons\, which form a break in the spectrum of the cosmic ray nucleon component of about 4 PeV\, are l ocated at distances of the order of 1 kpc from the Earth.\n\nhttps://indic o.nevod.mephi.ru/event/9/contributions/255/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/255/ END:VEVENT BEGIN:VEVENT SUMMARY:Combined diffusive shock and shear acceleration in astrophysical j ets DTSTART;VALUE=DATE-TIME:20230628T090000Z DTEND;VALUE=DATE-TIME:20230628T091500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-195@indico.nevod.mephi.ru DESCRIPTION:Speakers: Vladimir Zirakashvili (Pushkov Institute of Terrestr ial Magnetism\, Ionosphere and Radiowave Propagation\, Moscow\, Russia)\nA cceleration of cosmic rays in astrophysical jets is investigated. Particl es are \n accelerated at the outer bow shock and by shear flows in the je t cocoon. \nApplications for the origin and chemical composition of \nultr a high energy cosmic rays are discussed.\n\nhttps://indico.nevod.mephi.ru/ event/9/contributions/195/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/195/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic ray sources in the Galaxy DTSTART;VALUE=DATE-TIME:20230628T080000Z DTEND;VALUE=DATE-TIME:20230628T083000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-265@indico.nevod.mephi.ru DESCRIPTION:Speakers: Andrey Bykov (Ioffe Institute)\nCosmic ray sources i n the Galaxy\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/265/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/265/ END:VEVENT BEGIN:VEVENT SUMMARY:A new approach to determination of the cosmic ray composition DTSTART;VALUE=DATE-TIME:20230628T073000Z DTEND;VALUE=DATE-TIME:20230628T080000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-264@indico.nevod.mephi.ru DESCRIPTION:Speakers: Sergey Shaulov (FIAN)\nA new approach to determinati on of the cosmic ray composition\n\nhttps://indico.nevod.mephi.ru/event/9/ contributions/264/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/264/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic rays\, their role in atmospheric phenomena DTSTART;VALUE=DATE-TIME:20230628T070000Z DTEND;VALUE=DATE-TIME:20230628T073000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-263@indico.nevod.mephi.ru DESCRIPTION:Speakers: Yuri Stozhkov (Lebedev Physical Institute of RAS)\nC osmic rays\,their role in atmospheric phenomena.\n\nhttps://indico.nevod.m ephi.ru/event/9/contributions/263/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/263/ END:VEVENT BEGIN:VEVENT SUMMARY:Event reconstruction method in a hybrid muon hodoscope DTSTART;VALUE=DATE-TIME:20230627T144500Z DTEND;VALUE=DATE-TIME:20230627T150000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-227@indico.nevod.mephi.ru DESCRIPTION:Speakers: Nikita Pasiuk ()\nThe method of event reconstruction and obtaining of muonographs by a new hybrid muon hodoscope is considered . The design of the developed hodoscope is described. The first results of measurements\, as well as the obtained estimates of the angular and coord inate accuracy of the detector are discussed.\n\nThe muonography method is based on the registration of the penetrating component of cosmic rays (mu ons) and makes it possible to obtain images of various objects. In order t o implement the muonography method for studying large-scale objects\, a ne w wide-aperture precision hybrid muon hodoscope was created. This hodoscop e consists of two complementary recording systems - a scintillation strip detector and a drift tube detector. Alternating coordinate planes of the d etectors\, each with a sensitive area of 3×3 m2\, are fixed in a common f rame placed on a movable wheeled turntable.\n\nTo reconstruct events in th e drift detector\, the method of spatio-temporal clustering of signals by the drift time in the tubes is used. After the selection of hits from sing le cosmic muons\, the search for intersections of tangent lines between th e coordinate planes of the hodoscope\, the reconstruction of the muon trac k\, and the subsequent obtaining of muonographs follow. In the scintillati on hodoscope\, for the reconstruction of the muon track\, a two-coordinate method of searching for a straight line from triggered scintillation stri ps is used.\n\n*Keywords: Cosmic ray muons\, hybrid particle detectors\, d rift tubes\, muon hodoscope\, muonography\, muon tomography.*\n\nhttps://i ndico.nevod.mephi.ru/event/9/contributions/227/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/227/ END:VEVENT BEGIN:VEVENT SUMMARY:Influence of atmospheric fronts on cosmic ray muon flux DTSTART;VALUE=DATE-TIME:20230627T143000Z DTEND;VALUE=DATE-TIME:20230627T144500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-247@indico.nevod.mephi.ru DESCRIPTION:Speakers: Stanislav Timakov (MEPhI)\nA new approach to the ana lysis of muon flux during atmospheric fronts passage is discussed. It is p ossible to select muons in specific planes providing different counting ra te series that can reveal atmospheric waves that may accompany phenomena l ike the passage of atmospheric fronts. The plane includes muons from all z enith angles and some azimuth angles. This selection is made possible by t he URAGAN muon hodoscope\, which detects muons from all directions and rec ords them in matrices of zenith and azimuth angles. The value in the matri x cell corresponds to the number of muons in a specific range of angles. T he experimental setup consists of three supermodules that operate separate ly and independently from each other. It is possible to compare data from individual supermodules with each other and thus extract a useful signal. Data corresponding to the movement of atmospheric fronts above Moscow are examined. In the study\, warm\, cold\, and occluded fronts are considered. The new approach to processing of experimental data allows us to see wave s from approximately 60% of atmospheric fronts.\n\nhttps://indico.nevod.me phi.ru/event/9/contributions/247/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/247/ END:VEVENT BEGIN:VEVENT SUMMARY:The latest results obtained on the LVD experiment DTSTART;VALUE=DATE-TIME:20230627T141500Z DTEND;VALUE=DATE-TIME:20230627T143000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-197@indico.nevod.mephi.ru DESCRIPTION:Speakers: Natalia Filimonova ()\nThe LVD detector\, located i n the Gran Sasso Laboratory at a depth of 3600 m a.e.\, is designed for re search in the field of neutrino physics\, astrophysics\, cosmic ray physic s and the search for rare processes predicted by theory. The LVD experimen t was built in 1991 to register neutrinos from collapses of stellar nuclei in our galaxy. The background of the detector is atmospheric muons\, neut rons generated by muons in the detector material and natural radioactivity underground. The report presents the latest experimental results obtained at LVD: a limit on the frequency of supernova outbreaks\, muon variations with a period of 1\, 4\, 10 years\, and also describes the problems of st udying the low-energy background underground.\n\nhttps://indico.nevod.meph i.ru/event/9/contributions/197/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/197/ END:VEVENT BEGIN:VEVENT SUMMARY:A nuclear emulsion detectors for the muonography of underground st ructure of Holy Dormition Pskov-Caves Monastery DTSTART;VALUE=DATE-TIME:20230627T140000Z DTEND;VALUE=DATE-TIME:20230627T141500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-189@indico.nevod.mephi.ru DESCRIPTION:Speakers: Natalia Polukhina (Lebedev Physical Institute\, Russ ian Academy of Sciences\, Moscow\, Russia)\nMethods for visualizing the st ructure of large\, up to kilometer-sized objects based on recording the de gree of absorption of atmospheric muons\, which are called muonography\, u se the abundant natural flux of muons resulting from the interaction of co smic rays in the atmosphere. In recent years\, there has been an active de velopment of muonography in various innovative interdisciplinary approache s to the study of the internal structure of natural or artificial structur es\, the establishment of synergy between elementary particle physics and archeology. The paper presents the first results of a study of a unique un derground structure of the Holy Dormition Pskov-Caves Monastery with a lon g history.\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/189/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/189/ END:VEVENT BEGIN:VEVENT SUMMARY:High Energy Ray Observatory\, optimization and current status DTSTART;VALUE=DATE-TIME:20230627T123000Z DTEND;VALUE=DATE-TIME:20230627T124500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-231@indico.nevod.mephi.ru DESCRIPTION:Speakers: Dmitry Podorozhny (M.V.Lomonosov Moscow State Univer sity)\nThe High-Energy Ray Observatory (HERO) is a space experiment based on a heavy ionization calorimeter for direct study of cosmic rays. The eff ective geometric factor of the apparatus is not less than 12m2sr for proto ns and not less than 18m2sr for nuclei and electrons. During the exposure for ∼5-7 years this mission will make it possible to measure energy spec tra of all abundant cosmic ray nuclei in the knee region (∼3 PeV) with i ndividual resolution of charges with energy resolution better than 30% and provide useful information to solve the puzzle of the cosmic ray knee ori gin. HERO mission will make it also possible to measure energy spectra of cosmic rays nuclei for energies 1-1000 TeV with very high precision and en ergy resolution (up to 3% for calorimeter 70 tons) and study the fine stru cture of the spectra. The current status of the space mission is discussed .\n\nhttps://indico.nevod.mephi.ru/event/9/contributions/231/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/231/ END:VEVENT BEGIN:VEVENT SUMMARY:Development of an EAS type identification method based on an artif icial neural network for the TAIGA experiment DTSTART;VALUE=DATE-TIME:20230627T121500Z DTEND;VALUE=DATE-TIME:20230627T123000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-257@indico.nevod.mephi.ru DESCRIPTION:Speakers: Evgeniy Kravchenko (NSU/BINP)\nThe TAIGA experiment in Tunka valley is expanding the present scintillation detector array with new TAIGA-Muon detector stations. A simulation model was developed for th e new stations optimization and study of the identification performance of the array together with HiScore optical stations system. The extensive ai r showers (EASs) were simulated with the CORSIKA simulation tool\, and the detector response was simulated with the GEANT4 package. EASs induced by gamma quanta\, proton and nuclei from He to Fe at energies 1 and 3 PeV hav e been studied. For the identification of the EAS origin\, a method based on a neural network was suggested. Preliminary results show that with this method\, using information from scintillation and optical detectors it is possible to achieve proton EAS suppression factor of 1000 while having ga mma-quanta EAS detection efficiency about 50%. The analogous method was te sted for cosmic rays element composition study. Three groups of elements - - p-He\, CNO and Fe could be separated with efficiencies variyng from 30 t o 90% depending on the EAS type and predefined cuts.\n\nhttps://indico.nev od.mephi.ru/event/9/contributions/257/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/257/ END:VEVENT BEGIN:VEVENT SUMMARY:Magnetorotational supernova neutrino emission spectra and prospect s for observations by large-size underwater telescopes DTSTART;VALUE=DATE-TIME:20230627T120000Z DTEND;VALUE=DATE-TIME:20230627T121500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-204@indico.nevod.mephi.ru DESCRIPTION:Speakers: Vladimir Kondratyev (ОИЯИ)\nWe analyze neutrino fluxes near the surface of a protoneutron star in type II supernova explos ions at core-collapse regime. For dynamoactive supernovae it is shown that effective neutrino collisions in a magnetized nucleon gas caused by the n eutral current Gamow-Teller component lead to neutrino acceleration. Such an effect originates from spin-projection asymmetry in phase space volume of outer channel neutrino due to nucleon magnetic moment interaction with a field. Respective increase in a hardness of the energy spectrum is favor able for observations of supernova neutrinos using neutrino telescopes. Th e possibilities of detecting supernova neutrinos by large-volume Cherenkov observatories: KM3NeT and Baikal-GVD\, are discussed. As is demonstrated the upper limits of the distance thresholds for such observations can be i ncreased by a factor of 1.5 √k when employing the k-fold coincidence t echnique in data processing.\n\nhttps://indico.nevod.mephi.ru/event/9/cont ributions/204/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/204/ END:VEVENT BEGIN:VEVENT SUMMARY:Solar radio bursts in the Radio Neutrino Observatory in Greenland RNO-G DTSTART;VALUE=DATE-TIME:20230627T114500Z DTEND;VALUE=DATE-TIME:20230627T120000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-261@indico.nevod.mephi.ru DESCRIPTION:Speakers: Maria Mikhailova ()\nNeutrino radio detectors are de signed to target the first measurement of neutrinos beyond energies of ∼ 10 PeV. Several such radio detectors operate in Antarctica. They are scann ing the ice sheet in search of Askaryan radio emission from neutrino induc ed showers. The Radio Neutrino Observatory in Greenland (RNO-G)\, designed to monitor ultra-high-energy neutrinos in the northern hemisphere\, is un der construction. It currently has 7 of 35 stations with antennas inside t he ice and on the surface. Antennas on the surface should also measure rad io emissions from down-coming cosmic rays. The radio observatory may also be sensitive to solar radio bursts\, which will be a background for cosmi c rays. On the other hand\, solar flares also present a unique opportunity for detector calibration. This contribution presents the results of a sea rch for solar bursts in RNO-G data and demonstrates what calibration possi bilities can be derived from solar flare data.\n\nhttps://indico.nevod.mep hi.ru/event/9/contributions/261/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/261/ END:VEVENT BEGIN:VEVENT SUMMARY:The Baikal-GVD neutrino telescope: current status and development prospects DTSTART;VALUE=DATE-TIME:20230627T113000Z DTEND;VALUE=DATE-TIME:20230627T114500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-219@indico.nevod.mephi.ru DESCRIPTION:Speakers: Vladimir Aynutdinov (INR RAS)\nCurrently\, the deplo yment of the Baikal-GVD neutrino telescope is successfully underway in Lak e Baikal. Baikal-GVD now comprises 96 strings with 3456 optical modules. W e present the current status and plans for further deployment of the Baika l-GVD telescope and discuss issues related to the creation of a next-gener ation neutrino telescope in Lake Baikal.\n\nhttps://indico.nevod.mephi.ru/ event/9/contributions/219/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/219/ END:VEVENT BEGIN:VEVENT SUMMARY:Techniques for data analysis and primary mass reconstruction in th e ENDA experiment DTSTART;VALUE=DATE-TIME:20230627T101500Z DTEND;VALUE=DATE-TIME:20230627T103000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-198@indico.nevod.mephi.ru DESCRIPTION:Speakers: Kirill Kurinov (INR RAS)\nAs part of the high-altitu de LHAASO project\, ENDA (Electron Neutron Detector Array) is being create d in China. The concept of the ENDA consists in simultaneous registration of the electromagnetic and thermal neutron components (being a part of had ronic component) of the EAS. The report provides a brief overview of analy tical and ML (Machine Learning) methods for shower and primary particle pa rameters reconstruction for simulation data. Also methods for estimation t he uncertainty of such reconstruction is presented.\n\nhttps://indico.nevo d.mephi.ru/event/9/contributions/198/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/198/ END:VEVENT BEGIN:VEVENT SUMMARY:Title: Progress of Electron-Neutron Detector Array (ENDA) DTSTART;VALUE=DATE-TIME:20230627T100000Z DTEND;VALUE=DATE-TIME:20230627T101500Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-200@indico.nevod.mephi.ru DESCRIPTION:Speakers: Mao-Yuan Liu (Science School\, Tibet University\, Lh asa\, Tibet 850000\, China)\nAbstract-The origin of cosmic rays can be dec iphered by accurately measuring the components and energy spectrum in the knee region. Extensive air shower (EAS) studies rely on information provid ed by secondary high energy hadrons\, which generate evaporation neutrons when they interact with matter in the environment. In the early 21st centu ry\, the electron-neutron detector (EN-detector) was developed at the Inst itute for Nuclear Research of the Russian Academy of Science (INR RAS). Th e PRImary Spectrum Measurement Array (PRISMA) project was introduced to en hance the array capabilities of cosmic ray composition separation and impr ove measurement accuracy. Within the framework of Chinese-Russian cooperat ion\, at the Large High Altitude Air Shower Observatory (LHAASO) at Mt. Ha izi (4400 m a.s.l.) in Daocheng\, Sichuan province\, China\, a proposal wa s launched to establish the EN-Detector Array (ENDA) composed of 400 detec tors in area of $10\,000 m^{2}$ to measure cosmic rays up to 300 PeV. In 2 018\, a cluster\, having 16 EN-detectors\, at Tibet University (TU) in Lha sa\, Tibet\, China (3700 m a.s.l.) was built to test specification of the array. Since 2019\, another cluster so called ENDA-16 has started running at LHAASO\, and here we give the first result of thermal neutron distribut ion. After gaining experience from these previous works\, since April 2023 \, we have successfully extended ENDA to ENDA-64 composed of 64 detectors in area of $1\,000 m^{2}$ at LHAASO to measure cosmic rays from 400TeV to 20 PeV\, and we will describe status of ENDA-64 and hybrid detection of co smic ray by using ENDA and LHAASO.\n\nhttps://indico.nevod.mephi.ru/event/ 9/contributions/200/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/200/ END:VEVENT BEGIN:VEVENT SUMMARY:Overview on EAS neutrons: recording and simulations DTSTART;VALUE=DATE-TIME:20230627T093000Z DTEND;VALUE=DATE-TIME:20230627T100000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-233@indico.nevod.mephi.ru DESCRIPTION:Speakers: Yuri Stenkin (INR RAS)\nInterest to study neutrons p roduced in Extensive Air Showers (EAS) is rising last years. Recent public ations on this subject are overviewed and estimated. Advantages of the met hod to study hadronic component being the main EAS component\, as well as perspectives of the method are shown.\n\nhttps://indico.nevod.mephi.ru/eve nt/9/contributions/233/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/233/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic rays data for Space Weather forecasting DTSTART;VALUE=DATE-TIME:20230627T090000Z DTEND;VALUE=DATE-TIME:20230627T093000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-244@indico.nevod.mephi.ru DESCRIPTION:Speakers: Maria Abunina (IZMIRAN)\nWhen we speak on Space Weat her we are commonly meaning the radiation and electro magnetic conditions in the near Earth space. Cosmic ray variations define directly a radiation situation. And they are also related to the variations of electromagnetic conditions in the interplanetary space and Earth’s magnetosphere. This makes cosmic ray variations one of the important resources for validating the space weather state and forecasting its changes.\n\nhttps://indico.nev od.mephi.ru/event/9/contributions/244/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/244/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino telescope Baikal-GVD: status and results DTSTART;VALUE=DATE-TIME:20230627T073000Z DTEND;VALUE=DATE-TIME:20230627T080000Z DTSTAMP;VALUE=DATE-TIME:20260906T174359Z UID:indico-contribution-9-243@indico.nevod.mephi.ru DESCRIPTION:Speakers: Zhan-Arys Dzhilkibaev ()\nThe progress in the constr uction and operation of the Baikal Gigaton Volume Detector in Lake Baikal is reported. The detector is designed for search for high energy neutrinos whose sources are not yet reliably identified. It currently includes over 3500 optical modules arranged on 98 strings\, providing an effective volu me of 0.6 km3 for cascades with energy above 1 PeV. We review the scienti fic case for Baikal-GVD\, and first results from the partially built exper iment\, which is currently the largest neutrino telescope in the Northern Hemisphere and still growing up.\n\nhttps://indico.nevod.mephi.ru/event/9/ contributions/243/ LOCATION:National Research Nuclear University MEPhI B-100 URL:https://indico.nevod.mephi.ru/event/9/contributions/243/ END:VEVENT END:VCALENDAR