The 2nd international conference on particle physics and astrophysics

Nuclotron-based Ion Collider fAcility (the NICA project) is under construction at the Joint Institute for Nuclear Research (JINR, Dubna). The corresponding experimental program includes a study of hot and dense strongly interacting matter in heavy ion collisions (up to gold) in the energy range up to√ s_NN = 11 GeV and an investigation of the nucleon spin structure in collisions of polarized protons and deuterons at the energy up to √ s = 27 GeV. Two experiments are in preparation to study heavy ion collisions, the MPD detector at the collider, and experiment BM@N with extracted beams. The nucleon spin structure will be studied with the SPD detector at the collider. Designed average luminosity of collider is 10E27 cm-2 s-1 for Au(79+) and 10E32 for polarized protons. The proposed experimental program allows one to search for manifestations of the phase transitions and critical phenomena and shed light on the nucleon spin structure dynamics.

The 2nd LHC run has started in 2015 with a pp centre-of-mass collision energy of 13 TeV and ATLAS has taken more than 20 fb-1 of data at the new energy by 2016 summer. In this talk, an overview is given on the ATLAS data taking and the improvements made to the ATLAS experiment during the 2-year shutdown 2013/2014. Selected new results from the recent data analysis from ATLAS is also presented.

The recent experimental results on spectroscopy, decay and production of charmonium and charmoniumlike states obtained by Belle, BaBar, BES and LHCb experiments still require a consistent theoretical understanding. We present experimental status of charmonium physics including discussion of the new standard and exotic charmonium states. We also discuss the future perspectives of charmonium physics.

After the successful operation at the center-of-mass energies of 7 and 8 TeV in 2010 - 2012, the LHC is ramped up and successfully took data at the center-of-mass energies of 13 TeV in 2015. Meanwhile, plans are actively advancing for a series of upgrades of the accelerator, culminating roughly ten years from now in the high-luminosity LHC (HL-LHC) project, delivering of the order of five times the LHC nominal instantaneous luminosity along with luminosity leveling. The ultimate goal is to extend the dataset from about few hundred fb−1 expected for LHC running to 3000 fb−1 by around 2035 for ATLAS and CMS. The challenge of coping with the HL-LHC instantaneous and integrated luminosity, along with the associated radiation levels, requires further major changes to the ATLAS detector. The designs are developing rapidly for a new all-silicon tracker, significant upgrades of the calorimeter and muon systems, as well as improved triggers and data acquisition. ATLAS is also examining potential benefits of extensions to larger pseudorapidity, particularly in tracking and muon systems. This report summarizes various improvements to the ATLAS detector required to cope with the anticipated evolution of the LHC luminosity during this decade and the next. A brief overview is also also given on physics prospects with a pp centre-of-mass energy of 14 TeV.

To investigate the effects of intense radiation on the operation of the liquid xenon spectrometer was created apparatus complex based on liquid xenon detector. The experimental setup consists of a multifunctional chamber, gas system, cooling system, temperature control system, a special preamp, passive protection, scintillation monitor the accelerator beam, thermoluminescent dosimeters. Multifunctional chamber includes a detecting unit (flat or cylindrical ionization chamber), the cleaning unit of the xenon, control unit of the purity of liquid xenon. The liquid xenon detector was irradiated by bremsstrahlung pulses of the microtron. The frequency of irradiation pulses was 400 Hz. The absorbed dose was varied from 10-7 to 0.1 Gy per pulse. The electronic and ionic processes in liquid xenon at different radiation doses were investigated. Stable operation of the liquid xenon spectrometer in the intervals between the pulses of the accelerator shown for a long time.

We study observables sensitive to tensor structure of interactions of a hypothetical heavy spin-0 boson. It is assumed that interactions of this particle are dominated by interactions with photons. The interactions with other vector bosons and quarks are supposed to be suppressed. The above assumptions favor the production of this hypothetical particle through the vector boson fusion mechanism structurally dominated by the photon and Z-interactions. This particle will be produced in association with two light quarks. It is shown that the azimuthal angle difference between the tagging jets provides an observable to probe the tensor structure of the interaction vertices of such hypothetical particle.

To search cosmic ray Erzions the telescope "Doch-4AM" was used. For the digitization and transmission to the personal computer of scintillation detectors amplitudes the new LA-n10-12 two-channel ADC circuit became used. The thick amount (ρh$\sim$60g/cm2) of arid soda (Na2CO3), surrounded by the thick amount ($\rho$h$\sim$120g/cm2) of graphite been chosen for the optimum converter-material placed on the Al ($\rho$h$\sim$ 15.5g/cm2) plate above the telescope to convert neutral primary cosmic ray Erzions to negative one for their registration. There are presented and analyzed received results.

The author has performed an analysis of long-term variations of cosmic rays variation in connection with the planets motion, All neutron monitors selected for the study (Moscow, Apatyti, Irkutsk, Novosibirsk, Oulu, Jungfraujoch, Lomnicky Stit, Sanae, Calgary, McMurdo, Thule).show the same picture: the cosmic rays intensity changes depending on the planets position on their orbits. At the same time the obtained results reveal clearly that the process of modulation is controlled differently by planets with direct and retrograde rotation. At the moment when the planet with direct rotation passes its aphelion the intensity of cosmic rays as a rule is below normal and the occurrence of Forbush decrease events is increasing. At their perihelion the cold celestial bodies of this type produce an opposite effect. Venus and especially Uranus unlike the planets with direct rotation, are increasing the the intensity of cosmic rays at their aphelion points. A sharp contrast between action of the planets with direct and retrograde rotation action simulates the situation of the thought critical experiment in which we are able to find the only explanation of the observed effect, namely slowing down and speeding up of the Sun as consequences derived from the contact of its invisible envelop with similar envelops belonging to the planets. These outer parts of the celestial bodies consist of superlight gas newtonium – – transhydrogen chemical element predicted by D.I.Mendeleev along with other six elements which were discovered earlier. Described findings create a base for prediction of cosmic rays anomalies both in the near and distant future.

Although Cold Nuclear Transmutation (CNT) is rather reliable phenomenon, but there are few theoretic models for its explanation. Erzion model of the catalytic nuclear transmutation (EM) was one of the first such models which could in detail interpret this phenomenon. So in the report it is described the shot history of Erzion (new massive stable hadron) hypothesis appearance in Cosmic Rays in 1982 and Erzion Model development to explain the main features of Cold Nuclear Transmutation Experiments. Erzion Model can give principle explanation for many problems in Cosmic Ray, Astrophysics and Geophysics. In framework of EM Erzion is object of Dark Matter. Moreover, some applied problems can be decided in framework of Erzion Model, such as: 1) to create the new energy-capacious, ecology-pure with rather simple technology nuclear energetics; 2) principle and radical utilization of radioactive wastes; 3) cheap production of some chemical elements and isotopes (gold for example). Erzion Model can explain many experiments in Cold Fusion and can predict many new experiments for its testing.

A measurement of the CP-violating weak phase phi_s and the B0s meson decay width difference with Bs->JpsiPhi decays in the ATLAS experiment is presented. It is based on integrated luminosity of 14.3 fb-1 collected by the ATLAS detector from 8 TeV pp collisions at the LHC. The measured values are statistically combined with those from 4.9 fb-1 of 7 TeV collisions data, yielding an overall Run-1 ATLAS result.

For search in space beams of Erzion the Doch-4A telescope was used. Are presented in the report and new results are discussed: correlation dependence of amplitudes of scintillation detectors for the midday events which are selected with the 10th multiply increased specific ionization and their daily intensity in comparison with daily intensity of a stream of solar protons in solar flashes for the same period (11.09-26.11).14. The carried-out analysis gave their good coincidence and, thereby, indicated on solar origin of registed Erzions.

In this poster a search for a high-mass Higgs boson in the H-->WW-->lvlv decay channel is presented. The search is using pp collision data corresponding to an integrated luminosity of 13.2 fb-1 collected at a centre-of-mass energy of 13 TeV by the ATLAS detector at the Large Hadron Collider. No evidence of a high-mass Higgs boson is found. Upper limits on HxBR(H-->WW) as a function of the Higgs boson mass and width are obtained in the mass range between 300 GeV and 3 TeV.

Run2 sensitivity to quartic anomalous gauge couplings was estimated for ATLAS experiment at LHC with increased energy of proton-proton collisions $\sqrt{s} = 13$ TeV and expected 40 fb$^{-1}$ (2016) and 100 fb$^{-1}$ (2016-2017) of integral luminosity. Simulation of $Z\gamma\gamma$ process with anomalous $ZZ\gamma\gamma$ and $Z\gamma\gamma\gamma$ couplings was performed using VBFNLO MC generator. Differential distributions on four body invariant mass of final state particles was used for extraction of expected limits on Effective Field Theory parameters $f_{T0}/\Lambda^{4}, f_{T5}/\Lambda^{4}, f_{T9}/\Lambda^{4}, f_{M2}/\Lambda^{4}, f_{M3}/\Lambda^{4}$. Combined limits are obtained from two charged leptonic decay channels of Z boson ($Z\gamma\gamma\rightarrow l^{+}l^{−}\gamma\gamma$, where $l = e$ or $\mu$). Unitarity of expected limits was studied using dipole form factor.

For search in space beams of Erzion the Doch-4A telescope within 150 days of its operation was used (15.07.14 - 05.03.15). As optimum substance - the converter of neutral Erzion (E0) of primary space radiation into charged (E0 → E-) for the purpose of their registration the dehydrated calcinated soda was chosen (Na2CO3, ρh~50 g/cm2). In the report new results are presented and discussed: correlation dependence of scintillation detectors amplitudes, abnormal daily distributions of the events which are selected with the 10th multiply increased specific ionization (10m) and their daily intensity. The best data on daily distribution of events for the thick homogeneous converter from the dried-up Na2CO3 soda at its 30-day summer exposition are obtained new and even more. They testify about considerable (~ 50%, 4,8σ) a share of events with the Erzion nature (in morning period from E0 and in evening period from E-) for high ionization (10m) components of cosmic ray. It occurs only for the summer period of a solstice when the high-standing Sun on the heavenly sphere gets to a telescope aperture for registration neutral Erzion (E0). Charged Erzion (E-) from the Sun under the influence of a deviation with a magnetic field of Earth can come in the evening to Earth surface in near vertical direction during any season of year with different efficiency.

The COHERENT experiment goal are to detect and to study neutrino coherent scattering of elastic neutrino-nucleus scattering (CE$\nu$NS). This process is predicted by Standard Model but it has never been observed experimentally because of very low energy of recoil nucleus. COHERENT is using different detector technologies: germanium detectors, CsI[Na] and NaI scintillators and single-phase liquid Ar calorimeter. A description of liquid Ar detector, named CENNS-10, its current status and future plans will be presented.

The detectors based on liquid xenon have high radiation resistance. They are promising detectors for operation in the conditions of intense radiation. The recovery time of the spectrometric mode of the liquid xenon detector after intensive irradiation was investigated. We presented the results of the calculation of xenon activation by thermal neutrons and gamma rays. The operation of the liquid xenon spectrometer in the intervals between pulses of the radiation was studied. The possibility of using the liquid xenon spectrometer for activation analysis for the short-lived nuclides was shown.

Thermodynamic uncertainty relation (UR) was verified experimentally. The experiments have shown the validity of the quantum analogue of the zeroth law of stochastic thermodynamics in the form of the saturated Schrödinger UR. We have also proposed a new type of UR for the relativistic mechanics. These relations allow us to consider macroscopic phenomena in the within the limits of the ratio of the uncertainty relations for different physical quantities

Most of the modern calculations of galactic cosmic-ray (GCR) propagation are based on the local diffusion model acceptable for the Brownian motion (BM) of a heavy particle through the system of uniformly distributed uncorrelated (i.e. non-interacting) molecules. However, about 60 years ago it has been found that the BM model is unable to adequately describe the diffusion in turbulent media [1-3]. Without doubt, interstellar medium belongs to this class. For this reason, the nonlocal transport theory based on fractional calculus is developed in [4]. The series of calculations performed to 2010 confirmed the effectiveness of the approach, improved parameters and led eventually to involving the relativistic speed limit [5]. The obtained model was described in [5,6] and called NoRD in [7]. In this work, the key parameters of the NoRD model are obtained by specifying the Kolmogorov spectra of turbulence near the inertial interval edges. This specification leads to tempered power law distributions of free path lengths. The fractional differential operators are modified into their tempered generalizations. We coordinate energy dependent diffusion coefficient and truncation factor. For energies small enough for interested temporal and spatial scales, diffusion is normal. Extrapolating this dependence on large energies, we observe superdiffusive motion and tendency to ballistic motion. NoRD propagators are calculated and analyzed. Under basic assumptions about the GCR origin, the relativistic principle of maximum speed of propagation leads to the steepening of the equilibrium spectrum at energies close to the observed `knee'. In frames of the NoRD-model, we estimate the role of the local sources and the mass composition at PeV-energies. 1. Monin A.S., Yaglom A.M. Statistical fluid mechanics, Vol.II: mechanics of turbulence, 1965. 2. Heisenberg W. Proc Roy. Soc, A195 (1948) 402. (1948). 3. Tchen C. M. Physical Review 93 (1954) 4. 4. Lagutin A.A., Nikulin Y.A., Uchaikin V.V. Nuclear Physics B-Proceedings Supplements 97 (2001) 267. 5. Uchaikin V. V. JETP letters 91 (2010) 105. 6. Uchaikin V.V. Physics-Uspekhi 56 (2013) 1074. 7. Uchaikin V. V., Sibatov R. T. IJARSET 11 (2015) 1081.

The spectra of relativistic proton were obtained from measurements with the worldwide network of neutron monitors. The relativistic protons appeared after the flares occurring in the west side of the Sun disk arrive to the Earth after time of flight $\sim$15 min without collisions. This prompt anisotropic flux must bring information about spectrum of protons ejected from the solar cosmic ray source. The spectrum of prompt component of relativistic protons is exponential $\sim e^{-E/E_{0}}$, where typical $E_{0}$ is order of 0.5 GeV. After delay of 15 - 20 min the proton flux becomes isotropic with power spectrum $E^{-\gamma}$ where $\gamma \sim 5$. Apparently, beam instability is developed. The proton acceleration in the flare is numerically simulated. The MHD simulation of current sheet creation before the flare is carried out. Initial and boundary conditions have been set using photospheric magnetic field measurements. No assumption about solar flare mechanism is used. Appearance of a current sheet in the solar corona above the active region is proved by comparison of the current sheet position obtained by MHD simulations and the position of observed flare thermal X-ray source. During a flare the magnetic field energy is transferred into the particle energy. The positions of current sheets obtained by MHD simulation above the active region NOAA 10365 are coincided with the positions of soft X-ray emission sources for flares M1.4 May 27, 2003 in 02:53 and X1.2 May 29, 2003 in 00:51. Proton acceleration up to relativistic energy can occur in the electric field applied along the singular line in a current sheet. The electric field E = $-V \times B/c$ is created due to the rate reconnection V. At typical V = $2 \times 10^7$ cm/s the measured spectrum coincides with the calculated spectrum.

In modern experimental physics a heterogeneous coordinate-sensitive calorimeters are widely used due to their good characteristics and possibilities to obtain a three-dimensional information of particles interactions. Espesially it is important at high-energies when electromagnetic or hadronic showers are arise. We propose a quit efficient method to identify antiprotons (positrons) with energies more than 10 GeV on electron (proton) background by calorimeter of such kind. We construct the AdaBoost classifier to separate particles into two classes, different combinations of energy release along reconstructed particle trajectorywere used as feature vector. We test a preliminary verson of the method on a calorimeter of the PAMELA magnetic spectrometer. For high-energy particles we got a good quality of classification: it lost only $4*10^{-4}$ of antiprotons, while less than $10^{-3}$ of electrons were classified to antiproton class.

We study the process of splitting a photon in a strong magnetic field with taking account of the positronium influence on the photon dispersion. The positronium contribution into the photon polarization oprator leads to an essential modification of the photon dispersion law, and of the photon decay amplitude. It has been shown that the probability of the photon decay changes under an influence of the positronium on the photon dispersion.

The possibility of the contribution from standard neutrino processes to the total secondary positron and antiproton fluxes detected by contemporary experiments is analyzed in details. The results show that the considered impact is negligible that confirms once more a necessity of application a new physics beyond the standard conceptions. The designed technique could be implied to the further studies that is extremely interesting in the light of the results of the recent experiments in high energy cosmic ray physics such as PAMELA and AMS-02.

The mass composition of cosmic rays in the hundreds of TeV energy range is purely measured and uncertain, because primary cosmic rays measurements on satellites requires a large area of detectors, but energy is too low for application of methods developed for EAS measurements. In this paper we consider a possibility to use the hybrid method originally aimed to gamma hadron separation in TAIGA experimrnt, to distinguish the diffrent mass groups among cosmic rays in the energy range 100 TeV- 500 TeV. The international gamma-observatory TAIGA (Tunka Advanced Instrument for cosmic rays and Gamma-Astronomy) is intended for ultra high energy gamma-ray astronomy (>30 TeV). It aims at combining the cost-effective timing-array technique with IACTs, allowing to reach a total area up to a few square kilometers and strong suppressing hadron background because of a very precise angular resolution (order of 0.1 degrees at the energy >100 TeV). Hybrid operation of both of these techniques can lead to a relatively cheap way of development of a large area array. We analyze Hillas’s parameters of images produced by different nuclei in IACT together with known arrival direction and shower core position, measured by Hiscore timing arrays. We show that hybrid method can be very effective for this task.

Studying diffuse gamma-ray emission with energies higher than 100 TeV has become especially topical due to detection of astrophysical neutrinos in the IceCube experiment. If these neutrinos are a result of decays of charged pions, neutral pions of the same energy should exist, and their decays must generate considerable flux of gamma rays with energies above 0.1 PeV. In order to confirm these expectations, one should carry out new high-precision experiments in this energy range. An experiment for measuring the flux of gamma rays with energy above 100 TeV is currently being prepared at the Baksan Neutrino Observatory (the Carpet-3 experiment). Step-by-step increase of area of the muon detector of the Carpet air shower array is planned in this experiment. We present some results of calculations of selection efficiency of air showers from primary gamma rays for different configurations of the array. It is demonstrated that by increasing the muon detector area up to 615 m^2 (the maximum possible value) one can reach with the Carpet-3 the world-best sensitivity to 100 TeV gamma rays.

This is a review of a technology of two-phase emission detectors using liquid noble gases as working media. This kind of detectors invented at MEPhI almost 50 years ago is extremely sensitive to ionization (down to single electrons) and can be very massive (in ton scale) in order to provide high count rate for quite rare events and organize an active shielding from natural radioactivity in a wall-les configuration of readout system. The emission detectors found their unique application in the most sensitive at the moment experiments searching for cold dark matter in the form of weakly interacting massive particles (WIMPs). The last results of this search are reviewed in this paper. The current best limits for the spin-independent interaction of supersymmetric WIMPs having a mass in the range between 5 and 1000 GeV/c2 with nucleons were measured with PANDAX-II detector containing 500 kg of liquid xenon. Emission detectors of the next generation G2, such as LZ with an active detector mass of 7 tons, will either unambiguously detect WIMPs or rule out all current theoretical predictions for WIMP existence. Detectors of the G3 generation of up to 20 ton will be used for multiple purposes including detection of double beta neutrinoless decay and low-energy neutrinos using effect of elastic coherent scattering off nuclei. This process is allowed in the Standard Model and was predicted almost 50 years ago, but so far has not been observed. This process plays an important role in the formation of the Universe and the evolution of stars and can be a sensitive probe of New Physics beyond the Standard Model. Experimental observation of the effect is very difficult because of the extremely low energy deposition in a massive detector medium. The review includes a description of the RED-100 two-phase liquid xenon emission detector especially constructed to detect the elastic coherent neutrino scattering off xenon nuclei when the detector is installed practically on the Earth's surface.

The COHERENT experiment goals are to detect and study elastic neutrino-nucleus scattering (CE$\nu$NS). This process is predicted by Standard Model but it has never been observed experimentally because of very low energy of recoil nucleus. COHERENT is using different detector technologies: germanium detector, CsI[Na] and NaI scintillator crystals and single phase liquid Ar detector. All the detector setups placement is a basement of the Spallation Neutron Source (SNS) at Oak Ridge National Laboratory (ORNL). A description of the COHERENT experiment program and technologies used will be presented.

The COHERENT collaboration aims to observe coherent elastic neutrino nuclear scattering (CEvNS) using Ge, Ar, NaI and CsI detectors. The latter has completed the first year of operation at the Spallation Neutron Source located at the Oak Ridge National Laboratory. A description of the CsI detector setup will be presented as well as the current detector performance, related backgrounds and data analysis.

The experimental observation of coherent elastic neutrino-nucleus scattering is one of the most important physical tasks nowadays. The RED collaboration has built a LXe detector “RED-100” for this purpose. An LAr-detector “CENNS-10” is now under construction by COHERENT collaboration. The “RED-100” can be used with LAr filling after several modifications. The use of different working media allows one to determine parameters of the scattering process more precisely since this effect depends on number of nucleons in nuclei. These both detectors use PMTs as photodetectors. To collect the argon VUV light (128nm) with PMTs wavelength shifters (WLS) must be used. The R&D with different types of WLS (including new type of WLS, called NOL – nanostructured organic luminofor) is in progress using ITEP test chamber and Monochromator McPherson 234 in Indiana University.

The analysis of experimental data of the two-phase xenon emission detector has been conducted. There were determined ranges of parameters for neutrons and gamma events, using a two-dimensional diagram in isolines. The original method for estimating the deexcitation time of liquid xenon as a working environment of the detector was applied.

A very efficient purification technology of liquid xenon using a high-voltage discharge between titanium electrodes is described. Lifetime of quasi-free electrons in liquid xenon has been increased from less than 0.1 μs up to more than 50 μs at electric field strength from ~50 to ~500 V/cm. It was shown that this technology allows to remove even complicated molecular impurities from significant amount of liquid xenon what is quite difficult using standard getters. Purified with this method xenon is planned for the use in the RED-100 detector for observation of the elastic coherent scattering electron antineutrino off xenon nuclei.

The RED-100 two-phase xenon emission detector utilizes Hamamatsu R11410-20 PMTs to detect VUV luminescent photons. It was observed, that the background PMT illumination with the luminescent light from cosmogenic muons leads to signal generation at the PMT anode even when the photocathodes are blocked with the help of a dedicated controllable PMT base. We attribute this fact to the photoelectric effect occurring at the PMT first dynode. Results of quantitative measurements of its influence on the RED-100 photodetection system performance are presented here, including the estimation of the first dynode’s quantum efficiency, which is measured to be ≥9%.

A computer model of operation of Hamamatsu R11410-20 photomultiplier based on SPICE software package has been developed. The PMT amplification process is simulated with the use of voltage and current controlled sources of current. Boundaries of linear zone were obtained for high anode current (with respect to the base current) operation regime. The results of simulation are in a reasonable agreement with the experimentally measured characteristics of the PMT with serial # KB0278. The model can be used for simulation of any type of PMT.

The past successes and future plans for the NEST semi-empirical simulation model will be discussed. This work was instrumental in forging the field-dependent signal and background models for use in the LUX results, while also serving as a robust foundation for determining the expected performance of LZ in its technical design report. Lastly, progress on Generation-3 R&D on using superheated xenon at the University at Albany will be highlighted with data from a 100-gram-scale prototype (BubXe) focused on also improving existing G2 LZ.

The decorrelation in the azimuthal angle between the most forward and the most backward jets (Mueller-Navelet jets) is measured in data collected in $pp$ collisions with the CMS detector at the LHC at $\sqrt{s} = 7 TeV$. The measurement is presented in the form of distributions of azimuthal-angle differences, $\Delta\phi$, between the Mueller--Navelet jets, the average cosines of $(\pi-\Delta\phi)$, $2(\pi-\Delta\phi)$, and $3(\pi-\Delta\phi)$, and ratios of these cosines. The jets are required to have transverse momenta, $p_{T}$, in excess of $35 GeV$ and rapidities, $\vert y \vert$, of less than 4.7. The results are presented as a function of the rapidity separation, $\Delta{y}$, between the Mueller-Navelet jets, reaching $\Delta{y}$ up to 9.4 for the first time. The results are compared to predictions of various Monte Carlo event generators and to analytical predictions based on the DGLAP and BFKL parton evolution schemes.

The new SPASCHARM experiment for systematic studies of polarization phenomena in strong interactions is under construction now at IHEP, Protvino. The technical beam runs for the experiment first stage are planned for the Fall 2016 and Spring 2017. At this stage, the polarization measurements will be carried out with unpolarized hadronic beams of various compositions ($\pi^{\pm}$, $K^{\pm}$, $p$, antiprotons), using the polarized target. The universal large acceptance experimental set-up is capable detecting and identification most charged and neutral particles and reconstructing a large number of resonances produced in beam interactions at polarized proton target, and later on at the second stage, in collisions of polarized proton and antiproton beams with fixed targets of various materials. The large acceptance and wide data acquisition bandwidth would provide the capabilities for simultaneous data accumulation for a number of physics analyses from the measurements of single-spin asymmetries in inclusive and exclusive reactions to reconstructions of final state hyperon polarizations and spin density matrix elements for vector mesons in a wide range of kinematic variables ($p_T, x_F$).

Evidence of the $K^+\to\mu^+\nu\bar\nu\nu$ decay was searched for using E949 (Brookhaven National Laboratory, USA) experimental data with an exposure of $1.70\times 10^{12}$ stopped kaons. The data sample is dominated by the background process $K^+\to\mu^+\nu_\mu\gamma$. An upper limit on the decay rate $\Gamma(K^+\to\mu^+\nu\bar\nu\nu) < 2.4\times 10^{−6}\Gamma(K^+\to$ all) at 90% confidence level was set assuming the standard model muon spectrum. The data are presented in such a way as to allow calculation of rates for any assumed $\mu^+$ spectrum.

The talk will cover a present status of the spectroscopy of excited charmed baryons: their masses, natural widths, decay modes and presumably assigned quantum numbers.

Measurements of the cross sections of the production of multiple electroweak gauge bosons constitute stringent tests of the electroweak sector of the Standard Model and provide a model-independent means to search for new physics at the TeV scale. We present recent measurements of the inclusive and differential cross sections for WW, WZ, Z+photon, WWW, Z+2photons, exclusive WW and electroweak production of single W or Z bosons at pp collision energies of 8 TeV and 13 TeV. Distributions sensitive to anomalous triple or quartic gauge couplings have been studied and limits on new physics have been derived.

The LHC is sensitive to dark matter production if additional particles are produced in the process e.g. in initial state radiation. This results in events where the produced object is accompanied by large missing transverse momentum. In this talk the search for dark matter is discussed where a jet, a photon, heavy flavour quarks, gauge bosons or a Higgs boson are produced. If the dark matter is produced via an s-channel resonance the obtained limits can be compared with production rates of dijets. Such interpretations are also presented.

The search for the production of the Higgs Boson with a pair of top-anti-top quarks is both very important and very challenging. The final results from run-1 are presented, with about 20 fb^(-1) of data at 8 TeV, as well as first run-2 results with 13 fb^(-1) of data at 13 TeV.

Using the KEDR detector at the VEPP-4M $e^+ e^-$ collider, we have measured the values of R at twenty points of the center-of-mass energy between 1.84 and 3.72 GeV. At the moment it is the most accurate measurement of R(s) in this energy range.

Fermi-LAT appears to be one of the most successful space telescope missions in history. The Large Area Telescope (LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view, high-energy gamma-ray telescope, covering the energy range from 30 MeV to more than 300 GeV. Since its launch in June of 2008, it collected about 2 Petabytes of data, made a number of spectacular observations, and continues to deliver excellent science. I will talk about main results of the Fermi-LAT mission and its impact on other areas of astrophysics.

V. Pierrard (1, 2) , G. Lopez-Rosson (1) , J. Lemaire (1, 2) (1) BIRA-IASB, Brussels; (2) CSR/UCL, Louvain-La-Neuve Since May 2013, the Electron Proton Telescope (EPT) orbits at 820 km altitude on a polar LEO track (Cyamukungo et al. 2014; Pierrard et al. 2014). The fluxes of trapped electrons ranging from 0.5 MeV to 20 MeV are measured by the EPT in 7 energy channels. We present and discuss here the observations collected during the period of the 17 March 2015 geomagnetic storm (Dst: -231 nT). After the southward turning of the IMF, during the main phase of this large geomagnetic storm, an important dropout was observed at low altitudes in all energy channels of the EPT, for all drift shells of the outer Radiation Belt (L > 4). Penetration of relativistic electrons down to L = 2, into the inner Radiation Belt, was then also observed in the SAA at low altitudes (820 km). This strong injection event filled up the slot region between the inner and outer Radiation Belts, for a period lasting a few days. The (L-t) maps of the fluxes measured indicate that the outer belt electron fluxes finally became significantly larger after the geomagnetic storm than before this event. It was also observed simultaneously by the MAGEIS/VAP-B detector along the highly excentric equatorial orbit of the Van Allen Probes B. Similar post-storm enhancements of energetic electrons fluxes in the outer radiation belt have often been observed and reported earlier, but never simultaneously (i) at low altitudes (along a LEO alike that of EPT/PROBA-V) and (ii) at large radial distances in the equatorial region (along a GTO orbit alike that of MAGEIS/VAP-B). The time variations of the energy spectra, made at both altitudes along the same drift shells, have been compared to each other during the different phases of this geomagnetic storm. We show how Betatron deceleration and the uplift of mirror points (during the storm main phase), and Betatron acceleration and downward motion of mirror points (during the recovery phase) can explain the observed flux variations (i.e. the flux dropouts followed by the flux enhancements). Both at low altitude and at high altitude, these flux variations are due to Betatron deceleration and acceleration (the Dst-effect) induced by the initial built up of the Ring Current intensity, and subsequently by its decay, during the slower recovery phase. We also pointed out how the effects of a concomitant interaction of outer belt electrons with whistler and ULF waves, during main phases and recovery phases can account for observed post-storm flux enhancements (or decreases) of outer belt electron population, often observed after geomagnetic storm events.

It was the 15th of June of 2006 when the PAMELA satellite-borne experiment was launched from the Baikonur cosmodrome in Kazakstan. Since then, PAMELA has been making high-precision measurements of the charged component of the cosmic radiation opening a new era of precision studies in cosmic rays. The measured antiparticle component of the cosmic radiation shows features that can be interpreted in terms of dark matter annihilation or pulsar contribution. The measurements of the energy spectra of protons, electrons, helium and light nuclei and their isotopes challenges our basic vision of the mechanisms of production, acceleration and propagation of cosmic rays in the galaxy. The study of the time dependence of the various components of the cosmic radiations clearly shows solar modulation effects as well as charge sign dependence. PAMELA measurement of the energy spectra during solar energetic particle events fills the existing energy gap between the highest energy particles measured in space and the ground-based domain. Finally, by sampling the particle radiation in different regions of the magnetosphere, PAMELA data provide a detailed study of the Earth magnetosphere. In this talk we will review the PAMELA experiment and its scientific results.

Discussion about sources of energetic particles – solar cosmic rays (SCR) - emerging in the interplanetary space after an explosive energy release on the Sun lasts during more than 20 years. The main candidates for the SCR sources are a Solar flare and a Coronal Mass Ejection (CME). Enormous number of observational data is accumulated since 1942 when the SCR were observed for the first time. Interpretation of experimental results is often ambiguous. This talk gives a very brief overview of the most convincing recent observations that shed some light on the problem.

Sources of gravitational waves in the Universe are considered: relicts from the inflational stage of the early universe; non-spherical collapse in the large-scale structure formation; non-spherical collapse in SN formation, and formation of supermassive black holes in AGN; merging of neutron stars and black holes in close binary systems. Registration of GW of different frequencies is possible in following experiments. Observation of a polarization in the CMB perturbations; observations of the correlated pulsar timing in the group of radio pulsars; timing of the radio pulsars in a close binary with a compact object: NS or BH; observations of the GW signal in the Earth laboratories. The registration of GW signals in the LIGO-VIRGO labs is discussed.

After revise the main features required for an inflationary scenario, we present the Starobinsky model, which is one of the most susscefull inflationary models according to recent observational data. We introduce some new elements on the Starobinsky model, given by an exponential new term, exploring its consequences. The robustness of the Starobinsky inflationary model is analysed.

Recent observations made by imaging Cherenkov telescopes have found a pile-up in the TeV region of some blazar spectra in the optically thick regions (optical depth in this case is the measure of absorption of primary gamma rays on extragalactic background light (EBL) due to the γγ→e+e- process). This pile-up is not consistent with the predictions of the commonly-used models which include only absorption of primary photons and adiabatic losses. We believe that this “anomaly” may be accounted for if certain mechanisms such as electromagnetic (EM) cascade development are taken into consideration. There are three distinct regimes of cascade development depending on the energy of the incident particle. If this energy is high enough, then there are several generations of cascade particles and the observable spectrum is practically independent of the energy and type (electron/photon) of the primary particle but it depends on the distance to the source (the so-called universal regime). If that energy is comparatively low, the number of generations decreases and the spectrum becomes dependent on both energy and type of the primary particle (one-generation regime). The third possible regime is the “extreme Klein-Nishina regime” in which electrons transfer most of their energy to the background photons via inverse Compton scattering process (this regime may take place at ultrahigh energies of primary photons, E>1 EeV). In our work we, for the first time, consider in detail the “one-generation regime”, the universal regime and the transition between them. In this talk we will mainly focus on the so-called hadronic cascade models, in which primary protons create secondary photons by means of pair-production and photopion processes and these photons, in turn, initiate EM cascades. We will compare the results obtained in hadronic and electromagnetic cascade models (in the latter primary particles are photons instead of protons) and provide formal best fits for these models to the widely available data from the HESS and VERITAS experiments (which has never been done before). The sample of observations used in our work includes 6 blazars with hard spectra. In addition to that, to calculate observable spectra for the case of hadronic models, we will introduce a fast and reasonably accurate hybrid method using a large pre-computed database of cascades from primary electrons and photons. We also, for the first time, consider a possibility that the beam of primary protons is affected by an intervening galaxy clusters near the source and on the way from the source to the observer. For the first case, we perform a detailed statistical analysis for the case of blazar 1ES 0229+200 using the emission model of Tavecchio (2013) and show that this model is excluded with significance > 5σ unless the magnetic field strength near the source of protons is much lower than 100 nG. Finally, we show that the intermediate cluster may significantly affect both shape and normalization of the observable spectrum.

The results of simultaneous imaging of the Crab Nebula in the radio (JVLA), optical (HST ACS and WFC3), and X-ray (Chandra) bands are presented. The images show a variety of small-scale emitting structures, including wisps mainly located to the north-west of the pulsar and knots forming a ring-like structure usually associated with the termination shock of the pulsar wind.

Usually two GRBs groups separated in duration distribution: short and long. These types events classified due analysis of duration of interval which the integrated counts from the GRB raise from $5\%$ to $95\%$ ($t_{90}$). The value $t_{90}~\sim~2$s used as boundary between short and long events. Firstly GRB duration distribution was analysed on data of BATSE experiment onboard the (CGRO) Compton Gamma Ray Observatory ($\sim ~2700$ bursts) operated from April 1991 until to June 2000. However in 1999 third burst subgroup (intermediate GRBs) was found due GRBs duration and duration-hardness distributions analysis of 4B current BATSE catalogue (recently available as 5B one) in interval 1~s~$\le t_{90} \le 40$~s. Since CGRO operation finished five satellite experiments GRBs catalogues (Wind, Suzaku, RHESSI, Swift/BAT and Fermi/GBM) contain sufficient amount of bursts for duration distribution precision investigation. The results of these distributions analysis are discussed. It allows concluding the appearance of intermediate GRB subgroup on data of six experiments: BATSE/CGRO, Wind, Suzaku, RHESSI, Swift/BAT and Fermi/GBM.

One of the most interesting properties of astrophysical jets is that they propagates along the axis of rotation of the accretion disk on the distances, which are many times greater than its diameter. Using $Z$-Pinch facilities for laboratory simulation of astrophysical jets seems very logical. The Plasma focus is supposed to be a very suitable device for simulation of astrophysical jets. Results of MHD simulations of jet propagation and its compare with known properties of the laboratory and young stellar object's jets are presented.

Coronal mass ejections (CME) have an impact on the flux of cosmic rays that penetrate the space around us. Unlike most ground-based cosmic ray detectors, muon hodoscope URAGAN (MEPhI) allows to investigate both the integrated counting rate of registered particles and the spatial and angular characteristics of the muon flux at the ground level. This approach to particle detection allows to fix changes in the flux of cosmic rays not only for geoeffective CMEs but also for non-geoeffective ones. The results of the study of different types of CMEs at different stages of the 24 solar cycle are presented.

Muon hodoscope URAGAN operates in MEPhI since 2006 and allows to register muons at various zenith angles. In this work, the experimentally obtained temporal changes of the index of amplitude spectrum of Forbush decreases registered by muon hodoscope URAGAN are studied. To obtain the Forbush decrease amplitude energy spectrum in the flux of muons, the calculated coupling functions of primary and secondary cosmic ray fluxes for five zenith-angular intervals are used. Analysis of the energy characteristics is based on the dependence of the decrease amplitude in the intensity of cosmic ray muons on the mean log energy of primary particles, which influence to the change in the counting rate of the muon hodoscope URAGAN during Forbush decrease. Distributions of values of amplitude spectrum index of Forbush decreases accompanied by magnetic storms at different stages of their development are obtained. It is shown that the energy characteristics of Forbush decreases accompanied by magnetic storms are different for various values of the geomagnetic indices.

Ground Level Enhancement (GLE) is a significant increase of the count rate registered on ground-based neutron monitors (NMs). So far, 72 GLEs have been recorded by the worldwide neutron monitor network since the 1950s. The energy spectrum of solar energetic particles (SEP) for these events varied quite a lot between the events, as measured directly and indirectly. Here we studied a statistical relation between the event-integrated intensity of a GLE (expressed in percent-hours) and the 'hardness' of the solar particle energy spectra, quantified as the ratio of the the integral omnidirectional event-integrated fluences of particles with energy above 30 MeV ($F_{30}$) and above 200 MeV ($F_{200}$). We specifically analyzed the event-integrated energy spectrum for the GLE 71 (17-May-2012), the only directly measured by PAMELA over the entire span. We found no clear relation between the intensity and the spectral hardness for weak and moderate GLE events, but all extreme GLE events were characterized by a very hard spectrum. This implies that a hard spectrum can be securely assumed for all extreme GLE events, e.g., those studied using cosmogenic isotope data in the past.

Magnetic spectrometer PAMELA was launched onboard a satellite Resurs-DK1 into low-Earth polar orbit with altitude 350-600 km to the study cosmic ray antiparticle fluxes in a wide energy range from ~ 100 MeV to hundreds GeV. This paper presents the results of observations of temporal variations of the positron and electron fluxes in the 2006-2015. The ratio of the positron and electron fluxes below 2 GV shows sharp increasing since 2014 due to changing of the polarity of the solar magnetic field.

International space experiment PAMELA was started in 2006 and finished its work in 2016. The main aims of the experiment were the study of the spectra of cosmic rays and of their elemental composition, including the spectra of antiprotons and positrons in a wide energy range. The objective of this work is to develop a methodology for the selection of electrons (including positrons) with energies above 50 GeV and to obtain the summary spectrum of electrons and positrons in a wide energy range 50 – 1200 GeV. In our analyses we have used the data from three detectors - magnetic spectrometer, the calorimeter and neutron detector. We developed the simple method for separation of electrons and positrons from the total flux of charged particles entering the aperture of the spectrometer, and the determination of the energy of these particles. We have got the spectrum of electrons and positrons in the energy range of 50 to 1200 GeV. The geometrical factor of the magnetic spectrometer, the calorimeter and neutron detector is 21 cm2•ster. To extend energy range and increase the statistics at high energies, we developed a methodology of the selection of electrons according only of the calorimeter and neutron detector (in this case the geometric factor is increased more than 20 times). The events when the axis of the cascade passes through the top and bottom planes of the calorimeter were chosen. The preliminary results for this case are presented.

Experimental measurements of the antiproton flux in the near Earth space are important for astrophysics, including the exploration of the hypothetical "dark" matter particle properties. From June 2006 up to January 2016, the scientific experiment PAMELA on board the spacecraft Resurs-DK1 was carrying out the study the various cosmic rays components in the wide energy range. PAMELA spectrometer allows registering low-energy antiprotons (E <1 GeV) by two different detectors independently: the magnetic spectrometer and the coordinate-sensitive electromagnetic calorimeter. This paper presents a method of antiproton’s identification, stopping in the calorimeter. It based on the analysis of the topology of antiproton and a secondary charged meson tracks which arising in the annihilation process. The application of this method will independently confirm the results of the magnetic analysis, and increase of statistics due to a greater geometric factor of calorimeter in comparison with the magnetic spectrometer is expected.

One of main tasks in PAMELA experiment is identification of cosmic ray (CR) antiprotons on different kinds of background. One example of such background at low energies are pi-meson particles which are generated in elements of spectrometer construction by high-energy CR protons. We propose an approach based on machine learning methods, in particular, Support Vector Machines (SVM). We use two different sets of features for classification: track system features (12 measurements of ionization energy losses along particle track) and calorimeter features (different combinations of energy release inside calorimeter along reconstructed particle trajectory). Constructed classifier showed classification accuracy of 96% for antiprotons and 89% for pi-mesons when rigidity $R$ is up to 2 GeV. When $R \in (2, 5]$ classification accuracy for pi-mesons is 15%. For evaluation of classification accuracy we used k-fold cross-validation method with $k=5$.

The sampling imaging electromagnetic calorimeter of $\approx 16.3$ radiation lengths and $\approx 0.6$ nuclear interaction length designed and constructed by the PAMELA collaboration as a part of the large magnetic spectrometer PAMELA. Calorimeter consists of 44 single-sided silicon sensor planes interleaved with 22 plates of tungsten absorber (thickness of each tungsten layer 0.26 cm). Silicon planes are composed of a $3\times3$ matrix of silicon detectors, each segmented into 32 read-out strips with a pitch of 2.4 mm. The orientation of the strips of two consecutive layers is orthogonal and therefore provides two-dimensional spatial information. Due to the high granularity, the development of hadronic showers can be study with a good precision. In this work a Monte Carlo simulations (based on Geant4) performed using different available models, and including detector and physics effects, compared with the experimental data obtained on the near Earth orbit. The response of the PAMELA calorimeter to hadronic showers investigated including shower radius, longitudinal and transverse shower profiles etc.

The PAMELA and the ARINA experiments are carried out on the board of satellite RESURS-DK1 since 2006. The main goal of the PAMELA instrument is measurements of high energy antiparticles in cosmic rays while the ARINA instrument is intended studying high energy charged particle bursts in the magnetosphere. Both of these experiments have a possibility to study trapped particles in the inner radiation belt. The complex of these two instruments covers proton energy range from 30 MeV up to trapping limit (E= ∼2 GeV). Continuous measurements with the PAMELA and the ARINA spectrometers include falling and rising phases of 23/24 solar cycles and the maximum of 24th one. In this report we present temporal profiles of proton flux in the inner zone of the radiation belt (1.11 < L < 1.18, 0.18 < B < 0.22G). Dependence of proton fluxes on a magnitude of the solar activity was studied for various phases of 23/24 solar cycles. It was shown that proton fluxes at the solar minimum are several times greater than at the solar maximum.

The fast multilayer scintillation detector of the new telescope-spectrometer for the ALFA-ELECTRON space experiment is in ground testing mode now. A module data control system for spectrometer is discussed. An algorithm for data treatment is presented. The device will planned to install on the outer surface of the Russian Segment of the International Space Station in 2018.

We find the exact analytical expressions for metric functions of the classical Vaidya metric in the diagonal coordinates in the case of the linear mass function. By using these coordinates, we elaborate the maximum analytic extension of the Vaidya metric with a linear growth of the black hole mass and construct the corresponding Carter-Penrose diagrams for different specific cases. The derived global geometry seemingly is valid also for a more general behavior of the black hole mass in the Vaidya metric.

In the papers reporting about this discovery, the joint LIGO \& VIRGO team presented an upper limit on graviton mass such as $m_g < 1.2 \times 10^{-22} eV$ \cite{Abbott_16,ligo16}. The authors concluded that their observational data do not show violations of classical general relativity because the graviton mass limit is very small. We show that an analysis of bright star trajectories could bound graviton mass with a comparable accuracy with accuracies reached with gravitational wave interferometers and expected with forthcoming pulsar timing observations for gravitational wave detection. This analysis gives an opportunity to treat observations of bright stars near the Galactic Center as a tool for an evaluation specific parameters of the black hole and also to obtain constraints on the fundamental gravity law such as a modifications of Newton gravity law in a weak field approximation. In that way, based on a potential reconstruction at the Galactic Center we give a bounds on a graviton mass.

We present a systematic analysis of homogeneous and isotropic cosmologies in a particular Horndeski model with Galileon shift symmetry, containing also a $\Lambda$-term and a matter. The model, sometimes called Fab Five, admits a rich spectrum of solutions. Some of them describe the standard late time cosmological dynamic dominated by the $\Lambda$-term and matter, while at the early times the universe expands with a constant Hubble rate determined by the value of the scalar kinetic coupling. For other solutions the $\Lambda$-term and matter are screened at all times but there are nevertheless the early and late accelerating phases. The model also admits bounces, as well as peculiar solutions describing ``the emergence of time''. Most of these solutions contain ghosts in the scalar and tensor sectors. However, a careful analysis reveals three different branches of ghost-free solutions, all showing a late time acceleration phase. We analyse the dynamical stability of these solutions and find that all of them are stable in the future, since all their perturbations stay bounded at late times. However, they all turn out to be unstable in the past, as their perturbations grow violently when one approaches the initial spacetime singularity. We therefore conclude that the model has no viable solutions describing the whole of the cosmological history, although it may describe the current acceleration phase. We also check that the flat space solution is ghost-free in the model, but it may acquire ghost in more general versions of the Horndeski theory.

We study hypermagnetic helicity and lepton asymmetry evolution in plasma of the early Universe before the electroweak phase transition (EWPT) accounting for chirality flip processes via inverse Higgs decays and sphaleron transitions which violate the left lepton number and wash out the baryon asymmetry of the Universe (BAU). In the scenario where the right electron asymmetry supports the BAU alone through the conservation law B/3−L_{eR}=const at temperatures T>T_{RL}~ 10TeV the following universe cooling leads to the production of a non-zero left lepton (electrons and neutrinos) asymmetry. This is due to the Higgs decays becoming more faster when entering the equilibrium at T=TRL with the universe expansion, Γ{RL}~T>H~T^2, resulting in the parallel evolution of both the right and the left electron asymmetries at T

In 6D general relativity with a scalar field as a source of gravity, a new type of static wormhole solutions is presented: such wormholes connect our universe with a small 2D extra subspace with a universe where this extra subspace is large. We consider manifolds with the structure M0 x M1 x M2, where M0 is 2D Lorentzian space-time while each of M1 and M2 can be a 2-sphere or a 2-torus. After selecting possible asymptotic behaviors of the metric functions compatible with the field equations, we give explicit examples of wormhole solutions with spherical symmetry in our space-time and toroidal extra dimensions. In one example, with a massless scalar field (it is a special case of a well-known more general solution), the extra dimensions have a large constant size at the "far end"; the other example contains a nonzero scalar field potential which provides a 6D anti-de Sitter asymptotic behavior, where all spatial dimensions are infinite.

We study the properties of an effective potential for the scale factor of extra dimensions in a Kaluza-Klein-type model with a spherical extra factor space, including a function of the scalar curvature and other quadratic curvature invariants, taking into account the Casimir energy of massless scalar fields. We demonstrate the existence of a minimum of the potential, able to induce a physically reasonable value of the effective cosmological constant in our space-time. Under the adopted assumptions, it is shown that the huge Casimir energy density can be compensated by the fine-tuned contribution of the curvature-nonlinear terms in the original action.

Reduction mechanism of a scalar field insertion into a Lagrangian of nonlinear gravity is proposed. Equivalence between nonlinear gravity with two extra space and nonlinear gravity with an extra space plus a scalar field is studied. The scalar field mass depends on properties of a smaller extra space.

Estimates of the collision symmetry planes is a crucial part of the anisotropic flow analysis in heavy-ion collisions. HADES experiment at GSI has different subdetectors which can be used for symmetry plane estimates. In this presentation different methods of the event plane reconstruction and detector non-uniformity correction procedure used in HADES experiment will be discussed.

A new form of nuclear matter, where quarks and gluons are deconfined and interact strongly with each other, is produced in heavy ion collisions at the relativistic heavy ion collider (RHIC). Azimuthal anisotropies of particle distributions relative to the symmetry plane in high energy heavy ion collisions are used to characterize the collision dynamics. The results of measurements of the azimuthal anisotropy paramenters $v_n$ (n=2,3) of identified charged hadrons (pions, kaons and protons) as a function of centrality and transverse momentum in Au+Au collisions at $\sqrt S_{NN}$ = 39, 62.4 and 200 GeV will be presented and discussed. The energy dependence of the difference between the flow of the particles and their anti-particles will be discussed as well.

The spatial and temporal characteristics of particle emission source in high-energy collisions can be measured by using two-particle femtoscopic correlations. These correlations arise due to quantum statistics, Coulomb and strong final state interactions. In this talk, we report on the measurement of like-sign meson femtoscopic correlations produced in p+p, d+Au, Au+Au at top RHIC energy using Quantum Molecular Dynamics Model (UrQMD). Three-dimensional correlation functions are constructed using the Bertsch-Pratt parametrization of the two-particle relative momentum. The correlation functions are studied in several transverse momentum ranges. The emitting source radii of charged pions and kaons, $R_{out}$, $R_{side}$, $R_{long}$, are obtained from Gaussian fit to the correlation functions and compared to data from the STAR experiment.

The size and evolution of the medium created in a heavy-ion collision depends on collision geometry. Experimentally collisions are characterized by the measured particles multiplicities around midrapidity or energy measured in the forward rapidity region, which is sensitive to the spectator fragments. In the CBM experiment the multiplicity of produced particles is measured with the silicon tracking system (STS). The projectile spectator detector (PSD) is sensitive to spectator fragments. We present the procedure of collision centrality determination in CBM and its performance using the PSD and the STS information.

Compressed Baryonic Matter experiment (CBM) at FAIR has a potential of discoveries in the area of QCD phase diagram with high net baryon densities and moderate temperatures. Anisotropic transverse flow is one of the key observables to study the properties of matter created in a heavy-ion collisions. CBM performance for anisotropic flow measurements is studied with Monte-Carlo simulations of gold ions at SIS-100 energies using heavy-ion event generators. Different combinations of the CBM detector subsystems are used to investigate the possible systematic biases in flow measurement and to study effects of detector azimuthal non-uniformity. Resulting performance of the CBM for flow measurements is demonstrated for directed flow as a function of pseudorapidity and transverse momentum in different centrality classes.

We analyze several known models of solar atmosphere to find the most realistic one for understand nuclear interactions with it.

This work is devoted to the fundamental problems of physics, namely the check of the first postulate of the special theory of relativity about inertial frames of reference. The question of transition between inertial systems, which is bound to the need of their acceleration is considered in it. If an inertial frame of reference is bound to a physical body, then its property can be changed under an acceleration and this can influence further on its interaction with other bodies. From the point of view of STR a transition from one inertial system to another is defined by Lorentz transformation laws and the question of how this transition was carried out, is not considered. There is a certain contradiction between actual and ideal inertial frames of reference. The experiment on particle accelerators is offered for the check of the principle of an independence of a transition from one system to another from a way of this transition In this work a possibilities of carrying out the experiment on check of the first postulate of the special theory of relativity about inertial frames of reference are discussed. The factors capable to influence emergence of the possible deviations from the special theory of relativity expanding the idea of it are considered. These factors are the choice of power range of the particles participating in the offered reversible experiment which is reduced to mutual substitution of a shell and a target and also the choice of suitable elements for its carrying out. The nature of acceleration of the studied particles belongs to the factors capable to influence on emergence of deviations too.

The homogeneous subsample characteristics understanding is necessary for the investigation of any astrophysical objects redshift distribution, for example, gamma-ray bursts. The type Ia supernovae considered as a homogeneous subsample because of suggestion that these luminous events might be used as standard candles for cosmological measurements occurs since the earliest studies of supernovae in 1938. The parameters of our Metagalaxy Ω and ? were determine due sample of Ia supernovae from the Supernova Cosmology Project analysis in 1998. Since then more than 4000 supernovae were added. The results of the redshift distribution analysis for supernova from the catalog are presented in this work. The ability to use an analyzed dataset as homogeneous subsample also is discussed.

Calculation of the electronic wavefunctions and energies in the field of a homogeneously charged core of a large radius are reviewed. The Hartree-Fock self-consistent field method is applied for the problem. The model of large core is used for modeling small metal particles. Also the density-functional method is used in conjunction with the Hartree-Fock method. Results are compared with other authors.

The LHCb Hadron Calorimeter (HCAL) is a sampling iron-scintillator calorimeter of ${5.6λ_{I}}$ thickness. It is equipped with an embedded calibration system based on $Cs^{137}$ radioactive source, which is its main calibration tool. HCAL information is used in the LHCb L0 trigger for event selection, therefore it is important to have a precise and reliable calibration system which produces result immediately after the calibration run. This report describes the layout of the LHCb HCAL and its calibration system and details of the calibration procedure. Special emphasis is put on the data analysis procedure and visualization software. The cesium calibration system is regularly used for the HCAL calibration starting from the beginning of the LHCb operation in 2008. The results on the HCAL performance and last calibration run will be discussed.

The possibility of determination of plastic scintillator characteristics for detection nuclei with high ionizing density by numerical modeling was studied in this report. The scintillator detectors have the following main characteristics: light collection, transparency and light yield efficiencies. It was carried out numerically modeling scintillation photon generation and propagation in detector and evaluated the interrelating between signal amplitude from a photomultiplier and energy deposition of particles and nuclei. Using experimental data for the sample detector and comparing them with numerical modeling main characteristics of the selected plastic scintillator was obtained.

The matrices of silicon photomultipliers (SiPM) are promising multi-channel photosensors for scintillation detectors. A method for their use in this capacity depends on the type of detector and current task. Matrix attached directly to the plastic scintillator can be used for the selection of events in different parts of scintillator. We consider also the possibility to use the arrays of SiPM with a corresponding collector optical radiation to obtain a picture of glowing tracks of charged particles, passing through the scintillator. Such method will allow us to get the image of event within the volume of the scintillator, the analysis of which gives the possibility, in principle, to separate different classes of events. The snapshots of the events inside the scintillator were taken for the two SiPM matrices arrangements. In the first variant both matrices are placed on the surface of the plastic scintillator. In the second variant an optical system with Fresnel lens was used. It is expected that the proposed method of detecting particles may be useful in the creation of new large detectors to neutrino astrophysics, and geophysics.

An information about development of an anticoincidence system for charge particle rejection in “Signal” experiment on a board of “Interhelioprobe” spacecraft are presented. A construction of a detector and components of scientific equipment are described. Initial tests of the scintillation detector, silicon photomultipliers and future plans of developing are discussed.

The KEDR experiment is dedicated to a study of c- and b-quarks and the two-photon physics at the $e^+ e^-$ collider VEPP-4M in the Budker Institute of Nuclear Physics. Since 2002 the KEDR detector has been collecting data in the energy range 2E $\simeq 1.8\div4$ GeV. The main collection of data for the study of $\gamma \gamma$ physics is planned in the next few years, after increasing VEPP-4M energy. The detector is equipped with a special system to tag scattered electrons from $\gamma \gamma$ processes. The system detects electrons corresponding to small $Q_i^2$ of virtual photons. It has a high detection efficiency and good invariant $\gamma \gamma$ mass resolution. To analyze the $2\gamma$ data and estimate contribution of two-photon background events in the 1$ \gamma $ data samples, the event generators $e^+e^- \to e^+e^- \mbox{ + }hadrons$, $e^+e^- \to e^+e^- \mbox{ + } \pi^+ \pi^-$, and $e^+e^- \to e^+e^- \mbox{ + }$PS have been developed. The generator of pseudoscalar resonances production $e^+ e^- \to e^+ e^- \mbox{ + }$PS has the option of taking into account radiative corrections in the mode with a single tagging.

It is known that distorted extra space with point-like defect can take place in our Universe. In the space of 4-dimensions this defect will appear as a non-zero energy density, which can interact as classical field with fermions of Standard Model. Because of the mass and the size we will refer to these kind of extra-space defect as the dark matter "particle", though it is not a particle in common sense. But if distributed across the Universe these objects obviously will contribute to the dark matter density.

In the report, self-interacting dark matter is considered. It is supposed that it can form bound states (with possible successive annihilation) due to long-range dark forces. In the course of cosmological evolution, such dark matter may form two components: "passive" one in the form bound-states and "active" (possibly small) one in the form of free dark-charged dark matter particles. Such scenario may have implications for different astrophysical and cosmological issuses.

Orbital experiment ARINA on the board of Russian satellite Resurs-DK1 launched in 2006 developed to study charged particle flux (electrons $E \sim 3 - 30 MeV$, protons $E \sim 30 - 100 MeV$) in near-Earth space, especially high-energy electron precipitation from the inner radiation belt caused by various geophysical and solar-magnetospheric phenomena. Precipitated electrons under certain conditions (energy, LB-coordinate) drifts around the Earth and can be detected as fast increase in count rate of satellite spectrometer (so called bursts). High-energy electron bursts can be caused by local geophysical phenomena (like earthquakes or thunderstorms). Such bursts have distinct features in their measured energy-time distribution. These features contains information about initial location of electron precipitation. In previous works, particle precipitation region searching method is described, the main idea of the method is to use numerical model of electron movement in magnetosphere to find longitudinal distance between region of precipitation and burst registration location on the board of satellite, and with knowledge of L-coordinate define precipitation region borders. Major problem of this type of analysis is the high number of background electrons (atmospheric albedo). Several methods (linear, robust regression) were used previously to minimize number of background particles involved in analysis. In this report, the new committee method was developed, it uses the combining results from several methods in dependence of burst registration conditions. Committee method was tested on simulation and experimental data. Numerical simulation of local particles precipitations based on well-known equations of relativistic particle movement in Earth magnetosphere. In experimental data analysis, the results from ARINA experiment for $10$ years was used. Several results based on burst experimental data are shown. Committee method shows better results than any single method alone.

Decaying or annihilating dark matter model is a common way to explain positron anomaly, although it inevitably contradicts data on cosmic gamma-rays. We are going to show that introducing dark disk may evade this problem.

Simulation of the PAMELA spectrometer characteristics is performed now by Geant4 software package (in the PAMELA collaboration), which needs a detailed information about geometry, materials etc. of scientific equipment. This data is taken from manufactures or obtained from different ground-based tests including accelerators. But the characteristics may change a bit during a launch or a long time of operation on the orbit. We propose a method of in-flight correction of calorimeter characteristics. To calculate them we select relativistic particles passing through the calorimeter without interactions and low-energy particles stopping inside it (Bragg curves or stopping power). We obtain correction values from a comparison of various measurements between experimental data and simulation in assumption that electromagnetic processes are performed in Geant4 with high precision. As a result, characteristics of silicon sensors and tungsten absorber of calorimeter are refined. Correction values are within $\approx5\%$ of the original values.

First results of investigation of PAMELA detectors parameters for search of albedo tritons. PAMELA is an space-born international experiment is housed on board of Resurs DK-1 satellite which was launched on 16 June 2006. PAMELA experimental framework consists from several independent detectors including time-of-flight detector, tracking detector and calorimeter. These detectors allows to search and identify tritons in albedo radiation, but fluxes of tritons are small enough, so big data samples are required for clean identification. Therefore, it is mandatory to check stability of detector parameters during a long period of time. So in this work this analysis was done and it was used for search of deuterons.

A special phenomenon in the physics of cosmic rays, called Forbush decrease (FD), or Forbush effect was discovered in 1937 by S. Forbush. FD is a sudden supression of galactic cosmic rays (GCRs) intensity near the Earth. However, despite long term of investigations the nature of this phenomenon is still not completely understood. Today, this effect is investigated mostly by the neutron monitors and muon hodoscopes, which are located on the surface of the Earth. But these monitors can detect only interaction products of GCRs with the Earth atmosphere. Therefore, investigations of this effect using the detectors which are installed on the sattelites, allow to obtain more accurate information about the characteristics of FD. PAMELA experiment conducted research on board of the satellite for 10 years allowed to investigate the characteristics of the GCRs during FDs which occurred during the experiment. The possibility of investigation of this effect is shown on FDs which were registered in december 2006 and march 2012.

A calibration system based on two light-emitting diodes (LEDs) and finite difference technique is described. Pulses of the both LEDs have a complex shape like CsI(Tl) signals. The first LED has constant amplitude, while the amplitude of the second one varies all over the detector energy range. The differences between detector responses to summarized pulses of the both LEDs and pulses of the variable LED are measured. Then iterative fitting of the measured data is used for calculation of a detector response curve. This approach allowed us to design a calibration system for a scintillation detector with the energy range of 1-200 MeV, which is going to be part of the GRIS solar gamma ray spectrometer. The results of calibration and verification measurements are represented; the precision of the proposed method is discussed.

For measurements of particle fluxes with the PAMELA calorimeter within the wide angular range it is important to estimate some parameters (energy and angular resolution, acceptance, efficiency of particle registration and so on). The GEANT 4 simulation allowed to get values of such parameters. Here we present results of this simulation.

This work is devoted to methodology of solar neutrons search during solar events by using a neutron detector of the PAMELA the magnetic spectrometer on-board RESURS-DK1 satellite. Analysis of counts rates showed that in the geomagnetic equator region the detector performance is nominal and background conditions are stable. Maps of background fluxes were constructed and then 27 solar events were examined in the period from December 2006 to September 2014. In some events, there are evidence of neutrons count rate increasing during solar events. To make conclusion about the nature of these neutrons statistics and monitoring intervals need to be increased, that requires the analysis of background conditions in the Polar Regions

Multilayer diamond detectors of ionizing radiation were developed. Mathematical modeling and experimental research of detector output signal when exposed to beta radiation was made. Found an increase in the signal/noise ratio in the registration of beta radiation as compared to single-layer detectors.

PAMELA experiment on board Resurs DK satellite was equipped with electromagnetic imaging calorimeter, which comprises 44 silicon planes interleaved with 22 plates of tungsten absorber (total debth 16,3X0). High granularity of calorimeter allows an accurate spatial reconstruction of the shower development. New method of separation of electrons and protons based on single strip distribution ouside of main particle track is discussed. Monte-Carlo simulation hows that adding this method proton rejection power of the instrument can be increased several times in energy range from ~10 to ~100 Gev.

We consider a problem of estimation of relationship between scalar fields for a multifield data set. Evaluation techniques using computation of correlation matrix for fields give a global result and therefore are non-informative. As a satisfactory alternative, gradient comparison measure can be used [Nagaraj, 2011]. Another alternative is Jacobi sets, which are the sets of critical points of the restrictions of one function to the intersection of level sets of the other functions [Huettenberger, 2015]. We present the results of a numerical experiment for the case of multifield containing two fields: geopotential height on isobaric level 300 hPa and total ozone column in the Northern hemisphere in January 2005, when intensive solar proton events were observed. Estimation of relationship by gradient measure indicates strengthening interaction between fields at $18^{th}$ and $20^{th}$ of January. However, note that gradient measure value depends on gradient vectors length, so such strengthening may be related with magnitude change of gradient fields. Jacobi sets computation gives more reasonable estimate: relation between fields weakens during solar proton events; paths on Jacobi set between critical points of total ozone field become longer. In this work we also give physical explanations of obtained results.

3D self-consistent model is discussed which may describe the quasi-stable stellar system. Such model describes the system having the shape of oblate rotational ellipsoid. The common case of anisotropic "pressure" in the plane of symmetry is considered. Some aspects of quasi-relaxed states of such systems and possible system evolution are discussed shortly.

Prototype of the fast timing Cherenkov detector has been developed utilizing a modified Planacon XP85012 MCP-PMT for its use in collider experiments. We present the timing and amplitude characteristics of the prototype obtained with relativistic particles and with fast lasers. Also presented will be the reasons and description of the PMT modification, summary of the detector's response on particle hits at oblique angles, light yield of the MCP window, and amplitude homogeneity across the MCP area.

We show possibility of reionization of the Universe at redshifts z = 5-10 due to radiation of primordial black holes. The mass distribution is obtained in the framework of a specific model of their formation as a result of phase transitions in the early Universe. Hawking radiation is assumed to be ionization source.

In the case of charged particle beam propagation in terrestrial magnetic field the beam behavior may be described in the frame of Vlasov theory. The Vlasov theory requirement of the particle collision absence is fulfilled for the cosmic rays due to the high beam energy and rather low beam intensity. In such approach 2D self-consistent time-dependent model may be applied, based on the approximation that the particle ensemble is described by the distribution function dependent on the motion equation invariants. Analytical and numerical solutions of the model equations allow to predict the beam characteristics transformation during the beam propagation in terrestrial magnetic field, in particularly, the beam energy spread transfer into the particle transverse angles (velocities) and vice versa, which may be important for the estimate and the interpretation of the measurement results.

The statistics of reliable solar cycles (SC) leads to the scenario of the regular changes in generation regime of the magnetic field in the solar convection zone from the epoch of ''increased'' ($<$8 – 10 and 18 – 22 SC) to the epoch of "lowered" (12 – 16, 24>) solar activity (SA) and vice versa – from the epoch of ''lowered'' to the epoch of ''increased'' SA. These epochs significantly differ from each other in parameters, evolution characteristics and manifestations of sunspot-forming activity. From the current 24 SC, the Sun entered into second epoch of ''lowered'' SA, which, taking into account the steady nature of a sunspot reliable series, must be prolonged 5 solar cycles ($\sim$55 of years). The consequence of the low values of the background solar magnetic field became the significant drop the value of interplanetary magnetic field, which in turn led to the significant increase (approximately on 20%) the fluxes of galactic cosmic rays in the internal heliosphere in comparison with the epoch of "increased" SA (1944-1996). It is important to note that in the ''lowered'' SA epochs there are not observed high solar cycles and in the ''increased'' SA epochs are forbidden the low solar cycles. In the current 24 SC the picture of solar proton activity principally changed: significantly reduce the amount of solar proton events in the whole energy range, including GLE- events and there were no events with extreme proton flux (104 pfu). This facts shows that in the first half of the 21st century, we will have a high background of galactic cosmic rays, while the fluxes of solar protons and their number will be significantly less. It follows that manned space flights in the free space will become very problematic and probably should be postponed for the second half of the 21st century.

Associated with thunderstorm activity gamma-ray bursts (TGF - Terrestrial Gamma-Flash) were discovered in 1994, by the BATSE instrument on board the satellite (cosmic gamma-ray observatory Compton, NASA). As expected one of the main mechanisms of their generation is bremsstrahlung emission of relativistic electrons, accelerated by atmospheric electric field above thunderclouds. This work is devoted to investigation of the interrelation between TGFs and of high-energy electron bursts, which have been registered into near-Earth space below the radiation belt. The database of high-energy electron bursts with energies from 3 to 30 MeV obtained in ARINA and VSPLESK satellite experiments and the database of TGFs registered by RHESSI satellite (with energies up to 17 MeV) were used in this work. As it was shown earlier the most of electron bursts (70-80%) have the thunderstorm origin. Most of these bursts are associated with precipitations of the electrons from the radiation belts caused by electromagnetic disturbance generated by the lightning discharges. But some bursts could have another origin, for example, associated with acceleration-runaway mechanism (Gurevich’s mechanism). In this case, the electron bursts must be accompanied with flashes of bremsstrahlung. The database of TGFs and the data of the high-energy electron bursts were analyzed. The results of the analysis are presented at this work.

We derived a simple expression for total mass density of electrons and positrons in the region of equation-of-state parameters where electron-positron pairs are dominant by number (as compared with baryons). We estimated the total mass density of electrons and positrons in some models of superluminous supernovae developed by other authors. We found that at least in one model of pulsational pair instability supernova the mass density of electrons and positrons is comparable with the mass density of baryons. This fact can be used to assess the possibility of non-standard gravitational interaction of positrons with electrons and baryons.

We have studied the solar flare of January 20, 2005 by nuclear physics methods. The enreachment of the flare by helium-3 ions was found.

AE Aquarii has been known as one of the most enigmatic magnetic Cataclysmic Variables on various aspects, including large optical flares and flickering large radio flares, TeV gamma-ray emissions and X-ray emission. AE Aquarii is a close binary system composed of a magnetized white dwarf and a Roche-lobe filling K3IV red dwarf. A white dwarf has a very short rotational period about 33.08 s. We have made independence timing analisys of archival AE Aquarii X-ray observation, obtained using orbital observatories «XMM-Newton» and «Chandra» in 2001 and 2005 respectively. We compared our results with published data. Period searching with different numerical methods confirmed the presence of 33-s regular X-ray pulsations. Also we confirmed that pulsations with a period of 16.5 s, visible in optical and UV ranges, absents in the X-ray part of AE Aquarii spectrum. It can means that an X-ray emission comes from the one pole of white dwarf surface.

Unidentified EGRET sources from 3EG catalog have been analyzed. Preliminary data analysis has shown at least 31 of these sources coincide with those in 3FGL Fermi catalogue within 1,2 and 3 sigma error intervals of the coordinates and fluxes. Their properties are discussed in the presented work. Even 3-sigma difference allows supposing sources similarity because of more than 3-sigma distinctions in values of fluxes between identified EGRET sources and their Fermi counterparts. For instance, the coincidence between 3EG J1255-0549 and J1256.1-0547 was reported in Fermi catalogues 1FGL, 2FGL, 3FGL. However, these sources fluxes (in units of 10^-8 photons × cm^-2 × s^-1) in the energy band E > 100 MeV are 179.7±6.7 (3EG), 44.711±0.724 (3FGL), 53.611±0.997 (2FGL) and 67.939±1.861 (1FGL). Such effect observed for sufficient portion of identified EGRET sources. It could cause by troubles of particles identification by Fermi/LAT trigger system. Very often charged particles recognized as gamma-quanta because of wrong backsplash analysis. Nevertheless, gammas counts as charged particles due analogous reason and rejected during ground data processing. For example, it appears as geomagnetic modulation presence on gamma-quanta count rate latitudinal profiles in energy band E>20 MeV.

Analysis of experimental data of primary positrones and antiprotons fluxes obtained by PAMELA spectrometer, recently confirmed by AMS-02 spectrometer, for some reasons shows big interest to the high energies, which are more than 100 GeV. In this work we present a method for identification of high-energy antiprotons on a background of imitating them protons due to finite instumental resolution for high energies (so-called spillover). We base our approach on computing a set of distinctive features represented by differently computed rigidities and training AdaBoost classifier, which shows good classification accuracy of 89% for rigidity up to 1000 GeV.

Investigation of physical phenomena in heavy-ion collisions requires knowledge about collision geometry. It is characterized by the energy distribution in the overlap region of the colliding nuclei. Both the signal from particles produced around mid-rapidity, and the energy of the spectator nucleons can be used to estimate the initial geometry.Due to the pressure gradients during the system evolution, the spatial anisotropy of initial state geometry is converted to an anisotropy in the momentum space, which can be estimated via measured azymuthal distributions.We study the performance of the centrality and the symmetry plane determination for different flow harmonics using the multiplicity around mid-rapidity or the forward nucleon energy measured in various detectors by the ALICE experiment at LHC

A heavy ion collision data (Au+Au) was simulated at MPD (Multi Purpose Detector) at NICA (Dubna) during the study of the possible critical point in the phase diagram of hot nuclear matter. Real detector effects were simulated using realistic simulation of the MPD TPC (Time Projection Chamber), with as many details as possible. Also a new version of particle identification was developed and used for estimating MPD feasibility for this study including TPC and TOF (time of flight) identification.

The Nuclotron-based Ion Collider fAcility (NICA) in Dubna, Russia is currently under construction at the Joint Institute for Nuclear Research (JINR). A Multi Purpose Detector (MPD) at NICA is designed to study properties of baryonic dense matter in the range of center of mass collision energy from 4 to 11 GeV. We present a performance study for anisotropic transverse flow measurement in Au+Au collisions using the UrQMD event generator and Geant4 simulation of the MPD response. The collision symmetry plane is estimated from event-by-event transverse energy distribution in Forward Hadron Calorimeters (FHCal's). Performance of the MPD for a measurement of the directed (v_1) and elliptic (v_2) flow of identified charged hadrons is evaluated based on comparison between reconstructed v_1 and v_2 values and the input one from the UrQMD model.

Heavy-ion collisions provide the unique possibility to create and investigate hot and dense matter in the laboratory. At the initial stage of the reaction a QGP is formed, while the final stage is driven by the hadronization process and the formation of clusters. The capture of the produced hyperons by clusters of nucleons leads to the hypernuclei formation which is a very rare process at strangeness threshold energies. In this respect it is important to have the robust modeling of such processes in order to study the detector replica and to have the possibility to optimize the experimental setup for the best efficiency. We report on the results on the dynamical modeling of cluster formation with the combined PHQMD+FRIGA (Parton-Hadron Quantum Molecular Dynamics + Fragment Recognition In General Application) model at Nuclotron and NICA energies. The clusters selection in FRIGA is realised by a simulated annealing procedure to obtain the most bound configuration of fragments and nucleons. Based on present predictions of the combined model we study the possibility to detect such clusters and hypernuclei in the BM@N and MPD/NICA detectors.

The new model of solar interior structure is discussed. It is consistent with results of years INR RAS measurements of solar neutrino fluxes and with the multi-year observations of 160-minute solar atmosphere oscillations in the Crimean astrophysical observatory. The model is based on two hypotheses: 1. There is a slightly subadiabatic solar troposphere under the superadiabatic convective zone, which is a resonator for 160-minute *g*-mode oscillations. 2. In addition to thermal branch of *pp*-reaction of hydrogen chain, which gives the main contribution into solar luminocity, there is a side nuclear-molecular catalytic brunch of *pp*-reaction, which gives a small contribution into solar luminocity, but controls solar activity and supplies energy to processes of dynamical solar interiors self-organization which are responsible for vigorous solar activity. This new model can justify the necessity of further searches and investigations of non-stationary solar neutrino fluxes.

We solve the inverse problem of parameter determination for the generalized compound diffusion model from the simulation results [Pucci F. et al. Monthly Notices of the Royal Astron. Soc. (2016) 459, 3, 3395] for particle transport in the turbulent magnetic field (TMF). We find the distribution density p(x) of the parallel free path along a regular TMF component and the parameters of the field line wandering (FLW). Density p(x) has the form of a tempered power law function with an exponent close to 0.5 and the truncation parameter, depending on the Larmor radius, turbulence level, intermittency and width of the inertial interval. Parallel motion is associated with a stochastic process of tempered superdiffusion showing the transition from the Levy stable process to Gaussian one. Perpendicular diffusion is determined by the character of FLW, which is modeled by the fractional Brownian motion with Hurst exponent H> 1/2. The resulting random process is a generalization of the compound diffusion model for particle transport in a quasi-regular magnetic field. We use this model to assess the SCR fluxes accelerated in corotating interaction regions of solar wind and to study anomalous diffusion observed in several experiments.

The analysis of GOES spacecraft measurements confirms the data of worldwide network of neutron monitors about solar cosmic ray generation in the solar flares above of an active region with the complex magnetic field distribution. The proton acceleration in a particular flare is beyond doubt. The so-called prompt proton component arrives to the Earth from western flares with a sharp (~5 min) front. The fronts of the proton fluxes from the western flares begin to register with a delay not longer than the time of flight of the particles with their velocity. The protons of the prompt component can propagate without collisions along the magnetic lines of the Archimedes spiral. The proton from the eastern flare cannot reach the Earth moving along magnetic field lines. They can be transferred across the field lines by solar wind and propagate due to diffusion at scatterings with field fluctuations. The front of proton flux from flares that appeared on the eastern part of the disk is gently sloping. Its duration is bigger than 10 hours. The front of such protons arrives with a delay of several hours, which is much less than time of solar wind propagation from the Sun to the Earth. The typical duration of fast proton emissions from the flare that obtained using γ-ray pulses measurements is order of ten minutes, but the tails of proton flux from western and eastern flares (delayed components) last several days. Isotropic velocity distribution and long time duration of proton fluxes demonstrate diffusion particle propagation in the pulse tail of western and eastern flares. The proton scattering with field fluctuation can appear due to proton beam instability at the front, where particle distribution is anisotropic.

Solar modulation of galactic protons and helium with energies from ~50 MeV up to dozens of GeV during July ‘06 - January ‘16 studied based on a data of the magnetic spectrometer PAMELA and scintillation spectrometer ARINA. This period is interesting because it covers the end of 23rd and current 24th cycles of solar activity, including the abnormally long transient period and change of the polarity of solar magnetic field.

First results of cosmic ray deuteron spectra modulation are presented in this work. The data from the international space-born PAMELA experiment was analyzed. Deuterons were selected by multiparameter correlation technique in the energy range from 100 to 600 MeV/nucleon and the differential energy spectra were reconstructed for last solar minimum.

Measurements of the Transition Radiation (TR) yield from polyethylene foils covered with one monolayer of graphene will be presented. Theoretical description of the TR yield in such radiator and interpretation of the experimental results will be given.

The tracking performance parameters of the ATLAS Transition Radiation Tracker (TRT) as part of the ATLAS Inner Detector are described for different data taking conditions in proton-proton, proton-lead and heavy ion collisions at the Large Hadron Collider (LHC). These studies are performed using data collected during the first and the second periods of LHC operation and are compared with Monte Carlo simulations. The performance of the TRT, operating with different gas mixtures (Xenon-based and Argon-based) and for high track multiplicities is presented. These studies show that the tracking performance of the TRT with these two gas mixtures is similar and that the detector still provides a significant contribution to the particle momentum measurement of the overall Inner Detector of the ATLAS experiment up to very high track densities and detector occupancies.

The main aim of the Sphere-Antarctic project is connected to the fundamental problems of the cosmic ray (CR) physics and general astrophysics — the determination of the energy and mass composition of cosmic ray particles of ultra high and extremely high energies $10^{18}-10^{20}$eV. In the energy region above $6\cdot10^{19}$eV modern experiments (Telescope Array and Pierre Auger Observatory) observed anisotropy and the clustering of arrival directions of cosmic rays in some areas. The scientific importance of this problem stems from the lack of generally accepted acceleration mechanism of the CR particles above $3\cdot10^{18}$eV, the unknown nature of the sources of such particles, the inconsistencies of the results of major experiments in the part of the mass of CR composition and the discrepancy of experimental and model data. Scientific novelty f this project is in the methodology registration of the extensive air showers over a large area $\sim$600 km$^2$ from altitude 30 km, that allows to measure the two optical components of the shower Vavilov-Cherenkov radiation and fluorescence light by the same SiPM sensitive elements of the detector simultaneously.

The ICARUS-T600 is the biggest LAr-TPC detector ever realized. The ICARUS Collaboration concluded a very successful, long duration run with the T600 detector at the LNGS underground laboratory, taking data both with the CNGS neutrino beam and with cosmic rays. It performed a sensitive search for anomalous νe appearance as suggested by LSND signal and experimental neutrino anomalies at reactors and with the calibration sources in solar neutrino searches. The analysis of the νμCC events collected with the CNGS beam is progressing, in view of the comparison with the expected flux in absence of anomalies. The collected cosmic ray triggers are being analyzed too aiming at studying the atmospheric neutrino interactions. The detector is being overhauled at CERN and will be ready to be installed at Fermilab by the end of this year to investigate within the SBN project the presence of sterile neutrino, exploring in three years of data taking the νμ to νe appearance signal with 5 sigma sensitivity in the parameter region indicated by the LSND experiment and measuring the νμ disappearance with a sensitivity exceeding an order of magnitude the present experimental limits.

Operating conditions and challenging demands of present and future accelerator experiments result in new requirements on detector systems. There are a lot of ongoing developments and searches for new technologies to improve the properties of existing particle detectors and to develop devices based on some new principles. Several detector prototypes were studied in a test beam at the SPS accelerator at CERN. In this report we show some experimental results obtained with tested Transition Radiation Detector (TRD) prototype. TRD performance depending on transition radiation radiators used and on operation conditions, particularly - gas pressure, are presented and discussed.

The methods for independent measurements of proton and antiproton beam polarizations at the SPASCHARM experiment at U-70 of IHEP, Protvino, are discussed. The fist approach exploits the single-spin polarization asymmetry AN in elastic pp-scattering in the Coulomb-Nuclear Interference and diffraction kinematic regions. The second approach is based on using the earlier observed large AN asymmetry in inclusive charged pion production. The data accumulation times and measurement accuracies are estimated for the both methods and compared.

GlueX is the new experiment in Hall D at Jefferson Lab, which main main goal is to search for mesons with exotic quantum numbers using a beam of linearly polarized photons. The main goal of the pair spectrometer is to determine the photon beam flux and to measure beam polarization. The spectrometer reconstructs the energy of a photon by detecting the electron/positron pair produced by the photon in a thin converter. The pair spectrometer was successfully operated during the commissioning run in spring 2016. We present the design of the pair spectrometer and performance results.

Towards the end of LHC Run1, gas leaks were observed in some parts of the Transition Radiation Tracker (TRT) of ATLAS. Due to these leaks, primary Xenon based gas mixture was replaced with Argon based mixture in various parts. Test-beam studies with a dedicated Transition Radiation Detector (TRD) prototype were carried out in 2015 in order to understand transition radiation performance with mixtures based on Ar and Kr. We present and discuss the results of these test-beam studies with different active gas compositions.

We consider 6D manifolds with the structure M0 x M1 x M2, where M0 is 2D Lorentzian space-time while each of M1 and M2 can be a 2-sphere or a 2-torus.Among such geometries, we find examples of regular solutions of 6D general relativity with a scalar field as a source of gravity, which depend on a single coordinate x ranging over the whole real axis, with different asymptotic behavior at plus and minus infinity. On one end, it is a 4D de Sitter universe times small extra dimensions, while on the other end there is some kind of a static space-time. We thus obtain configurations called black universes, looking as a black hole on the static end and as an expanding universe on the other, and the cosmological expansion begins from a horizon.

The main goal of the AEgIS collaboration is the measurement of the gravitational acceleration of antimatter in the Earth field. The AEgIS experiment is presently taking data at the CERN Antiproton Decelerator (AD) facility. The first step of the measurement is the creation of a beam of anti-hydrogen through the combination of antiprotons and positrons. The beam will be directed toward a moiré deflectometer able to detect the vertical displacement due to the interaction of the neutral anti-atoms with the Earth gravitational field. This measurement would be of great interest as it would probe the Weak Equivalence Principle of General Relativity with antimatter. The experimental apparatus, the measurement strategy and technique and the results obtained so far will be presented.

We study scalar field models with polynomial self-interaction. We write out conditions for the potential which are to be satisfied for kinks with power-law asymptotics to exist. Using the model $\varphi^8$ as an example, we show that power-law asymptotics of kinks lead to their long-range interaction. Within the collective coordinate approximation we estimate the effective kink-antikink potential and force in two cases: for kinks with power-law asymptotics, and for kinks with exponential asymptotics. The numerical results from the collective coordinate approximation are compared to asymptotic estimates of the force of interaction via Manton's method. This long-range interaction can have substantial consequences for phenomenology of physical systems, the dynamics of which is described by field-theoretical models with polynomial potentials. In particular, domain walls in such models would interact at large distances.

A $(n+1)$-dimensional gravitational model with Gauss-Bonnet term and cosmological constant term is considered. When ansatz with diagonal cosmological metrics is adopted, the solutions with exponential dependence of scale factors: $a_i \sim \exp{ ( v^i t) }$, $i =1, \dots, n $, are considered. We study the stability of the solutions with non-static volume factor, i.e. if $K(v) = \sum_{k = 1}^{n} v^k \neq 0$. We prove that under certain restriction $R$ imposed solutions with $K(v) > 0$ are stable while solutions with $K(v) < 0$ are unstable. Certain examples of stable solutions are presented. We show that the solutions with $v^1 = v^2 =v^3 = H > 0$ and zero variation of the effective gravitational constant are stable if the restriction $R$ is obeyed.

The theory of the cosmological inflation successfully describes the accelerated expansion of the universe evolution at early stages. Also, inflation in the early universe has become the standard model for the generation of cosmological perturbations in the universe, the seeds for large-scale structure and temperature anisotropies of the cosmic microwave background. Quantum fluctuations of the inflaton field give rise to an almost scale-invariant power spectrum of cosmological perturbations. String theory is often regarded as the leading candidate for unifying gravity with the other fundamental forces and for a quantum theory of gravity. It is known that the effective supergravity action from superstrings induces correction terms of higher order in the curvature, which may play a significant role in the early universe. The simplest such correction is the Gauss-Bonnet term in the low-energy effective action of the string theory. Such term provides the possibility of avoiding the initial singularity of the Universe. We consider an action with the Gauss-Bonnet term that is coupled to a scalar field \begin{equation} S_{GB}=\int d^{4}x\sqrt{-g}\left[\frac{1}{2}R-\frac{1}{2}(\partial^{\mu}\phi\partial_{\mu}\phi)-V(\phi)-\frac{1}{2}\xi(\phi)R^{2}_{GB}\right], \end{equation} where $\phi$ is an inflaton field with a potential $V(\phi)$, $R$ is the Ricci scalar curvature of the spacetime, $R^{2}_{\rm GB} = R_{\mu\nu\rho\sigma} R^{\mu\nu\rho\sigma} - 4 R_{\mu\nu} R^{\mu\nu} + R^2$ is the Gauss-Bonnet term, and $8\pi G=c=1$. The Gauss-Bonnet coupling $\xi(\phi)$ is required to be a function of a scalar field in order to give nontrivial effects on the background dynamics. The method of exact solutions of the background dynamical equations in a spatially flat Friedmann-Robertson-Walker universe is based on the connection between Hubble parameters for inflation with Gauss-Bonnet term and standard inflation is considereded in this work. On the basis of this connection we calculate the exact values of the parameters of cosmological perturbations at the crossing of the Hubble radius for the inflationary models with Gauss-Bonnet correction. The detection of relic gravitational waves can provide the main information about early universe and can be used to test the theoretical models. In this context, it is important to develop a new methods for the detection of gravitational waves. One of the promising method in the high-frequency part of the spectrum is based on the low-frequency optical resonance phenomenon in the Fabry-Perot interferometers. The description of this method and comparison with another methods are also presented.

In 1930, Reichenbach established the possibility of generalization of Einstein's definition of synchronizing spatially separated a couple of hours, introducing Reichenbach parameter that varies from zero to one, which defines one-way speed of light. A fundamental constant is the average speed of light back and forth. The independence of this observed value of the choice of inertial reference systems supported by the Michelson-Morley experiment.Then John A Winnie in 1970, formulated a generalization of the special theory of relativity to the case of generalized synchronization Reichenbach. Currently, there is discussion about the consistency with the physical experiments of Reichenbach's thesis of the conventionality of simultaneity spatially separated clocks. Without entering into this discussion about the physical reality according to Reichenbach's thesis in this paper, we propose the possibility of using non-standard synchronization in the relativistic -invariant integral formulation of the laws of conservation of charge, the energy - momentum, and other conserved quantities. For two inertial reference systems, the relativity of simultaneity phonological paradigmatic events.Richard Feynman in his Nobel lecture gave an example of the departure of electron-positron pair from the two ends of the rod of finite length. On the basis of the fact of the relativity of simultaneity of these two events, he concluded that the local law of conservation of electric charge for non-point objects. At first, for example, in a textbook of Theoretical Physics Landau-Lifshitz theory of special relativity is formulated in four-dimensional space-time of Minkowski. The equations of the dynamics of the material point is a relativistic generalization of Newton's laws contain as a time parameter interval proportional to the proper time of the moving material point, which does not depend on clock synchronization. By synchronizing the clocks do not depend on the energy, momentum, and other conserved quantities. Consider the insular system of mutually motionless particles. The law of conservation of charge for this system in differential form is expressed as the vanishing of the divergence of a four-vector volumetric current density. To calculate the integral formulation of the integral over the four-volume tube world lines of particles insular system, forming a four-cylinder. This cylinder ends of two perpendicular to the world lines of the surfaces of simultaneous events belonging to the two points in time of the observer in his own frame of reference insular system. The lateral surface of the cylinder tends to spatial infinity, where the charges are zero. In the four-dimensional Gauss theorem the volume integral is converted to the integral over a closed surface, decaying on the lateral surface and two bases. The result is an equality of two integrals over the three-dimensional hypersurfaces for different points in time. This means consistency, i.e the conservation of the total charge insular system. All the above corresponds to the integrated treatment of conservation laws in the course of Landau-Lifshitz. If we move to the laboratory reference system relative to which the insular system is moving inertially, then the hypersurface of simultaneity used in the insular system, cease to be orthogonal to the temporal axis of the laboratory system. Because of the relativity of simultaneity there is an unequal one second parameter Reichenbach, the speed of light is a fundamental constant is only an average. The hypersurfaces of simultaneity in the four-dimensional Minkowski space are invariant geometric objects. In the area of the relativity of simultaneity, you can choose any hypersurface, while the numerical values of the integrals of the remaining quantities do not depend on the choice of hypersurfaces of simultaneity. Thus, if you declare a custom setting for the Reichenbach physically invalid, it returns solemnly to ensure the covariant integral formulation of the conservation laws of physical quantities.

An extension of the Standard Model is considered, which is built on the basis of the Randall-Sundrum model with two branes. The metric of the background solution is not flat, which allows to solve the hierarchy problem of the gravitational interaction. In the case of unstabilized interbrane distance the model predicts the existence of the "strongly" coupled massless scalar mode, the radion, which contradicts the experimental data. In the present work the stabilization of the extra dimension size is achieved with the help of the five-dimensional Higgs field, which plays the role of the Goldberger-Wise filed. The stabilization makes the radion massive, and all the fermion fields, which are assumed to be localized on the TeV brane, get their masses due to the interaction with the boundary value of the Higgs field. The gauge invariance of the theory demands that the electroweak gauge fields also live in the bulk. The equations of motion for the background field configurations are obtained, the second variation Lagrangian for the field fluctuations against a background solution is derived and the equations of motion for them are obtained. The interactions of the bulk Higgs field with the multidimensional gauge and fermion fields are studied and possible values of the model parameters are estimated.

The experimental evidence for BSM physics such as the non-zero neutrino masses, the baryon asymmetry in the Universe, and the presence of non-baryonic dark matter may have their origin in new physics involving very weakly interacting particles as predicted by models with a secluded or hidden sector of particles. In general, these models contain mediators that couple very weakly with SM particles, acting as portals to the hidden sector, e.g. dark photon,Majorananeutrinos,darkscalars,etc... Relativelylightwarmdarkmatterisnaturally accommodated in these models. Given the small coupling constants and typically long lifetimes, hidden particles have not been significantly constrained by previous experiments, and the reach at current experiments is limited by both luminosity and acceptance. This talk will describe the recently proposed SHiP experiment at the SPS which is aiming at generically searching for hidden particles. The high power and unique operational mode of the SPS provide ideal conditions for accessing a wide variety of light long-lived very weakly interacting particles and light dark matter. With 2x1020 protons on target, SHiP is able to achieve sensitivities which are up to four orders of magnitude better than previous constraints, accessing a significant fraction of the unexplored parameter space. Such an experiment would be an essential complement to the LHC in the search for new physics at CERN. The SHiP experiment is also ideally suited to study the interactions of tau neutrinos.

The study of the neutrino oscillation has made important advances in the recent years with the measuremement of the last mixing angle theta13. This has opened up the interesting prospect of probing CP violation effects in the leptonic sector. In this talk I will review the status of the neutrino oscillation studies, with particular emphasis on the most recent results from T2K and NOvA, with first constraints on the CP violation parameter delta_CP. I will also briefly cover the future developments, in particular the T2K-II phase and the next generation long baseline projects Hyper-Kamiokande (Japan) and DUNE (USA), as well as various projects aimed at the determination of the neutrino mass ordering.

Use of ultracold neutrons (UCN) gives unique opportunities of a research of fundamental interactions in physics of elementary particles. Search of the electric dipole moment of a neutron (EDM) aims to test of theories of CP violation. Precision measurement of neutron lifetime is extremely important for cosmology and astrophysics. Considerable progress in these questions can be reached due to supersource of ultracold neutrons on the basis of superfluid helium which is under construction now in PNPI NRC KI. This source will allow to increase density of ultracold neutrons approximately by 100 times in respect to the best UCN source at high flux reactor of Institute Laue-Langevin (Grenoble, France). Now the project and basic elements of a source are prepared, full-scale model of a source is tested, the scientific program is developed. Increase in accuracy of neutron EDM measurements by order of magnitude, down to level 10^-27 - 10^-28 e cm is planned. It is highly important for physics of elementary particles. Accuracy of measurement of neutron lifetime can be increased by order of magnitude also. At last, at achievement of UCN density ~ 10^3 – 10^4 cm^-3, the experiment search for a neutron-antineutron oscillations using UCN will be possible. The present status of the project and its scientific program will be discussed.

The search for neutrinoless double beta decay might be the only window to observe lepton number violation and is therefore considered to be of highest relevance. The isotope 76Ge has historically been most important for this search and the ongoing experiment GERDA has the lowest background and best energy resolution of all experiments in the field. The talk reviews the motivation, the current status of experiments and future programs.

Existing models of hadron-hadron interactions do not give comprehensive description of the result of cosmic ray investigations above 1015eV. Observed phenomena: changes of cosmic ray spectrum and mass composition, “muon puzzle”, various unusual events cannot be explained in frame existing models. The model of quark-gluon blobs allows explain all observed in cosmic rays phenomena and events from single point of view.

A neutron detector providing charged particle detection capability has been designed for pulsed flux measurements. The detector consists of commonly used neutron-sensitive ZnS(Ag)/6LiF scintillator screens wrapping a layer of polystyrene scintillator (BC-454, EJ-254 or similar boron loaded plastic). This type of the detector can be made positionally sensitive and can be constructed in any size. Different variations of the design were considered and modelled. The article presents design features and simulation results.

The paper discusses the method of designing channels based on numerical simulations with the aim of achieving optimal beam parameters at the exit of the channel. Methodology was used to optimize the parameters of the transport channel of the electron accelerator, with significant loss of beam intensity in the output beam from the accelerator and in the process of transport of the beam for the experi-mental equipment.

Pyroelectric crystals, such as LiNbO3 or LiTaO3 being under influence of temperature gradient produce electric field up to 106 kV/cm. It was experimentally confirmed that the crystal installed in the chamber with residual gas pressure about 1 mTorr can be used for generation of X-Rays [1], electrons [2] and neutrons [3]. Due to the unique properties such as On/Off mode of operation and absence of radioactive materials pyroelectric generators seems to be promising tool for calibration of neutrino and dark matter detectors [4,5]. We have developed the laboratory experimental setup for development of pyroelectric neutron generator for calibration of neutrino and dark matter detectors [5]. The setup allows providing and controlling the neutrons generation process realized during d-d nuclear fusion. It is shown that the neutrons with energy 2.45 MeV can be generated starting from a level of electric potential generated by pyroelectric crystal about 30 kV, in contrast to the typical neutron tubes which need the applied outer high voltage level about 100 kV. The results of the neutrons observation and possible construction of the pyroelectric neutron generator are presented. The work was supported by a program of the ministry of education and science of The Russian Federation for higher education establishments, project №14.578.21.0192 (RFMEFI57816X0192).

An experiment on search for neutron–antineutron oscillations is proposed based on the storage of ultracold neutrons (UCNs) in a material trap. The main factors influencing sensitivity of the experiment are the trap size and the amount of UCNs trapped. A high-intensity UCN source will be created at the WWR-M reactor of Petersburg Nuclear Physics Institute, which must provide an UCN density two to three orders of magnitude higher than that in the existing sources. The results of simulations of the experiment for detecting neutron–antineutron oscillations with the new source show that the sensitivity can be increased by ~ 20–80 times compared to existing sensitivity. The range depends on the model of neutron reflection from walls.

For verification of mathematical model the radiation environment sensor a series of experiments was delivered. Researches were conducted by use the radiation beta source Sr90-Y90 . Based on the obtained experimental data comparison with work of mathematical model was carried out them. It is established that experimental values of the transformation coefficients K of charge sensitive amplifier match the calculated values the first four channels within 6%, and also that relative errors of the calculated account speeds of particles counters, rather experimental, don't exceed 10%.

The paper presents the research results of slow neutrons detector based on thin film CVD-diamond with a deep graphitized layer. It is shown the low sensitivity of the detector to the g- and β- radiation. As a converter of slow neutrons used boron isotope 10B and lithium carbonate 6Li2CO3. In both cases, the efficiency of slow neutrons registration was about 3%

Considered a modern implementation of a computer environment for the design of channels of trans-portation of high-energy charged particle beams. The environment includes a software package for the simulation of the dynamics of charged particles in the channel, operating means for changing parame-ters of the channel, the elements channel optimization and processing of the output characteristics of the beam with the graphical output the main output parameters.

The paper presents a new method of identifying signals in a statistically noisy non-stationary time series. In difference from Fourier and wavelet analysis in the processing of data does not make any assumptions about the structure of the signal-analyzer. The proposed method of flicker-noise spectroscopy is demonstrated on simulated and real time series related to monitoring solar activity registration flow of solar and cosmic radiation using ground level muon hodoscope. The method is applicable for analysis of a wide range of different helio - and geophysical processes. This work was supported by RFBR grant 16-05-00997.

The process of neutrino-electron scattering in a dense plasma and magnetic field of arbitrary strength, where electrons can occupy the states corresponding to excited Landau levels, is analyzed. The total probability and the mean values of the neutrino energy volume density and momentum losses due to this process are calculated. Possible astrophysical applications are discussed.

There is description of the development of detectors for neutrons, based on polystyrene and cadmium layers. Cadmium is used as neutron’s converters via reaction (n,γ) and polystyrene is used as scintillation material to register the originated gamma quanta. The simulation and experimental investigations of proposed detectors design are presented. The main advantages of proposed detection is short measurement time- approximately 5 µsec. It is shown that the principle, suggested in the models, can be applied to the detection of neutrons from a pulsed neutron source, for example, secondary neutrons, generated by hadron showers in the space environment or by high-intensity pulsed sources based on accelerators. Detection efficiency for the 24*20 cm2 size detector model, measured during the experiment and simulated by the Monte Carlo technique is about 1% with the measurement time being approximately 5 µsec

We present $\beta$-spectra calculations for two $^{144}$Pr decay branches which are needed to obtain antineutrino spectrum of $^{144}$Ce-$^{144}$Pr source that will be used in SOX experiment. We analyze the factors that affect on beta spectrum, give their calculation methods and compare the calculations with experiment.

The Inner Tracking System (ITS) is the vertex detector that surrounds the interaction point and plays a key role in tracking of charged particles and secondary vertices determination in ALICE (A Large Ion Collider Experiment) experiment at the LHC. After the LHC reconstruction in 2019-2020, when the luminosity of the collider will be increased more than 10 times, new physical tasks of rare processes registration involving heavy flavours, may be solved by the application of fast and high resolution ALICE Pixel Detector (ALPIDE) based on 180 nm CMOS technology. In this work the noise characteristics of the full-scale prototypes of the pALPIDE-1,2,3 detectors have been studied. These detectors were developed within the ALICE ITS upgrade project. It has been determined that for selected parameters of pixel front-end electronics the fake hit rate of the pixels does not exceed the level, required by the general concept of the ALICE ITS upgrade. This work was supported by the Russian Foundation for Basic Research, project no. 15-32-20546.

The long-baseline experiment T2K (Tokai-to-Kamioka) is a world leading setup to study neutrino oscillations and neutrino properties. The experiment uses an intense beam of (anti-) muon neutrinos, which is measured by the near (ND280) and far detectors (Super-Kamiokande). The near detector complex is designed to study neutrino flux prior to oscillations and is an apparatus consisting of several sub-detectors. Plastic scintillator counters with the Hamamatsu MPPC readout are utilized as active elements of the detector sub-modules. The poster will summarize scintillator aging studies based on the data collected by ND280 from 2010.

Registration of supernova neutrinos is one of the main goals of large underground neutrino detectors. We consider the possibility of using the large 2 kT water veto tank of DarkSide-20k dark matter detector as the additional facility for future Supernova detection. Simulations were performed for registration of cherenkov light in water tank from high energy positrons created by supernova electron antineutrinos via inverse beta decay reaction. The expected number of events and their energies for standard galactic Supernova is compatible with the information extracted from the neutrinos from Supernova 1987a. Comparison between characteristics of different supernova neutrino detectors are presented.

A prototype of the calibration system for the Liquid Scintillator Veto (LSV) and Water Cherenkov Veto (WCV) of the DarkSide detector have been developed. The instrument consists of a fast double output flasher which can be configured and controlled via USB, the appropriate application software. UV, visible or combination of both LEDs could be installed. Flashes amplitude, repetition rate and delay time between two continuous pulses are adjustable. High –OH silica fibers are used to minimize intensity losses on the delivery path. X shape splitter is used to combine two LED’s pigtailed output and then to split the sum of the signals. One output feeds calibration path to the detector, while the second is used for pulse-to-pulse measurement of the flash intensity with compatible photodiode in combination with Flash ADC. The instrument allows to simulate point physical events in very wide energy range from a few hundred keV up to several dozen of MeV. Additional studies (pile-up analysis, spatial reconstruction, quenching as a function of position and wavelength) can be performed due to double-LEDs scheme and possibility of fast replacement of diodes. The research was supported by the grant of the Russian Science Foundation (project № 16-12-10369).

The processing of the IceCube experiment data obtained during 988 days (2010–2014) revealed 54 neutrino-induced events with deposited energies 20 TeV - 2 PeV [1]. The hypothesis of an astrophysical origin of these neutrinos is confirmed at $5.7 \sigma$ CL. To identify reliably the neutrino events a thorough calculation of the atmospheric neutrino background should be performed. We calculate the atmospheric neutrino spectra in the energy range of 100 GeV - 10 PeV using the set of the hadronic models and several parametrizations of cosmic ray spectra supported by experimental data. It is shown that rare decays of short-lived neutral kaons contribute close to one third of the atmospheric conventional electron neutrinos at the energies above 100 TeV. The account for kaons production in pion-nucleus collisions gives rise to increase the $\nu_{e}$ flux by 5–7% in the energy range of 100 GeV – 100 TeV. The detailed comparison of our calculations performed with use of $Z(E,h)$ -functions approach [2], with those of MCEq method by A.Fedynitch et al. [3], shows the consistency on the whole at least in the energy range 100 GeV – 1 PeV. Calculated neutrino spectra agree rather well with the measurement data of the experiments IceCube [4,5] and ANTARES [6]. Uncertainties of the measurement data above 400 TeV leave a window for the the QGSM prompt neutrino component [2]. [1] Aartsen M.G. et al. (IceCube Collaboration). Evidence for high-energy extraterrestrial neutrinos at the IceCube detector // Science 2013. V. 342, 1242856; Phys. Rev. Lett. 113, 101101 (2014); arXiv:1510.05223. [2] Sinegovskaya T.S, Morozova A.D., Sinegovsky S.I. High-energy neutrinos fluxes and flavor ratio in the Earth’s atmosphere. Phys. Rev. D. 2015. V. 91, 063011. [3] Fedynitch A. et al. Calculation of conventional and prompt lepton fluxes at very high energy, EPJ Web Conf. 2015. V. 99, 08001; arXiv:1503.00544.; Fedynitch A. et al. MCEQ - numerical code for inclusive lepton flux calculations. PoS (ICRC2015) 1129; http://github.com/afedynitch/MCEq/. [4] Aartsen M.G. et al. (IceCube Collaboration). Development of a general analysis and unfolding scheme and its application to measure the energy spectrum of atmospheric neutrinos with IceCube. Eur. Phys. J. C. 2015. V. 75, 116. [5] Aartsen M.G. et al. (IceCube Collaboration). Measurement of the atmospheric νe spectrum with IceCube. Phys. Rev. D. 2015. V. 91, 122004. [6] Adrian-Martinez S. et al. Measurement of the atmospheric muon neutrino energy spectrum from 100 GeV to 200 TeV with the ANTARES telescope. Eur. Phys. J. C. 2013. V.73, 2606.

URAGAN is a wide-aperture precision muon hodoscope located in Moscow, Russia, 55.7$^\circ$ N, 37.7$^\circ$ E, 173 m a.s.l. It allows to obtain the angular distribution of the muon flux. This distribution may be characterized by a vector of local anisotropy (the sum of the vectors of the particle arrival directions, normalized to the total number of muons). It was shown earlier that annual variations in the vertical projection of the anisotropy vector $A_{\rm Z}$ are observed, and they are not related with changes in atmospheric conditions. It was supposed that the annual variations are caused by changes in the shape of the energy spectrum of primary particles. The dependence of $A_{\rm Z}$ on the index of the primary particles spectrum $\gamma$ was calculated for several zenith angle intervals with the help of simulation of generation and propagation of secondary cosmic ray particles through the atmosphere using the CORSIKA program package. Experimental temporal series of the vertical projection of the local anisotropy $A_{\rm Z}$ for several intervals of zenith angles were obtained for 2007-2015. For $A_{\rm Z}$ estimations, 1 h averaged muon matrices with corrections for barometric and temperature effects were used. According to obtained $A_{\rm Z}$ time series, the average annual daily changes of $\Delta\gamma$ were estimated. Annual and daily changes in the slope of the energy distribution of primary protons are observed. In the range of the mean energy of primary protons 70-110 GeV the annual changes of $\gamma$ are 0.02-0.04, and the daily changes are 0.0025-0.004.

Investigations of cosmic rays on the surface of the Earth allow to derive information of applied character on the conditions of the interplanetary magnetic field and of the geomagnetic field. For this purpose, it is necessary to collate the trajectories of the particles detected in the ground detector to trajectories of primary cosmic rays in the heliosphere. This problem is solved by means of various back-tracking methods. In this work, one of such methods is presented.

Study of the energy characteristics of EAS muon component with an increase the primary particle energy can be a key to solving the "muon puzzle" – the problem of muon excess in EAS observed in several experiments. Such investigations are currently being conducted in the NEVOD-DECOR experiment on detection of inclined muon bundles. Cherenkov water detector NEVOD measures the energy deposit of muons, which is almost linearly related to their energy. Coordinate-tracking detector DECOR measures the number of muons and their direction. The detection of muon bundles of various multiplicities in a wide range of zenith angles allows to explore the interval of primary particles energies from 10^16 to 10^18 eV. In the present work, data of long series of measurements from May 2012 to March 2016 are analyzed. The experimental data are compared with the results of calculations based on simulations of the muon component of EAS by means of the CORSIKA code. d simulations of the EAS muon component. A possible evidence for an increase of the energy deposit at primary energies above 10^17 eV is observed. It has been found that the average specific energy deposit in the Cherenkov calorimeter appreciably increases with zenith angle, thus reflecting the increase of the mean muon energy in the bundles. It is in a reasonable agreement with CORSIKA-based simulations of the EAS muon component. A possible evidence for an increase of the energy deposit at primary energies above 10^17 eV is observed.

The results of the long-term investigations of very high energy extensive air showers with the calibration telescope system (CTS) are presented. The CTS setup is a part of the NEVOD experimental complex. Its top plane is used to register the electron EAS component in the primary particle energy range of 10^14–10^15 eV, while the bottom plane can register muon component in the primary energy range of 10^16–10^18 eV. Two independent methods of reconstruction of the spectrum of the local density of charged particles are considered. The effects of building construction and water pool on the measurement results were calculated using Geant4. The exponents of charged particles local density spectra are obtained for different energy ranges, and the presence of the second “knee” in the spectrum of the muon EAS component is confirmed. The results are compared with CORSIKA calculations and data from other setups.

The description of the NEVOD detector multi-level system of trigger signal formation created for on-line selection of events is presented. The first level forms signals of three types for each quasispherical module (QSM) and provides registration of events with one or several photomultipliers. The second level represents a coincidence circuit of triggers from QSM clusters. This level is based on three V1495 CAEN programmable logic units. Each unit processes its own type of trigger signals. One of the units ensures formation of system-wide signal and its broadcasting to all installations of the complex. The fourth unit produces trigger signals from the top and the bottom planes of the calibration telescopes system. The NEVOD detector triggering conditions and their synchronization with other installations are described. Results of studying of the trigger signal counting rates for different coincidence multiplicities and temporal dependences of the used triggers are given.

In MEPhI, the URAN array for registration of the neutron component of extensive air showers (EAS) is being created. The setup has a cluster structure and includes 6 clusters of 12 detectors each, located on the roofs of the buildings. En-detectors capable of simultaneous registration of two main EAS components are used: electromagnetic (e) and neutron (n). The recording system of the setup consists of twelve boards of amplitude analysis (two boards per cluster), which are synchronized in time with the accuracy of 10 ns. Each board has six dual-12-bit channel ADC with 200 MHz sampling frequency. To register the delayed EAS neutrons the ability to change the sampling frequency in six cards from 200 MHz to 1 MHz is used. Recording time at 1 MHz sampling frequency is 20000 ms. The recording system is integrated by the Central DAQ Post and data transmission from the boards is performed via fiber optic lines.

The more accurate original calculations of the atmospheric vertical energy spectrum at energies $10^{2} - 10^{5} \space $ GeV have been carried out in terms of DPMJET $~2.55 \space $ and VENUS $~4.12 \space $ models. The Gaisser-Honda approximation and results of measurements of energy of primary protons, helium and nitrogen nuclei has been used. The package CORSIKA $~7.4 \space $ has been used to simulate in the standard atmosphere cascades induced by different primary particles with various fixed energies $E_{0} \space $. Statistics of simulated cascades for secondary particles with energies (0.01–1)$ \cdot E_{0} \space $ was increased up to $10^{6} \space $. The results of simulations have been compared with data. This fit showed how the used models have been changed.

The TAIGA Observatory is aimed to provide the study of gamma-rays of high energies (above 100 TeV) and cosmic rays with energies higher than 10 PeV. The main advantage of the observatory is a hybrid method of detection of EAS generated by gamma rayswith an array of wide-angle detectors of Cherenkov radiation of EAS and by the network of IACT. In the report the features of design of the camera of Cherenkov telescope and its detection system designed to work in the condition of hard Siberian winter are discussed.

Charm and beauty production with the future upgraded Inner Tracking System for ALICE at the LHC Grigory Feofilov (for the ALICE Collaboration) The capabilities of detector ALICE detector (A Large Ion Collider Experiment) at the LHC, as expected after the upgrade of the Inner Tracking System (ITS), are reported. The physics motivation of new studies of open charm and beauty measurements of rare processes with charmed and beauty baryons in ALICE, accessible for the first time in heavy-ion collisions at the LHC, are discussed. The relevant requirements to the upgraded ITS and the corresponding design and construction challenges are presented. One of the most unique features is the extremely low material budget of the upgraded ALICE ITS (about 0.3% X/Xo for 3 innermost layers). Charged particles will be reconstructed starting from a pT of 50 MeV/c and charm and beauty mesons will be measured down to zero pT. The currently implemented technical and detector solutions for the upgraded ITS will be also presented. They will provide both the increase of rate of ALICE data taking in Pb–Pb collisions from 1 kHz to 50 kHz and the general improvement of the impact parameter resolution by a factor of 3. Acknowledgements. This work was supported for the SPbSU participants within the Program of Russian groups activities in the ALICE upgrade by the Ministry of Education and Science of Russian Federation, contract No14.610.21.0003, identification number RFMEFI61014X0003 (SPbSU identification number No. 11.19.1632.2014).

As a result of the LHC injectors upgrade after the Long Shutdown (2019-2020), the expected Pb-Pb luminosity and collision rate during the so called Runs 3 and 4 will considerably exceed the design parameters for several of the key ALICE detectors systems including the forward trigger detectors. Fast Interaction Trigger (FIT) will be the primary forward trigger, luminosity, and collision time measurement detector. It will also determine multiplicity, centrality, and reaction plane of heavy ion collisions. FIT is expected to match and even exceed the functionality and performance currently secured by three ALICE sub-detectors: the time zero detector (T0), the VZERO system, and the Forward Multiplicity Detector (FMD). FIT will consist of two arrays of Cherenkov radiators with MCP-PMT sensors and of a single, large-size scintillator ring. Because of the presence of the muon spectrometer, the placement of the FIT arrays will be asymmetric: ~800 mm from the interaction point (IP) on the absorber side and ~3200 mm from IP on the opposite side. The ongoing beam tests and Monte Carlo studies verify the physics performance and refine the geometry of the FIT arrays .The presentation gives a short description of FIT , triggers and readout requirement for the ALICE Upgrade, a summary of the performance, and the outcome of the simulations and beam tests.

We present the design and performance of the Electromagnetic Calorimeter (ECAL) of the Compressed Baryonic Matter (CBM) Experiment at FAIR. The main purpose of the ECAL detector is the identification and the measurement of energy and position of photons and electrons, which are produced in high-energy heavy-ion collisions in the beam energy range from 4 to 40 AGeV. ECAL will measure spectra of photons and neutral mesons decaying in their photonic decay channels. Precise measurement of masses and widths of short-living mesons ($\omega$, $\eta$, $\eta$’, $\phi$, $\chi_c$ etc.) will shed light on the chiral symmetry restoration which is expected to occur in dense nuclear matter. Measurements of the $\pi^0$ and eta meson spectrum are important to study dependence of the particle yield on thermodynamical parameters of nuclear mater.

CBM is the first experiment gaining advantage of free-streaming triggerless readout system. All readout channels of the detector going to work in self triggered mode. Dedicated methods are developed to extract individual events (collisions) from continuous information stream rejecting noise. Efficiency of the methods depends on projectile energy, masses of colliding nucleons, interaction and accelerator frequencies. Quality control of the algorithms and comparison of the methods require special efforts.

The airborne gamma-ray spectrometry data processing technologies for gamma-emitting sources search, localization and identification. V.V.Drovnikov, N.J.Egorov, V.M.Zhivun, A.V.Kadushkin, V.V.Kovalenko National research nuclear university MEPhI The airborne gamma-ray spectrometry data processing methods were developed for gamma-emitting sources search, localization and identification. The experimental data set used is the following: start time, stop time, live time, flight altitude and geographical coordinates for each spectrum measured, corresponding spectrum.No priory information about the characteristics of the gamma-emitting sources and radiation background on survey territory is used.The methods developed make it feasible to calculate: • Spatial distribution of gamma-emitting Nuclide Presence Criterion (NPC) all over the territory surveyed. • Full gamma-spectrum of each radionuclide found for its identification. • Activities, coordinates and corresponding uncertainties for each local source spotted. • Activity spatial distribution of each radionuclide identified all over the territory surveyed. The experimental results are presented. The sensitivity of the methods developed is compared with other data processing methods sensitivities.

New detectors based on thin films of diamond for measurig linear energy transfer were developed. Detectors was tested by rradiation from next isotopes: 90Sr-Y90, 239Pu, 252Cf. It is shown that developed detectors effectively records a heavy charged particles, whereas beta, neutron and gamma radiation does not give a significant contribution to their signals.

The space experiment SONYA is designed to detect cosmic positrons and electrons through their synchrotron x-ray emission in the Earth magnetic field. The proposed instrument can identify the sign and determine the energy of TeV electrons and positrons. Modern magnetic spectrometers aren't able to measure positrons above several hundreds GeV. Simulation of the instrument were performed. Advantages of the method are high proton background rejection and increase of effective area of the instrument with energy. As estimation shows the proposed experiment with size about 1m^2 will detect several tens of TeV positrons per year

Authors: Dmitrii Nikolaev and Marina Chadeeva Presenter: Dmitrii Nikolaev Abstract: The technological prototype of CALICE highly granular analogue hadron calorimeter for future experiments with lepton colliders was tested using electron beams from DESY accelerator facility. The active layers of the prototype are assembled from 3x3x0.3 cm^3 scintillator tiles with silicon photomultiplier readout. The response of individual tiles to minimum ionising particles was measured using a stack of active layers without absorber. We describe the procedure of MIP calibration and present the results obtained during 2016 test beam campaign.

The T2K long-baseline neutrino oscillation experiment in Japan is designed to study neutrino oscillations using a muon (anti-)neutrino beam produced by J-PARC and propagating to Super-Kamiokande detector (located at 295 km across Japan). T2K has conclusively presented results on muon neutrino disappearance and electron neutrino appearance, allowing to perform precise measurement of lepton mixing parameters. Since 2014, the experiment is running in anti-neutrino mode allowing to study anti-neutrino oscillations and has obtained first constraints on CP violation in leptonic sector. We will present the latest results in both appearance and disappearance channels (joint analysis neutrino and anti-neutrino modes), leading to the most up-to-date measurements of $\theta_{23}$, $\Delta m^2_{23}$ and $\delta_{CP}$. The future prospects of T2K will also be discussed.

Magnetized Iron Neutrino Detector (Baby-MIND) is Muon Range Detector (MRD) for WAGASCI experiment in T2K. The Baby-MIND modules are composed of magnetized iron and the long plastic scintillators bars which are read out with wavelength shifting (WLS) fibers. Event reconstruction resides in selecting tracks above the certain threshold in length. Analyzing the vertex allow us to reconstruct the hadronic component of interactions. New frontend board CITIROC was created for readout of Baby-MIND. The bar elements and frontend board were tested with cosmic rays and on with beam at T9 CERN the results are reported.

In connection with the question of possible existence of sterile neutrino the laboratory on the basis of SM-3 reactor (Dimitrovgrad, Russia) was created to search for oscillations of reactor antineutrino. In the middle of 2015 the multisection prototype of a neutrino detector with liquid scintillator volume of 350 l was installed. It can be moved at the distance of 6-11 m from the reactor core inside passive shielding. For the first time the measurement of the reactor antineutrino flux dependence at so short distances from the reactor core center with movable detector was realized. Different methods of cosmic background suppression were studied. After half year collecting statistics the accuracy of measurements of first point at 6.5 m is 10%. The full-scale detector with volume of liquid scintillator 3 m$^{3}$ (5$\times$10 section) is in the stage of preparation. It will allow obtaining the statistic accuracy of measurements at 6-11 m up to 1.5 – 3.0 % after 2 years of measurements.

The experiment on first observation of the elastic coherent scattering of neutrino off atomic nuclei is proposed with the use of the RED-100 emission two-phase xenon detector. This process was theoretically predicted more than 40 years ago by the Standard model of particle physics but has not been observed yet because of lack of the detection technique of the events with the low energy deposition in massive (more than several dozens of kg) targets: the energy of nuclear recoil from the neutrino scattering in detector is in the keV- and sub-keV- energy ranges. This can be done with a technology of particle detection by means of a two-phase emission detector proposed in Russia and well worked out in the experiments on search for dark matter. The RED-100 two-phase emission detector and proposed experiment with it at the Kalinin nuclear power plant (KNPP) are described in this talk. The perspective of the use of such type detectors for neutrino monitoring of nuclear power reactors is considered.

The GERDA (GERmanium Detector Array) is an experiment for the search of neutrinoless double beta decay (0νββ) in Ge-76, located at Laboratori Nazionali del Gran Sasso of INFN (Italy). GERDA operates bare high purity germanium detectors submersed in liquid Argon (LAr). Phase II of data-taking started in Dec 2015 and is currently ongoing. In Phase II 35 kg of germanium detectors enriched in Ge-76 including thirty newly produced Broad Energy Germanium (BEGe) detectors is operating to reach an exposure of 100 kg•yr. The design goal of Phase II is to reduce the background by one order of magnitude to get the sensitivity for T0ν1/2 = O(10^26) yr. To achieve the necessary background reduction, the setup was complemented with LAr veto. Analysis of the background spectrum of Phase II demonstrates consistency with the background models. Furthermore Ra-226 and Th-232 contamination levels consistent with screening results. In the first Phase II data release we found no hint for a 0νββ decay signal and place a limit of this process T0ν1/2(Ge) > 5.2•10^25 yr (90% C.L., sensitivity 4.0•10^25 yr). First results of GERDA Phase II will be presented.

Setup description and the latest results for EXO-200 experiment are presented. Detector is liquid xenon TPC dedicated to study of $^{136}$Xe double beta decay. It contains 175 kg of xenon and is located in underground low-background laboratory. Careful material selection and cleaning procedures along with complicated analysis resulted in one of the the lowest Background Index amoung comparable detectors. Experiment discovered $2\beta2\nu$ decay and made the most precise measurement of half-life of it. Special attention is this talk is given to a dedicated study of activation of detector materials by cosmic ray muons and resulting backgrounds in the detector. This is very important for such a sensitive experiment since it produces unavoidable background.

The review of double beta decay experiments is done. Results of the most sensitive current experiments are discussed. The main attention is paid to KamLAND-Zen, GERDA-II, MAJORANA-DEMONSTRATOR, CUORE-0 and NEMO-3 experiments. Modern values of T1/2 (2v ) and best present limits on neutrinoless double beta decay and double beta decay with Majoron emission are presented. In the second part of the review prospects of search for the neutrinoless double beta decay in new experiments with sensitivity to neutrino mass at the level of ~ (0.01-0.1) eV are discussed. The main attention is paid to experiments of CUORE, GERDA, MAJORANA, nEXO, KamLAND-Zen-2, SuperNEMO and SNO+. Possibilities of low-temperature scintillating bolometers on the basis of inorganic crystals (ZnSe, ZnMoO4 , Li2MoO4 , CaMoO4 and CdWO4) are considered too.

An estimation of the fast neutron flux in an underground laboratory excavated under about 320 m of rock has been performed on a data set acquired during the 2001-2015 years. A neutron background measurement relies on the production of a cosmogenic nuclide $^{12}B$ by fast neutrons in an organic scintillator. The estimated full fluxes of neutrons agree with results of Monte-Carlo simulation.

Recently, it was proposed to use storage rings with $\beta^+$-radioactive nuclei as sources of electron neutrino beams. If the nuclei have large electron capture branching, than such beams could have a significant monochromatic component. Under certain conditions, in particular, for hydrogen-like ions, one can modulate the monochromatic component. We propose the selection criteria for $\beta^+$-decaying nuclei that could be used to produce intense beams of partially monochromatic and modulated electron neutrinos. It is shown that such beams are obtainable on practice and might be interesting for future experiments.

Relativistic Heavy-Ion collisions aim to create the Quark Gluon Plasma (QGP). The QGP is a state of matter with a high enough energy density that hadrons "melt", and quarks and gluons can move over length scales larger than that of a hadron. The Large Hadron Collider at CERN is able to collide heavy-ions at the highest energies achievable within the laboratory. I will review results from the first year of data taking (2010) until now, and discuss what information these results provide about the QGP.

The experiments at RHIC have produced convincing evidence during last decade that strongly interacting partonic matter, Quark Gluon Plasma (QGP) is created in the central collisions of heavy ions. The unique flexibility of RHIC to collide different nuclear species over wide range of collision energies together with STAR's wide acceptance and particle identification are ideally suited for systematic exploration of the properties of this QCD matter. STAR collaboration has successfully completed first phase of Beam Energy Scan, program focused on searching for the onset of the QGP signatures and studying the nature of the phase transition, indicating that the region of interests for critical point and the first-order phase transition is within the reach of RHIC experiments. Moreover, with it's detector upgrades, STAR has launched a comprehensive heavy-flavor program which allows high precision measurements of the properties of the partonic matter. In this talk I will present highlights of that STAR latest heavy-ion results. I will also discuss the results of the first phase of RHIC Beam Energy Scan and present the plan of the future measurements and upgrades.

The Compressed Baryonic Matter (CBM) experiment will be one of the major scientific pillars of the future Facility for Antiproton and Ion Research (FAIR) in Darmstadt. The goal of the CBM research program is to explore the QCD phase diagram in the region of high baryon densities using high-energy nucleus-nucleus collisions. This includes the study of the equation-of-state of nuclear matter at neutron star core densities, and the search for the deconfinement and chiral phase transitions. The CBM detector is designed to measure rare diagnostic probes such as hadrons including multi-strange (anti-) hyperons, lepton pairs, and charmed particles with unprecedented precision and statistics. Most of these particles will be studied for the first time in the FAIR energy range. In order to achieve the required precision, the measurements will be performed at very high reaction rates of 1 to 10 MHz. This requires very fast and radiation-hard detectors, a novel data read-out and analysis concept based on free streaming front-end electronics, and a high-performance computing cluster for online event selection. The physics program and the status of the proposed CBM experiment will be discussed.

According to many theoretical calculations vorticity plays a very important role in the dynamics of the heavy ion collisions. In this talk I am trying to summarize what is known and how we can learn more about vorticity from the experimental side

Numerous phenomena in astrophysics and cosmology ask for new neutral heavy stable particles to form Dark Matter. We review the present status of the problem, its developing solutions and further prospects in hunting for the Dark Matter in particle physics experiments.

The main purpose of the DarkSide project carried out at the Gran Sasso underground laboratory in Italy is direct detection of Dark Matter particles (WIMPs). The Dark Matter search program is based on Time Projection Chambers filled with liquid Argon. The DarkSide-50 TPC, with 50 kg of active mass, is installed inside active neutron and muon detectors. DarkSide-50 has been taking data since 2013 with Atmospheric Argon (AAr) and since April 2015 with Underground Argon (UAr), depleted in 39Ar by a factor of about 1400. The run with AAr has demonstrated the ability of the detector for three years operation in a background free condition. The result obtained with UAr has shown no candidate for Dark Matter events, thus we were able to set the best limit for Spin-Independent elastic nuclear scattering of WIMPs for Argon-based detectors, corresponding to a cross-section of about 2x10−44 cm2 at a WIMP mass of 100 GeV. The detector design, its performance and the physics results will be discussed. The future of the DarkSide experiment will be introduced.

The LUX collaboration has recently released its 332 live-day WIMP search result. LUX remains at the forefront of the search for this dark matter candidate particle, in the 7 $GeV/c^2$ and higher range, with a maximal spin-independent sensitivity of 2.2 x $10^{-46}$ $cm^2$ cross-section for a mass of 50 $GeV/c^2$ now established. Spin-dependent and axion limits will also be discussed, as well as the present status of of LUX’s 10-ton-scale, Generation-2 successor LZ. It plans on achieving a sensitivity of better than 3 x $10^{-48}$ $cm^2$ for a WIMP of 40 $GeV/c^2$ rest mass.

A detector of the reactor antineutrino based on a cubic meter of plastic scintillator is installed below 3.1 GW industrial reactor. The detector is placed on a movable platform which allows to change the distance from the reactor core center in the range 10.7-12.7 m. 2500 scintillator strips are readout individually by SiPMs and in groups of 50 by PMTs. In addition to the overburden by the reactor (~50 m w.e.) the detector has multilayer passive shielding and active muon-veto. Inverse beta-decay count rate of about 5000 events per day in the fiducial volume (78% of the detector) with bout 5% of cosmic background has been reached. DANSS is sensitive to sterile neutrino in the most interesting region of mixing parameter space. The talk will cover the detector status and performance, as well as the first results.

The proposed device combines the advantages of Silicon and Gas-pixel detectors. 7 micron space resolution and down to 0.2 degree both angles measurements are inside 10 mm thick and very low material detector. Binary readout, advanced data collection and preliminary analysis logic allow to obtain all the information in less than 1 microsecond and to use it for the fast trigger generation.

A novel room-temperature ion source for the production of ions with charges from $2^{+}$ up to $80^+$ in electron beam within wide ranges of electron energy $E_e$ (500 eV $\leq E_e \leq 60$ keV) and current density $j_e$ ($10$ A/cm$^2 \leq j_e \leq 20$ kA/cm$^2$) is developed. Due to combination of two methods of sequential ionization of atoms, the device can operate both as conventional Electron Beam Ion Source/Trap (EBIS/T) and novel Main Magnetic Focus Ion Source (MaMFIS). In EBIS/T, ions confined in the potential well are stored in the smooth electron beam going through a few drift tubes with positive potentials applied at the edge sections. In MaMFIS, the local ion traps with extremely high electron current density are formed in crossovers of the rippled electron beam in a thick magnetic lens [1,2]. The device is suitable for generation of both the low- and high-density microplasma in steady state, which can be employed for investigation of a wide range of physical problems in an ordinary university laboratory, in particular, for astrophysics and Tokamak microplasma simulation. For the electron beam characterized by the incident energy $E_e = 10$ keV, the current density $j_e \sim 20$ kA/cm$^2$ and the number density $n_e \sim 2 \cdot 10^{13}$ cm$^{-3}$ were achieved experimentally [1-3]. For $E_e \sim 60$ keV, the value of electron number density $n_e \sim 10^{14}$ cm$^{-3}$ is feasible. The efficiency of MaMFIS for laboratory astrophysics significantly exceeds that of the existing warm EBIT at the National Astronomical Observatory of China and superconducting EBITs at the Lawrence Livermore National Laboratory and the Harvard-Smithsonian Center for Astrophysics. References [1] V. P. Ovsyannikov and A. V. Nefiodov, Nucl. Inst. Meth. B **367**, 1 (2016). [2] V. P. Ovsyannikov and A. V. Nefiodov, Nucl. Inst. Meth. B **370**, 32 (2016). [3] A. Borovik, Jr, J. Dreiling, R. Silwal, E. Takács, J. Gillaspy, R. Lomsadze, V. Ovsyannikov, K. Huber, S. Schippers, A. Müller, and Yu. Ralchenko, 18th Int. Conf. on the Physics of Highly Charged Ions, 2016, Kielce, Poland, Book of Abstracts, p. 44.

The design, layout and parameters of the polarized-beam facility at U-70 proton synchrotron of IHEP, Protvino, are presented. The polarized proton and antiproton beam line 24A is currently under development at IHEP. It will serve as a main playground for carrying out the rich program of the SPASCHARM experiment for comprehensive studies of spin phenomena in a wide variety of hadronic reactions in the beam energy range of ~10-45 GeV.

A beam line of polarized protons and antiprotons, obtained from decays of Λ (anti-Λ)-hyperons for SPASCHARM experiment at U-70 accelerator is under development at IHEP, Protvino. For precise asymmetry measurements one needs to know beam polarization with a relatively low error. Tagging of the beam particle provides a possibility to perform measurements for both polarizations of the beam at the same time to reduce systematic errors and increase statics. Beam tagging station will measure both polarization and beam particle momenta on-line. The correlation between the position of the proton (antiproton) with respect to the channel axis and the value of its polarization is used to measure the relative polarization. The system of detectors with good spatial resolution designed for those measurements as an integral part of the beam line of polarized particles is discussed in the report

This report is based on the results of use the PAVICOM facility in investigations of nuclear and elementary particles tracks. This facility has been constructed in Lebedev Physical Institute and includes three automatic microscopes. They allow to analyse particles tracks in different kinds of material: nuclear photo emulsion, plastic and minerals (olivine). As a result the images of tracks and their geometrical characteristics very differ in various experiments. This circumstance demands use of various image recognition methods depending on properties of images and aims of experiment. During work in different experiments the PAVICOM group designed numerous algorithms of processing particles tracks in complicated events. In this report some of them are represented.

A 'knee-like' approximation of Cherenkov light Lateral Distribution Functions, which we developed earlier, now is used for the actual tasks of background rejection methods for high energy (Tens and hundreds of TeV) gamma-ray astronomy. We use our methods basically for HiSCORE wide angle timing array consisting of Cherenkov light detectors with spacing 100 m covered 0.2 km2 presently and up to 5 km2 in future. However, it can be applied for other similar arrays. It is shown that application of multivariable approach (where 4 parameters of knee-like approximation are used) allows to reach a large factor of background rejection but it strongly depends on number of hit detectors.

Potashev S., Burmistrov Yu., Drachev A., Karaevsky S., Konobeevski E., Zuyev S. Institute for Nuclear Research, Russian Academy of Sciences, 117312, Moscow, Russia E-mail: potashev@inr.ru Two-dimensional hybrid solid state gas multiwire detector of thermal and cold neutrons [1] is created at the Institute for Nuclear Research. The detector has an active area of 128 x 128 mm2 with double gas gap of 2 mm and a 10B converter. The input window is made of a thin aluminum layer (3mm) to prevent scattering and absorption of neutrons. The operation of the detector was studied using W-Be photoneutron source. The photoneutron source (IN-LUE) was created on the base of industrial electron linac LUE-8 operating at electron energy of 7 - 8 MeV, tungsten electron-gamma convertor, photoneutron beryllium target and moderator of fast neutrons. The detector is located at a distance of 6 m from the source at an angle of 60 relative to the electron beam axis. The detector efficiency is estimated as ~3% at neutron wavelength λ = 1.82 Å and 6% at λ = 8 Å. The efficiency of the background detection was less than 0.001% of that for thermal neutrons. The resulting pulse height resolution is 15% and the spatial resolution is 2.5 mm for the X coordinate with gas mixture Ar + 25% CO2 + 0.3% CF3Br under standard conditions. The resistive charge-division readout is applied to determine neutron position from pulse height values. 1. Litvin V.S., Potashev S.I., Razin V.I. and Sadykov R.A. Bull. Russ. Acad. Sci. 75, 229 (2011).

Short-lived hadronic resonances provide the means to study properties of the relativistic heavy ion collisions. The hot and dense medium produced in such collisions can modify spectral shapes of the reconstructed resonances. Due to short lifetimes resonances are sensitive to rescattering and regeneration in the time interval between the chemical and kinetic freeze-outs making them sensitive to properties of the hadronic phase. Along with stable hadrons resonances contribute in systematic study of parton energy loss and intermediate transverse momentum phenomena. Measurements in small systems are used as a reference and utilized in search of collective effects. In this talk we present overview of the most recent ALICE results on resonance production in pp, p-Pb and Pb-Pb collisions at different energies. The results are compared with model predictions and measurements at lower energies.

Proton-nucleus collisions provide a reference to study the signatures already present in the initial state, due to the complex structure of the colliding nuclei which confirm that the suppression of high $p_T$ hadron production observed in heavy ion collisions is a genuine effect of the hot deconfined QGP. However, several measurements of particle production in the low and intermediate momentum region indicate the presence of coherent and collective effects, already in small systems, as those produced in p-Pb collisions. Measurements from proton-lead collisions at $\sqrt{s_{NN}}$=5.02 TeV obtained by the ALICE experiment at the CERN LHC will be presented and compared to p-p, A-A and d-A experimental results at different collision energies and to the available theoretical model predictions.

Transverse momentum spectra of charged particles are an important tool to investigate the properties of the Quark Gluon Plasma created in heavy ion collisions. While the measurement in pp collisions provides a baseline test of perturbative QCD, in Pb--Pb collisions any deviation from a scaling with the number of elementary nucleon-nucleon collisions, quantified by the nuclear modification factor, provides insights on the parton energy loss in the hot and dense medium. We present measurements of transverse momentum spectra in pp and Pb--Pb collisions collected by the ALICE experiment at the top-LHC energy in Run 2 and compare the results to the previous measurements at lower energy as well as to the expectations from Monte Carlo event generators and model calculations which include jet quenching in the medium.

Multiparticle azimuthal correlations are nowadays utilized regularly by all major collaborations worldwide which are analyzing heavy-ion data. Most notably, correlation techniques are used to explore the collective properties of the new state of matter, the Quark-Gluon Plasma (QGP), composed of deconfined quarks and gluons, by performing measurements of anisotropic flow phenomenon in heavy-ion collisions. In this talk we will present in detail multiparticle azimuthal correlations and summarize briefly the most important physical results obtained with them so far.

We report on the measurement of like-sign kaon femtoscopic correlations in p+p collisions at $\sqrt{s}$=200 and 510 GeV and in Au+Au collisions at $\sqrt{s_{NN}}$ recorded by STAR at the Relativistic Heavy Ion Collider. These type of correlations allow to extract statial and temporal characteristics of the particle emitting source. The femtoscopic analysis was performed using one- and three-dimensional correlation functions for several multiplicity (centrality) and pair transverse momentum ranges. The source sizes were extracted by fitting the experimental correlation functions. The measured multiplicity and transverse pair momentum dependencies of the kaon emitting source radii were compared to those obtained for pions.

Long-range correlations between particles separated by a pseudorapidity gap are a powerful tool to explore the initial stages and evolution of the medium created in hadron-hadron collisions. An overview of the long-range correlations measured by the ALICE detector in pp, p-Pb and Pb-Pb will be presented. This includes analyses of forward-backward, two- and multi-particle correlations with the use of the central barrel and forward detectors. Comparisons to existing models will be also discussed.

The Borexino experiment is taking data since 2007 at the „Laboratori Nazionali del Gran Sasso“ in Italy accomplishing outstanding achievements in the field of neutrino physics. Its success is strongly based on the unprecedented ultra-high radio-purity of the inner scintillator core. In this talk, after introducing the main features of the detector, the impressive results for solar and geo-neutrinos obtained by Borexino so far will be summarized. The main focus will be laid on the most recent and most prominent results, i.e. the first real-time measurement of the solar pp neutrino flux and the detection of the signal induced by geo-neutrinos with a significance as high as 5.9 sigma. Besides the measurement of the pp neutrino flux representing a direct probe of the major mechanism of energy production in the Sun, it makes Borexino the only experiment being able to probe the entire solar neutrino spectrum and puts it in the unique position of being capable to test the MSW-LMA paradigm across the whole solar energy range. The geo-neutrino data allow to infer information concerning important geophysical properties of the Earth that shall also be discussed. To conclude the talk, the perspectives of the final stage of the Borexino solar neutrino program that are centered on the goal of measuring the only missing part of the solar neutrino spectrum, the CNO neutrinos, will be outlined. In case of success, this measurement would constitute the climax of Borexino’s long search to reveal the properties of solar neutrinos and extend the understanding of our Sun.

Solar flares are sudden variations in brightness observed near the Sun's surface. Some theorethical models predict production of electron and muon neutrinos with energies up to few tens of MeV during solar flares. In 1980th the Homestake experiment reported excess of detected neutrino events possibly correlated with large solar flares. Since then the interest to similar studies by other neutrino detectors has increased. In this talk we summarize the status of experimental searches and describe the methodology for the study of neutrinos from solar flares in Borexino liquid scintillator detector.

Atmospheric neutrinos are produced in interactions of cosmic rays with atomic nuclei in the Earth’s atmosphere. In low energy neutrino experiments they mainly considered as a background for studied processes. For atmospheric neutrinos in energy range below 1 GeV we present semi-analytical expected yield for four neutrino detection reactions: νp-ES, νe-ES, inverse β-decay and ¹²C(ν, ν′)¹²C*(15.1 MeV), as well as results of Monte-Carlo simulation for other ν¹²C interaction channels. Calculations are made for several neutrino experiments and include neutrino oscillation averaged over neutrino arrival directions.

The Troitsk $\nu$-mass experiment was starter in the 1985 and was initially intended to search for the mass of electron neutrino. Currently it give the best direct upper limit on that mass. In 2012, after reanalyzing old data for traces of relatively light sterile neutrinos (with masses up to 200 eV), the setup was modified to search for sterile neutrinos in a wider range (up to 3 keV and in future probably up to 5 keV). The report contains a brief overview of the experiment layout, past results, some unique techniques developed in this experiment and finally, some preliminary results on keV sterile neutrinos.

High-intensity artificial Cr-51 sources are used to calibrate solar neutrino detectors. The necessary amount of Cr-51 can be obtained by irradiating chromium enriched in Cr-50 in a thermal neutron trap of the SM-3 high-flux reactor in JSC “SSC RIAR”. The paper presents the analysis of irradiation options both using the existing trap and advanced trap designs to be used during the reactor future refurbishment. The feasibility to produce 3.85Ci of Cr-51 by the end of irradiation is shown.

The current status of the short baseline experiment BEST with a 3MCi 51Cr artificial neutrino source to search for transitions of electron neutrinos to sterile states on the Gallium Germanium Neutrino Telescope at the Baksan Neutrino Observatory INR RAS is presented. The experiment has the great potential to search for transitions of active neutrinos to sterile states with Δm2~ 1 eV2 and to set the limits on short baseline electron neutrino disappearance oscillation parameters. The possibilities of the further constraints of the oscillation parameters region with use of 65Zn source are discussed.

The report presents the results of measurements of the spectrum of internal bremsstrahlung (IB) Cr51. The isotope Cr51 was used for production of intense neutrino sources for calibrations of gallium solar neutrino detectors. By measuring the IB spectrum Cr51 it is planned to determine the source activity in the experiment BEST to search for sterile neutrino in gallium target.

Recent data of reactor neutrino experiments give a hint for anomalously low antineutrino flux at short distances. A possible explanation of this anomaly is the presence of sterile neutrinos. SOX project is based on the idea of placing a neutrino source close to a large volume detector in order to look for the flux suppression and the oscillation pattern inside the detector volume. In this project a ~100 kCi 144Ce-144Pr source is intended to be placed under the Borexino detector.

Anisotropic flow of identified charged hadrons are currently being measured at both the Relativistic Heavy Ion Collider (RHIC) and the Large Hadron Collider (LHC), to aid investigations of the temperature (T ) dependence of the equation of transport properties of the hot and dense plasma produced in energetic heavy ion collisions. In this work we will provide the detailed comparison of the measured v2 and v3 of identified charged hadrons from the PHENIX (RHIC) and ALICE (LHC) heavy-ion programs.

Per-event charged particle spectra and nuclear modification factors are measured with the ATLAS detector at the LHC in p+Pbinteractions at sqrt(s_NN)=5.02 TeV. Results are presented as a function of transverse momentum, rapidity, and in different intervals of collision centrality, which is characterised in p+Pb collisions by the total transverse energy measured over the pseudorapidity interval -3.2

Under this study we considered active regions of the 23-rd an 24-th cycle of solar activity which were observed with the 2D spatial resolution at two frequencies: 17 and 34 GHz with the Nobeyama Radioheliograph (NoRH) and we used daily solar observations with the RATAN–600. We detected appearance and rapid development of a compact microwave source above the neutral line of the magnetic field (NLS-source) one-two days or few (14–17) hours before the X-class flares. The position of this source associated with the place of the maximum of magnetic field gradient at the photosphere. A compact source (NLS) under 2D observations at NoRH is characterized by a shift of the centers of brightness in the polarization and intensity before powerful flare. In most cases the formation of δ-configuration of the magnetic field preceded the detection of NLS.

Forward hadron calorimeter (FHCAL) is intended for the measurements of the geometry of heavy ions collisions. The main purpose of the FHCAL is to provide an experimental measurement of a heavy-ion collision centrality and orientation of its reaction plane. Precise event-by-event estimate of these basic observables is crucial for many physics phenomena studies to be performed by the MPD experiment. FHCAL consists of two identical left/right arms placed at the distance of about 3.2 meters from the beam collision point. This is a compensating lead-scintillator calorimeter designed to measure the energy distribution of the projectile nuclei fragments (spectators) and forward going particles produced close to the beam rapidity. The main design requirements of the FHCAL are (a) forward rapidity coverage and sufficient energy resolution to allow for precise collision centrality determination and consequently of the number of participating nucleons and (b) granularity in the plane transverse to the beam direction which is needed for the reaction plane reconstruction. The proposed modular design of the FHCAL covers large transverse area around the beam spot position such that most of the projectile spectator fragments deposit their energy in the FHCAL. The expected FHCAL centrality resolution is below 10% for the most parts of the events, excluding the most central ones, where the internal fluctuation of the number of spectators is significant. At the same time, the proper transverse segmentation and the energy resolution of FHCAL ensures the reconstruction of the event plane orientation with the accuracy of about $30^{0}$.

We demonstrate that the investigations of the forward-backward correlations between intensive observables enable to obtain more clear signal about the initial stage of hadronic interaction, e.g. about the process of string fusion, compared to usual forward-backward multiplicity correlations. As an example the correlation between mean-event transverse momenta of charged particles in separated rapidity intervals is considered. We show that this type of correlation is robust against the volume fluctuations and the details of the centrality determination. The calculations are fulfilled both in the simple model with string fusion by introducing a lattice in transverse plane and in the framework of dipole-based Monte Carlo string fusion model. The dependence of the correlation strength on the collision centrality is obtained for different initial energies. It is shown that at LHC energy the dependence reveals the decline of the correlation coefficient for most central collisions and Pb-Pb, reflecting the attenuation of color field fluctuations due to the string fusion at large string density. This non-monotonic behavior with centrality is achieved only in heavy ion collisions at LHC, while in Au-Au collisions at RHIC and p-Pb at LHC the string density is not enough to provide a decline of the correlation coefficient for most central collisions. We compare the results both with the ones obtained in alternative models and with the ones obtained by us using various MC generators. We conclude that this type of correlation is promising for the observation of the signatures of string fusion and for detailed study of the initial stage of hadronic interaction in relativistic heavy ion collisions at LHC energy. The work was supported by the RFBR grant 15-02-02097-a and the Saint-Petersburg State University grant 11.38.197.2014.

The Projectile Spectator Detector (PSD) is a segmented hadron calorimeter used in NA61 experiment (CERN) to determine a collision centrality as well as an event plane orientation in nucleus-nucleus collisions. The main goal of the experiment includes studying the onset of deconfinement and searching for the critical point of strongly interacting matter. It is of crucial importance to have a precise characterization of the event class with the PSD for the analysis of event-by-event observables. The PSD has been already used for centrality selection on trigger level in measurements of Be+Be and Ar +Sc reactions at beam energies 13 – 158 AGeV and Pb+Pb reaction at beam energy 30AGeV. In 2016, the central modules of PSD have been equipped with new Hamamatsu MPPC silicon photodetectors in order to extend dynamic range for studying Pb+Pb reaction at the full energy range (13 – 158 AGeV). Results of the PSD response on proton and lead beams will be presented.

The simulation software to research the work of the linear modulator with the discharge line on the thyratron (generator with a soft switch) is presented. In this software it is possible to configure the generator and to research the influence of the parasitic inductances and capacitances on the nanosecond pulses.

The physical and mathematical model of the radiation situation in the diamond sensor detector was developed. Count rates of the particle sensors were measured in the registration of a monoenergetic electron and proton radiation. The simulation of the sensor data was made for simultaneously iradiation by electrons and protons with spectral characteristics, that were corresponded to cosmic spectra. It is shown that structure of data, that were measured with sensors, let effectively separate signals from electronic and proton cosmic radiation component.

The software implementation of the voltage pulse generator mathematical model with a hard switch is considered. The interactive object-oriented interface provides the choice of generator parameters and the type of its load, as well as the generator switching on and the analysis of the "waveform" pulse on the load.

This document describes a 2D model of the bipolar transistor 2T312 under X-ray pulse ionizing radiation. Both the Finite Element Discretization and Semiconductor module of Comsol 5.1 are used. We present an analysis of energy deposition in this device under X-ray and the results of transient ionizing current response for some different carrier densities.

Evolution of flaring active regions (AR) shows high spatial complexity and nontrivial changes of observed patterns over time. It is practically impossible to give detailed description of magnetogram morphology. This is why signatures are quite often used: critical points, neutral lines, unsigned and signed areas of magnetic textures. However, when comparing two magnetograms adjacent in time, it is difficult to find or evaluate significant signature changes because of high patterns variability. This is why it is more convenient to use approximating simplicial structures like graphs, namely set of vertices connected by edges. We compute so-called critical nets, which consist of stable minima and maxima points connected by ascending paths in terms of Morse theory. Critical net approximates singular manifold of AR with graph which is rebuilt during evolution. Dynamics regimes can be conveniently tracked using methods of spectral geometry. For that we use discrete laplacian and its spectrum. We present examples of critical nets for flaring AR and estimations of their spectra. This work was supported by the Russian Foundation for Basic Research (grant 15-01-09156 A)

Design and performance of large scittillator detectors developed for fixed-target experiments NA62 and SHIP at CERN will be presented. The main components of the detectors are extruded polystyrene based scintillators, wavelength shifting (WLS) fibers and micropixel avalanche photodiodes, SiPM’s produced by Hamamatsu and SensL. The tests with charged particle beams at CERN showed very good performance of these detectors: high light yield for minimum ionizing particles (MIPs), good timing resolution, and high detection efficiency for MIPs.

The article deals with the latest version of a computer part of Vacuum Engineering laboratory in which means of fragmentary pumping and receiving of fine vacuum are studied. The virtual laboratory allows to carry out a heatup and processing of preselected surface materials of the pumped-out objects in acceptable time limits by using any means of preselected pumping (from the built-in database). It is possible to retrace online dynamics of receiving fine vacuum in time by having started the procedure of pumping.

Computed yield function of solar neutron telescope at Mt. Aragats, for solar neutrons is presented. The computations of cascade in the atmosphere were made by Monte Carlo using the GEANT4-based PLANETOCOSMICS tool. Recalculated attenuation length in the atmosphere for neutrons is presented.

Presented web-based resource for information support the engineering, science and education in Electrophysics, containing web-based tools for simulation subsystems charged particle accelerators. Formulated the development motivation of Web-Environment for Virtual Electrophysical Laboratories. Analyzes the trends of designs the dynamic web-environments for supporting of scientific research and E-learning, within the framework of Open Education concept.

The heavy-ion programme of the NA61/SHINE experiment at CERN SPS is expanding to allow precise measurements of exotic particles with short lifetime. Vertex Detector for open charm measurements at the SPS is being constructed by the NA61/SHINE Collaboration to meet the challenges of high spatial resolution of secondary verticies and efficiency of track registration. This task is solved by the application of the coordinate sensitive Si-sensor chips in CMOS technology with extremely low material budget in the new Vertex Detector. A small-acceptance version of the Vertex Detector is being tested this year, later it will be expanded to a large-acceptance version. Simulation studies will be presented. A method of track reconstruction in the inhomogeneous magnetic field for the Vertex Detector was developed and implemented. Numerical calculations show the possibility of high precision measurements in heavy ion collisions of strange and multi strange particles, as well as other heavy flavours, like charmed particles. The authors of this report acknowledge the support by the Russian Science Foundation research grant 16-12-10176.

Fermi-LAT has made a significant contribution to the study of high-energy gamma-ray diffuse emission and the observation of ~3000 discrete sources. However, one third of all gamma-ray sources (both galactic and extragalactic) are unidentified, the data on the diffuse gamma-ray emission should be clarified, and signatures of dark matter particles in the high-energy gamma-ray range are not observed up to now. GAMMA-400, currently developing gamma-ray telescope, will have the angular (~0.01° at 100 GeV) and energy (~1% at 100 GeV) resolutions in the energy range of 10-1000 GeV better than the Fermi-LAT (as well as ground gamma-ray telescopes) by a factor of 5-10 and observe some parts of the universe (such as Galactic Center, Fermi Bubbles, Crab, Cygnus, etc.) in the highly elliptic orbit (without shading the telescope by the Earth) continuously for a long time. It will permit to resolve gamma rays from dark matter particles, identify many discrete sources (many of which are variable), to clarify the structure of extended sources, to specify the data on the diffuse emission.

The present status of scientific data acquisition system (SDAQ) developed by SRISA for the GAMMA-400 space telescope mission is presented. SDAQ provides the collection of the data from telescope detector subsystems (up to 100 GB per day), the preliminary processing of scientific information and its accumulation in mass memory, transferring the information from mass memory to the satellite radio line for its transmission to ground, the control and monitoring of the telescope subsystems. SDAQ includes special space qualified chipset designed by SRISA and has scalable modular net structure based on fast and high-reliable SerialRapidIO 1.25 Gbit/sec interface.

The detailed description of special radiation-hardened microprocessor series developed by SRISA for different space applications is presented. The microprocessors have 32-bit and 64-bit KOMDIV architecture and built-in fast SpaceWire, SerialRapidIO, Ethernet, MIL-STD-1553B interfaces. These devices will be used for design of GAMMA-400 space telescope scientific data acquisition system and can be applied in the other future highly informative experiments in deep outer space (such as “Millimetron” observatory, etc.).

Modifying a method of incident angle reconstruction for low-energy gamma rays in the GAMMA-400 gamma-ray telescope. The GAMMA-400 gamma-ray telescope is designed to measure the gamma-ray fluxes in the energy range from 20 MeV to 1 TeV, performing a sensitive search in high-energy gamma-ray emission when annihilating or decaying dark matter particles. Such measurements also will concern the following scientific goals: searching for new and studying known Galactic and extragalactic discrete high-energy gamma-ray sources: supernova remnants, pulsars, accreting objects, microquasars, active galactic nuclei, blazars, quasars; studying their structure with high angular resolution and measuring their energy spectra and luminosity with high-energy resolution; identifying discrete gamma-ray sources with known sources in other energy ranges. The major advantage of the GAMMA-400 instrument is excellent angular and energy resolutions for gamma rays above 10 GeV. The gamma-ray telescope angular and energy resolutions for the main aperture at 100-GeV gamma rays are ~0.01° and ~1%, respectively. The motivation of presented results is to improve physical characteristics of the GAMMA-400 gamma-ray telescope in the energy range of ~10-100 MeV, most unexplored range today. Such observations are crucial today for a number of first-rank problems faced by modern astrophysics and fundamental physics, including the origin of chemical elements and cosmic rays, the nature of dark matter, and the applicability range of the fundamental laws of physics. To improve incident angle reconstruction accuracy for low-energy gamma rays the special analysis of topology of pair-conversion events in thin layers of converter was performed. Choosing the pair-conversion events with more precise vertical localization allows us to obtain significantly better angular resolution in comparison with previous and current space and ground-based experiments. For 50-MeV gamma rays the GAMMA-400 gamma-ray telescope angular resolution is better than 5°.

Timing large area plastic scintillation detectors are developing for the space gamma-ray telescopes now. For the in-flight calibration of these detectors the use of ultra-violet light-emitting diode, irradiating the 1 m long detector module at the center along its width is suggested. The results of the measurements show the possibility of this calibration system implementation.

The timing large area plastic scintillation detectors with silicon photomultipliers as photosensors properties were investigated using a cosmic radiation at the ground level. Different techniques of the amplitude spectra and efficiency measurements were implemented. The measurements results are presented also.

Scientific project GAMMA-400 (Gamma-Astronomy Multifunction Modules Apparatus) relates to the new generation of space observatories for investigation of cosmic gamma-emission in the energy band from $\sim~{20}$ MeV up to several TeV, electron/positron fluxes from $\sim~{1}$ GeV up to $\sim~{10}$ TeV and cosmic-ray nuclei fluxes with energies up to $\sim~{10}^{15}$ eV in the main aperture by means of GAMMA-400 gamma-telescope represents the core of the scientific complex. For gamma-rays in the energy region from 10 to 100 GeV expected energy resolution changes from $\sim~2\%$ to $\sim~1\%$ and angular resolution from $\sim~0.1\%$ to $\sim~0.01\%$ respectively, electron/protons rejection factor is $\sim~{5}•{10}^{5}$. The GAMMA-400 satellite will be launched on the high apogee orbit with following initial parameters: apogee altitude $\sim~300000$ km, perigee altitude $\sim~500$ km, rotation period $\sim~7$ days, inclination to the equator plane $\sim{51}^{o}$. The active functioning interval will be 5-10 years. The system of triggers and counting signals formation represents the electronic system consists of control and interface unit, set of program controlled digital delay lines, counters and units for master triggers signals formation from any combination of input digital and analogue pulses from detecting subsystems of gamma-telescope. The structure, logic of operation and distinctive features of the system are presented.

GAMMA-400 (Gamma Astronomical Multifunctional Modular Apparatus) parameters are optimized for detection of gamma-quanta with the energy $\sim~100$~GeV in the main aperture. Also there are opportunities to detect particles in additional and lateral apertures. Registered events identification procedures details are discussed in the presented article for gammas, electrons/positrons and protons both in low and high energy bands of 0.2 - 10~MeV in additional and lateral apertures and from ~20~MeV to several TeV in all three ones. It allows providing energy resolution $8\% - 2\%$ for gamma-quanta in low energy region and $~2\%$ for gammas and electrons/positrons in high one.

The features of organization, operation principle and characteristics of the data acquisition system of a new cluster type shower array NEVOD-EAS which is being created in MEPhI (Moscow, Russia) are discussed. The main structural element of the setup is a cluster of scintillation detector stations (DS). Each cluster includes 4 DS consisting of 4 scintillation counters of the EAS electron-photon component particles, as well as of local post (LP) of primary data processing. LP performs preliminary processing of experimental information (digitizing of analog signals from the counters, selection of events according to specified triggering conditions), ensures cluster operation in exposition and monitoring modes, controls and maintains operating temperature, provides DS power supply, as well as transmits data to the central DAQ post (CP). Central post of the NEVOD-EAS array provides reception, storage, express analysis of experimental data and synchronous operation of all clusters at the unified clock frequency corrected according to timestamps from the GPS/GLONASS antenna.

In 2015-2016 in MEPhI (Moscow, Russia) on the basis of the Scientific and Educational Center NEVOD the central part of a new cluster type array NEVOD-EAS for the determination of size, arrival direction, axis position of extensive air showers with energies of 10^15 – 10^17 eV was created and launched. Central part of the setup includes 4 clusters of scintillation detector stations located around the complex of detectors NEVOD and DECOR at the area of about 10^4 m^2. Studies of amplitude and time parameters of cluster response, as well as EAS registration are being conducted. The express analysis of experimental data and monitoring of operating parameters are being performed. The results of studying of the setup operating parameters and analysis of experimental data obtained during continuous series of measurements on the registration of extensive air showers with the central part of NEVOD-EAS are presented.

The large-scale coordinate-tracking detector TREK for registration of inclined EAS is being developed in MEPhI. Detector is based on the multiwire drift chambers from the neutrino experiment at the IHEP U-70 accelerator, their key advantages are a large effective area (1.85 sq.m), a good coordinate and angular resolution with a small number of measuring channels. Detector will be operated as a part of the unique scientific facility NEVOD, in particular, jointly with Cherenkov water detector (CWD) with volume of 2000 cubic meters and coordinate detector DECOR. The first part of the detector named Coordinate-Tracking Unit based on the Drift Chambers (CTUDC) representing two coordinate planes of 8 drift chambers in each has been developed and mounted on the opposite sides of the CWD. It has the same principle of joint operation with NEVOD-DECOR triggering system and the same drift chambers alignment, so main features of the TREK detector will be examined. Results of a cross-calibration of the CTUDC and coordinate-tracking detector DECOR and a joint operation with NEVOD-DECOR complex are presented.

Some results on the EAS neutron component measured by means of the PRISMA-32 array are presented. The array consists of 32 en-detectors capable to detect two main EAS components: electronic one consisting of charged particles, and hadronic one by measuring delayed thermal neutrons accompanying the showers. For thermal neutrons detection, we use a compound of a well-known inorganic scintillator ZnS(Ag) and LiF, enriched to 90 % with 6Li isotope. This array allows register neutron component at whole area of the EAS. Information about EAS electron and neutron component can be used for EAS energy estimations.

The detection system of the Cherenkov water detector NEVOD includes 546 photomultipliers FEU-200 (Joint-Stock Company "Ekran - Optical Systems", Novosibirsk). To control the main parameters of the PMT the monitoring procedure is conducted every 20 minutes. During monitoring gain dynode system, the linking coefficient of two linear ranges of the 12th and 9th dynodes and counting rate of noise pulses are measured for each PMT. The analysis of behavior of characteristics of PMT FEU-200 during the period from 2011 to 2016 years is presented in the report.

The detector based on the drift chambers for registration of inclined EAS is being developed in the MEPhI. One of the key characteristic of inclined EAS is multiplicity of muon bundles. Numerical simulation and simulation by Geant4 were performed to study drift chamber abilities for event multiplicity definition. Three methods were developed to reconstruct particle tracks: enumeration, search of a straight section and a histogram method. This work contains results of an application of the reconstruction methods to simulated and experimented data.

Registration systems of rare events from $^{71}$Ge decay in radiochemical gallium experiments SAGE and BEST are presented, where miniature proportional counters are used as detectors. The registration of the events is provided by eight counting channels simultaneously in the energy range of 0.4-15 keV which includes the $^{71}$Ge decays in the region of the L and K peaks with total efficiency up to 75%. Data analysis is based on full charge pulse shape recording using digital oscilloscope. Effective background discrimination is basically obtained due to low noise ($<$0.32 keV) and wide bandwidth ($>$100 MHz) of the system electronics. The design and main parameters of base components of the registration systems, description of electronics and comparison of their electrical and counting characteristics are given.

Response function simulation using Geant 4 for the detector based on NaI crystal of complex shape in registration systems for SAGE and BEST experiments is presented. Cylindric NaI crystal has a large well for placing up to eight proportional counters. The detector is using as anti-coincidence shield for counters and an instrument for detail analysis of different gamma-rays sources. The result of detector response function simulation for different background sources and their registration efficiency are given.

Muon hodoscope URAGAN detects the flux of cosmic ray muons on the Earth’s surface simultaneously from various directions (hodoscopic mode). This allows studies of the energy, angular and spatial-temporal characteristics of variations of the cosmic ray muon flux during Forbush decreases (FD). These characteristics are obtained for the FDs detected in the period from 2006 to 2014. The results of the analysis of the largest (with amplitudes more 1.5%) FDs are discussed. The FDs characteristics are compared with the conditions in of the near-Earth space.

Based on the new fit of hadron yield ratios within the multicomponent hadron resonance gas model we have found several remarkable irregularities at chemical freeze-out. In particular, 121 hadron multiplicity ratios measured in the nucleus-nucleus collisions at AGS, SPS and RHIC energies were successfully described within the new formulation of HRGM with $\chi^2/dof \simeq 63.978/65 \simeq 0.98$. A dramatic jump in the center of mass collision energy dependence of pressure, energy density and baryonic charge density in the narrow range between 4.3 and 4.9 GeV is found. These irregularities are also accompanied by a sudden increase of the particle decays at chemical freeze-out which is seen at this collision energy range. We argue that a strong correlation which we observe between the previously found irregularities and an enhancement of strangeness production can serve as the quark-gluon plasma formation signature. Thus, we conclude that a dramatic change in the system properties seen in the narrow collision energy range $\sqrt{s_{NN}} = 4.3-4.9 $ GeV opens entirely new possibilities for experimental studies of quark-gluon plasma properties at NICA JINR and FAIR GSI accelerators.

The liquid droplet formula is applied to an analysis of the properties of geometrical (anti)clusters formed in SU(2) gluodynamics by the Polyakov loops of the same sign. Using this approach, we explain the phase transition in SU(2) gluodynamics as a transition between two liquids during which one of the liquid droplets (the largest cluster of a certain Polyakov loop sign) experiences a conden-sation, while another droplet (the next to the largest cluster of the opposite sign of Polyakov loop) evaporates. The clusters of smaller sizes form two accompanying gases, which behave oppositely to their liquids. The liquid droplet formula is used to analyze the size distributions of the gas (anti)clusters. The fit of these distributions allows us to extract the temperature dependence of surface tension and the value of Fisher topological exponent for both kinds of gaseous clusters. It is shown that the surface tension coefficient of gaseous (anti)clusters can serve as an order parameter of the deconfinement phase transition in SU(2) gluodynamics. The Fisher topological exponent of (anti)clusters is found to have the same value 1:806 0:008. This value disagrees with the famous Fisher droplet model, but it agrees well with an exactly solvable model of nuclear liquid-gas phase transition. This finding may evidence for the fact that the SU(2) gluodynamics and this exactly solvable model of nuclear liquid-gas phase transition are in the same universality class. Kewords: geometrical clusters, size distributions, liquid droplet model formula, surface tension

We present the status of the analyses and latest results on $\pi^0$-hadron correlations measured with ALICE experiment in pp and Pb-Pb collisions at $\sqrt{s_{NN}}$ = 2.76 TeV and p-Pb collisions at $\sqrt{s_{NN}}$ = 5.02 TeV. Two-particle correlations technique is a powerful tool to study collective motion effects and energy deposition of partons in quark-gluon matter formed in high-energy particles collisions. Measuring the hadron per-trigger yield with high $p_T$ trigger hadrons we observe the correlation of particles belonging to the same jet as the trigger hadron, and those hadrons from the jet on the opposite side. A detailed study of di-hadron correlations with its centrality dependence in p-Pb and Pb-Pb collisions, comparison to pp collisions at the same $\sqrt s$ and model predictions could provide more insight to the nature of the jet modification in Quark Gluon Plasma (QGP). Using identified particles as trigger is advantageous for determination of constrains on theoretical models describing parton energy loss in the quark-gluon medium. ALICE experiment includes two electromagnetic calorimeters, PHOS and EMCAL, which can measure and identify $\pi^0$ mesons in a wide $p_T$ range. Associated charged hadrons are measured with the ALICE Central Tracking System. We present measured correlation functions and per trigger yields and compare them to the theoretical predictions.

Measurements of direct photon and neutral pion production in heavy-ion collisions provide a comprehensive set of observables characterizing properties of the hot QCD medium. Unlike hadrons, direct photons are produced in all stages of a nucleus-nucleus collision and therefore probe the initial state of the collision as well as the space-time evolution of the produced medium. Prompt direct photons provide means to control the initial stage of the collision and ensure that the yield suppression of hard hadrons and in particular neutral pions in Pb-Pb collision is a final-state effect and should be attributed to the parton energy loss in the hot medium. The thermal direct photon spectrum and flow carry information about temperature and space-time evolution of the emitting medium. Measurements of neutral meson spectra in pp collisions at energies $\sqrt{s}$=0.9, 2.76, 7 TeV serve a reference for heavy-ion collisions, and also provide valuable data for pQCD calculations and for studying scaling properties of hadron production at the LHC energies. The ALICE experiment at LHC reconstructs photons via complementary methods, using the ALICE electromagnetic calorimeters and the central tracking system identifying photons converted to $e^+e^-$ pairs in the material of the inner barrel detectors. Neutral pions are reconstructed using their two-photon decays. Since calorimetric and tracking approaches have practically independent systematic uncertainties, their comparison provides a strong cross-check. In this talk, we review recent ALICE results on neutral pion and direct photon production in pp, p-Pb and Pb-Pb collisions.

We address the issue of energy and charge dependence of global polarization of $\Lambda$ hyperons in peripheral Au−Au collisions recently observed by the BES STAR collaboration at RHIC. We compare different contributions to the anomalous mechanism relating polarization to vorticity and hydrodynamic helicity in QCD matter. We stress that the suppression of the gravitational anomaly contribution in strongly correlated matter observed in lattice simulations confirms our earlier prediction of rapid decrease of polarization with increasing collision energy. Our mechanism leads to polarization of anti-$\Lambda$ of the same sign and larger magnitude than the polarization of $\Lambda$. Polarization calculated in the kinetic QGSM model has a maximum at the NICA and FAIR energy range. The energy and charge dependence of polarization is suggested as a sensitive probe of fine details of QCD matter structure.

Spherically symmetric relativistic stars with the polytropic equation of state, which possess the local pressure anisotropy, are considered in the context of general relativity. The generalized Lane-Emden equations are derived for the arbitrary anisotropy parameter. They are then applied to some special ansatz for the anisotropy parameter in the form of the differential relation between the anisotropy parameter and the metric function *ν*. The analytical solutions of the obtained equations are found for incompressible fluid stars and then used for getting their mass-radius relation, gravitational and binding energy. Also, the equation for studying the dynamical stability of incompressible fluid stars with respect to radial oscillations is obtained and analyzed.

In ultrarelativistic collisions of heavy-ions at the RHIC and LHC colliders we have seen behaviour which can be interpreted as a formation of locally thermalised system which expands as a fluid. In this talk I will review this data, and what we have learned of the dissipative properties of the formed partonic matter based on it.

Recent ideas will be presented on critical phenomena in the context of event-by-event fluctuation measurements. More in particular, the interface between experimental measurements and theoretical calculations will be explored. Moreover, insights gained from different experimental results will be highlighted and discussed.

Exotic states of the nuclear matter i.e., of the nuclei in extreme states (with high spin, large deformation, high density and temperature, the neutron- or proton- rich nuclei on the boundary of nucleon stability) play an important role in studies of fundamental nuclear properties, which bring us closer to deducing the equation of state of the nuclear matter. This is undoubtedly of great significance for extrapolating microcosm characteristics to the macroworld that presents our Universe. Synthesis and study of neutron-rich isotopes have two main goals: finding the position of neutron stability boundaries and obtaining data on properties of exotic nuclei near these boundaries. The development of accelerator technology has made it possible to obtain the accelerated beams of secondary radioactive nuclei. In this connection, new vast opportunities have opened up for studying both the structure of light exotic nuclei themselves and the peculiarities of nuclear reactions induced by these nuclei. It is extremely important to obtain new information regarding nuclei near the nucleon stability boundary because considerable deviations of properties of such nuclei from the widely known regularities may be expected (and are already observed). Here the nuclei in a range of small Z serve as convenient objects for investigation. However, the question of how general the corollaries made for this small number of nuclei is crucial. The experiment alone can give an answer to this question. At present the most sophisticated physics experiments, which are carried out at large-scale accelerator facilities and require enormous financial investments, can be realized only through the combined efforts and cooperation of the leading scientific centers. As an example, we can mention the creation of the Large Hadron Collider at CERN and of the heavy ion accelerators at the Joint Institute for Nuclear Research (Dubna) which count about 20 member-states. Thus, the research is being done in collaboration of the research centers of several countries. Each country makes its financial and intellectual contribution to the creation of the large-scale facilities, allowing to penetrate deeply into the mysteries of matter and to obtain new information not only for nuclear physics, but also for other scientific fields such as astronomy, condensed matter physics and up-to-date technologies. The present work reviews the properties of the super neutron-rich isotopes. The changes in nuclear structure appearing as one goes away from the β-stability line are discussed in detail. Information is presented on the mass (hence, on the separation energy of nucleons and on nuclear stability), the radii of nucleon distributions, the momentum distributions of fragments from the break-up of neutron-rich nuclei, on the possibility of halo formation as well as on the deformation and quantum characteristics of the ground states of different isotopes. The location of the neutron drip line and questions about the stability of nuclides are considered in connection with the weakening or even vanishing of the shell effects at the magic numbers 20 and 28, and the discovery of the new neutron magic number.

A low power area efficient 5 bit current steering DAC is presented. The proposed DAC is integrated to prototype the readout channel for muon chamber in CBM experiment. DAC was implemented with an area of 0.019 mm2 in the CMOS process using UMS MMRF 180 nm technology. This DAC has ultralow power consumption - 25μW. The measured differential nonlinearity (DNL) is better than 0.25 LSB, integral nonlinearity (INL) is better than 0.2 LSB. In this paper the main steps of design flow, simulation results and measurement results are presented.

Kirillovykh E.V., Nikitaev V.G.,1, Ulin S.E.1, Polyakov E.V.1, Trubilin V.N., Orlova O.M.. 1National Research Nuclear University «MEPhI» (NRNU MEPhI) Russia, 115409, Moscow, Kashirskoe shosse, 31 2Ophthalmology Centre FMBA of Russia Russia 123098, Moscow, Gamalei st., 15. Automation aid system for an ophthalmologist is being proposed. The system is to enable an ophthalmologist to gather/acquire primary medical background by means of questioning. Application of the system will facilitate early cataract diagnosis. The system will allow a doctor to select a possible kind of intraocular lens for phacoemulsification. Results of the system’s operation are presented.

A low-power digital peak detector, intended for use in a 32-channel IC, reading out and processing the signals of the FAIR accelerator detectors of the CBM experiment, is considered. In compare with its analogues the peak detector (PD) has been added by an option of correcting input disturbances, which may be digitized by on ADC. The block has been designed for operation with an 8-bit ADC, placed in the IC’s readout channel and having the following characteristics: power consumption 0.46 mW, occupied area 115 x 115 mm2, operation frequency of 50 MHz. Due to its efficient parameters on power consumption and occupied areas the given block meets the requirements, set to the CBM electronics, and will be included in the 32-channel IC for reading out the GEM detector signals, which is under development in MEPhI ASIC LAB. The PD block is implemented by the 180nm CMOS technology of UMC (Taiwan).

An application specific design flow for multichannel analog-digital ICs for front end electronics is presented. The design flow allows to reduce the terms of designing the IC, raise the efficiencies of CAD operation and reach substantially better parameters of the IC in performance, occupied area and power consumption. This flow was successfully applied to the design of the readout ASIC prototype for the CBM muon chambers. The approach was probated in UMC CMOS MMRF process.

The structure of the interface of data exchange with the GBTX chip for the CBM experiment is considered. The interface generate data package, consisting of the digital codes of signal amplitude, of signal superposition in peak detector, of signal arrival time and channel number, wherein the event has occurred, generated by the readout blocks of IC. The created data package is coded according to the 8b/10b format for transferring to the GBTX chip. The package of control date (warnings on error and desynchronisation) of registers for a correct exchange (correspondence) under the GBTX protocol. The adjustment of the quantity of channels, generating data packages, connected to the GBTX chip, is possible. The interface has been design according to the 180nm CMOS technology of UMC.

Nikitaev V.G., Polyakov E.V. National Research Nuclear University «MEPhI» (NRNU MEPhI) Russia, 115409, Moscow, Kashirskoe shosse, 31 The paper considers random component error study while measuring characteristics of cell nuclei structure with application of structural unit technique. Poor accuracy may result in an incorrect diagnosis. Error estimation has been carried out in the information-measuring system of acute leukemia as well as its versions diagnostics.

1National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russian Federation, 115409, Moscow, Kashirskoe shosse, 31 2N.N. Blokhin Russian Cancer Research Center, Russian Federation, 115478, Moscow, Kashirskoe shosse, 23 3A.I. Evdokimov Moscow State University of Medicine and Dentistry, Russian Federation, 127473, Moscow, Delegatskaya st., 20/1. The method of creation of information system for the diagnosis of melanoma is described in the presented work. Malignant tumors are investigated at the level of macro - and microimages in combination with clinical data. The development is made with the use of MySQL. The information system is a result of joint activities of the National research nuclear University (MEPhI) and the N.N.Blokhin Russian Cancer Research Cente.

Nikitaev V.G., Polyakov E.V. National Research Nuclear University «MEPhI» (NRNU MEPhI) Russia, 115409, Moscow, Kashirskoe shosse, 31 The effect of artifacts on the result of blast and lymphocytes separation in the task of diagnosing of acute leukemia types is under consideration. Within the framework of the investigation, a group of artifacts was formed and a technique for study has been proposed. The conducted experiments have showed a degree of the effect of artifacts on the result of cell classification, which is to be taken into account while diagnosing.

One of the main stages of blood and bone marrow cells recognition at the acute leukemia diagnosing is the leukocyte segmentation. The quality of cell separation methods in computer microscopy can be constrained by different exposure conditions which can in turn cause worse segmentation quality. Leukocyte segmentation efficiency based on the histogram method is considered in the paper.

The method of selection of useful events in the stopped pion absorption reactions has been developed. The method is based on the use the system of monitor semiconductor detectors calibrated using registration of pion stops in the “living” target (a silicium detector). The monitor system energy threshold values are determined that allow to reach the maximum efficiency (~ 90%) of the selection of pion stops in the targets. The method was tested on the experimental data obtained on targets 6,7Li, 9Be, 10,11B, 12C, 28Si, 40Ca, 59Co, 93Nb, 114,117,120,124Sn, 169Tm, 181Ta, 209Bi. It is shown based on the analysis of the systematical errors that the absolute normalization precision of spectra with the method is 8%. This precision is significantly better than the results obtained with other methods.

A method for 222Rn concentration monitoring by means of intensity measurement of its daughter nuclei (214Pb and 214Bi) gamma-ray emission using xenon gamma-ray spectrometer is presented. Testing and calibration results for a gamma-spectrometric complex based on xenon gamma-ray detector are described.

Silicon photomultipliers (SiPM) are very promising semiconductor single photon sensitive devices with high gain. One of the challenge of use these detectors in radiation environment such as high energy physics experiments is a radiation hardness. Experimental samples were produced and then irradiated with different doses of X-rays with energy E≈12 keV. Simulation of these SiPMs was performed using Synopsys TCAD software. Current-voltage characteristics were measured and simulated for the low voltages. Correlation between different parts of SiPM structure and current-voltage characteristics will be presented.

Hi-Cal (High-Altitude Calibration) is a balloon experiment that will be launched in Antarctica after ANITA-IV (Antarctic Impulsive Transient Antenna) and will generate a wide beam pulse in the frequency range expected from radiation induced from a cosmic ray shower. In this work a device based on an array of silicon photomultipliers (SiPMs) for determination of the azimuthal position of Hi-Cal is presented. The angular resolution it provides is about 3 degrees. Since during the flight at the altitude of ~38 km the pressure will be ~0.5 mbar and temperature ~ – 20 °C, the equipment has been tested in a chamber at different pressures (0.5 ÷ 1000) mbar and temperatures ( –40 ÷ +50) °C.

The paper describes methodology of substrate noise isolation for ASICs implemented in the CMOS processes. Up-to-date CMOS technologies allow embedding the digital processing blocks into the same die as the readout analog part. This significantly improves the functionality and complexity of the readout ASICs. In fact performance of the precision analog circuits (e.g. charge sensitive amplifier, shaper, etc.) can suffer from the additional noise contribution from the high-frequency digital part. This work describes the ways of decrease the substrate noise influence on the sensitive circuits of the readout channels. Simulation results and comparison of different isolation approaches are considered in the paper.

Polyakov E.V.1, Sukhova O.G.1, Korenevskaya P.Yu.1, Ovcharova V.S.1, Kudryavtseva I.O.1, Vlasova S. V.1, Selchuk, V.Y.1, 2, 3 1National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russian Federation, 115409, Moscow, Kashirskoe shosse, 31 2N.N. Blokhin Russian Cancer Research Center, Russian Federation, Russian Federation, 115478, Moscow, Kashirskoe shosse, 23 3A.I. Evdokimov Moscow State University of Medicine and Dentistry, Russian Federation, 127473, Moscow, Delegatskaya st., 20/1. Stomach cancer is one of the most common causes of death among cancer patients. The creating of integrated expert system for decision support is aim of the work. The system includes the data of histological, cytological, and clinical research. The system is aimed at improving the quality of diagnosis of stomach cancer.

The trend of using of the radiaton with shorter wave length in leading high technological processes demands the detected search of materials for the solid-state electronics equipment and optical systems of an ultra violet and vacuum ultra violet spectral range. Diamond photon detectors of ultra violet radiation have the advantage of their opponents due to their unique properties, such as high sensitivity at the range of 190-250 nm and low sensitivity to the solar irradiation. The modification of semiconductive diamond material properties by the doping to get photon detectors with different of photosensitivity range is of a great interest. Due to this fact the spectroscopic investigation of artificial diamonds doped with boron took place for the definition of their applicability to produce the wide-spectral photosensitive equipment. The samples of thin diamond films were cut out in a crystallography plane (001). Sample transmission spectra were measured by vacuum infrared Fourier transform spectrometer at the range of 400-7000 sm -1. As a result it was explored that diamond based detectors doped with boron could be applied for the detection of infrared irradiation at the average infrared spectral range, however it is necessary to optimize the doping level of diamond materials to reach the compromise between the sensitivity and the speed capability of produced diamond photodetectors.

The evolution of gaseous detectors and their main characteristics are presented. The performance of various types of detectors and the main trends in the development of Micro-Pattern Gaseous Detectors are illustrated. The efforts in efficiently detect charged particles, neutrons, gamma and X-rays are described. The field of gaseous photon detectors is then described in details and the perspectives of future advances in gaseous detectors are discussed.

Integrated Circuits are one of the important elements of detector system. A number of factors make ICs obligatory for Particle Physics and Astrophysics experiments. These are: integration scale, low power dissipation, radiation tolerance. Today chips should provide new level of functionality, fitting to a new set of constraints and trade-offs. The talk presents overview of the state of the art and trends in nowadays chip design. It shows a next stage of micro- and nanoelectronics usage at physical instrumentation.

The paper is a brief review of activities of National Research Nuclear University “MEPhI”, and Federal State Unitary Enterprise “VNIIA” in the development of radiation detectors for common use. It describes design and operating characteristics of the following neutron and X-ray (Gamma) detectors. 1) Radiographic detectors for imaging X-rays and neutrons [1-9]: - detectors for fast neutron radiography with a cone beam; - detector for simultaneous imaging fast neutrons and X-rays; - detector for pulsed radiography with a plasma focus generator. 2) Segmented 3-D arrays of scintillation detectors [10]. The 3-D array of scintillation detectors is a three dimensionally configured system consisting of scintillation elements coupled with photoreceivers and front-end electronics. The considered concept of highly segmented 3-D arrays of scintillation detectors is based on the application of crossed wavelength shifting (WLS) fibers reading out scintillation bursts generated in scintillation elements. The scintillation location (corresponding scintillation element) is being fixed by the intersection point of two crossed WLS fibers generating optical signals at their ends practically at the same time. The application of the crossed WLF fibers enables the large volume 3-D arrays design. One of the most important features of 3-D arrays is the capability of radiation source detection and imaging. At that 3-D arrays allow to: - identify the radiation source; - determine the source position; - measure the source activity; - discriminate neutrons and gamma rays in mixed radiation fields; - reject background, and to improve sensitivity of interrogation systems. 3) Multi-energy X-ray sensors [11]. The operation of the described multi-energy sensor (MES) is based on the relationship between the spatial distribution of scintillation signal generated in a scintillation plate, stretched along the radiation beam, and the radiation spectrum. For that, the scintillation plate consists of a number of scintillators placed one after another with effective atomic charge increasing along the plate.The scintillators and their sequence are chosen in such a way that the radiation hitting any scintillator does not contain X ray quanta with the energy corresponding to the K-edge of the photo-absorption band and to the production of electron-positron pairs in this scintillator. MES can be used to measure X-ray energy distribution in the range of 15 keV-1 MeV. 4) Position sensitive detectors for well logging devices [12]. Position sensitive detectors have been invented for registering spatial distribution of both neutrons and gammas in a well while well logging. They consist of cylinder-shaped coaxial arrays of elongated scintillators. The opposite ends of each scintillator are connected to two photoreceivers. The arrays each provides registering a specific radiation. The scintillator type in an array and arrays positional relationship are accordingly chosen to register different radiation at the same time. Detectors axial resolution is supported by the amplitude comparison of two scintillation signals received by photoreceivers. Detectors azimutal resolution is privided by arrays segmention. Measurements of neutron and gamma spatial distributions provide more precise computing formation density and porosity, fixing the boring tool position in regard to the formation boundaries, as well. 5) Neutron electrometrical sensors [13]. Neutron electrometric sensors (NES) are based on accumulating electric charge when irradiated by neutrons. They contain the emitter and the absorber of charged particles. The absorbed charge can be measured in a variety of ways using, for example: the frequency of the emitter and the absorber electric locking, their displacement, the deformation of the elastic element (in the presence), electric field strength in the gap between the emitter and the absorber. NES may be used, for example, in control systems of nuclear reactors and subcritical assemblies, for measuring pulsed neutron flux, in scientific investigations, as well. ## References ## 1. V.I. Mikerov, A.P. Koshelev, O.V. Ozerov, A.S. Sviridov, and D.I. Yurkov, Two Dimensional and Linear Scintillation Detectors for Fast Neutron Imaging – Comparative Analysis, 2014 JINST 9 C05003. 2. E. Bogolubov, A. Koshelev, V. Mikerov, An Estimation of Efficiency and Spatial Resolution of Radographic Detectors for Fast Neutrons, Nuclear Physics and Engineering, Vol. 1, #4 (2010) 319-325 (in Russian). 3. Yu.N. Barmakov, E.P. Bogolubov, V.I. Mikerov, G.A. Smirnov, Neutron Radiography on the basis of Generator Sources, Nuclear Physics and Engineering, Vol. 1, #1 (2010) 61-69 (in Russian). 4. E.P. Bogolubov, M.V. Koltunov, B.D. Lemeshko, V.I. Mikerov et al., Application of a Plasma Focus-based Source for Fast Neutron and X-ray Radiography, NIM A 605 (2009) 62–64. 5. V. Mikerov, E. Bogolubov, V. Samosyuk, S. Verushkin, Fast Neutron Imaging with CCD Detectors and Imaging Plates, POS (FNDA2006) 007. 6. V. Mikerov, V. Samosyuk, S. Verushkin, Detectors Based on Imaging Plates for Fast Neutron Radiography, NIM A 542 (2005) 192–196. 7. E. Bogolubov, O. Bugaenko, S. Kuzin, V. Mikerov et al., CCD Detectors for Fast Neutron Radiography and Tomography with a Cone Beam, NIM A 542 (2005) 187–191. 8. Yu. Barmakov, E. Bogolubov, A .Koshelev, V. Mikerov, V. Ryzhkov, Detection Quantum Efficiency and Spatial Resolution of Neutron CCD-detectors, NIM B 213 (2004) 241-245. 9. V. Mikerov, I. Zhitnik, A. Ignat’ev et al., Neutron Tomography with High Spatial Resolution, Physica Scripta 57 (1995) 190-195. 10. E. Bogolubov, A. Koshelev, V. Mikerov, and A. Sviridov, Specific Features of 3-D Detection Arrays of Plastic Scintillators, NIM A 652 (2011) 99-102. 11. V. Mikerov, A. Koshelev, O. Ozerov, A. Sviridov, and D. Yurkov, Multi-Energy X-ray Sensors Based on Pixilated Scintillators - Conceptual Study, IEEE Transactions on Nuclear Science, Vol. 60, Issue 2 (2013) 963-967. 12. Patents RF for invention: # 2574322, # 2574323, # 2574415, # 2574416; patent RF for utility model # 153278. 13. E. Bogolubov, A. Koshelev, V. Mikerov, and A. Sviridov, Electrometric Sensors for Neutron Radiation: Conceptual Study, 2012 JINST 7 C03026.

Results of nuclear physics research made using track detectors are briefly reviewed. Advantages and prospects of the track detection technique in particle physics, neutrino physics, astrophysics and other fields are discussed on the example the results of research into the search for direct origination of tau neutrino in a muon neutrino beam within the framework of the international experiment OPERA (Oscillation Project with Emulsion-tRacking Apparatus) and works on search for superheavy nuclei in nature on base of their tracks in meteoritic olivine crystals. The spectra of superheavy elements in galactic cosmic rays are presented. Prospects of using the track detection technique in fundamental and applied research are reported.

The development of an analog read-out channel for time projection chambers (TPC) is presented both in schematic and layout. Structure of the channel consists of a preamplifier, fourth order shaper and differential buffer. It also includes pole-zero cancellation circuit. The channel operates with positive and negative polarities of input charge and has a single-ended input and differential output. The prototype has the following features: dynamic range of 100 fC for both polarities, 20 mv/fC of sensitivity for differential output, peaking time – 160 ns, ENC - <1000e at 40 pF of source capacitance. The presented channel was designed and verified in the CMOS UMC MMRF 180 nm process. The results of post layout simulation are presented.

Noted that the work of on-board and land data transmission systems, operating at speeds of several Gbit/s and above, greatly influenced by the parasitic parameters of the internal and external connections of the chip, which leads to violation of the integrity of transmitted and received signals, including due to the effect of interference at common circuits. The method of analysis of the impact of interference on the supply lines and ground within the front-end parts of high-speed transceivers to establish a predominantly circuit macromodels with the selected nodes are affected by interference is presented. Unlike the well-known IBIS models, that contain information on I/O buffers in the tables with counts of the current-voltage characteristics and time-dependency of the output voltage, the proposed macromodels are deprived of a number of shortcomings and limitations of these models. In particular, the possibility of using macromodels are not limited to solving specific computational problems related to the analysis of signals integrity. This paper shows how to use the proposed macromodels to refine the system parameters, describing the interference of power circuits and ground, for a wide range of devices and blocks. The results of the comparison in general the alternative embodiments of high-speed transceivers at the physical layer with the use of additional noise immunity criteria are also presented.

The structure of a 32-channel system of asynchronous data processing is considered. The data come from the detectors of nuclear physics experiments. Processing is provided for signals with a mean frequency of up to 10 MHz in each channel. The system provides generation of data packages, consisting of digital codes of signal amplitude, of signal superposition in peak detectors, of signal arrival time and number of channel wherein the event has occurred with a subsequent 8b10b coding. The considered system allows us to regulate dynamically the number of active channels. Two interface of data exchange – the slow I2C and high-speed (320 MHz), providing communication IC with the GBTX chip, have been built in the system. The results of developing the structural diagram and circuital-layout solutions of separate units are presented. System prototyping is implemented by the 180nm CMOS technology of UMC. The results of testing both separate blocks and the whole system are presented.

Problems of onboard space scientific devices control, collecting auxiliary service information about working capacity, conditions of experiment carrying out and preliminary data processing for real time calibration and stabilizing of operational parameters are actual for any space devices. In this paper we describe and discuss service data acquisition and onboard control for “GRIS-BD” unit in “GRIS” space experiment onboard ISS. This system provides temperature measurements in different equipment parts (in power supplies, on scintillation crystals for energy ranges correction, etc.), precision thresholds measurements in discrimination circuits, status different switching on/off (in real time), precision control detector parameters by high-voltage regulation, fine thresholds changing (analog regulation), different switching on/off (in real time), statistical analysis of data flows and change of operation modes of the device.

The implementation of the high voltage power supply control system (HVPSCS) for experimental setup FODS(FOcusing Doublearmed Spectrometer) at accelerator U-70 of the Federal state budgetary institution State Research Center Of Russia Institute for High Energy Physics of the National Research Centre "Kurchatov Institute" (hereinafter referred to as IHEP) or for the test bench of the detector components is considered. The required set of hardware is defined and the appropriate software to operate HVSCS is written in C/C++ codes. The data acquisition (DAQ) system makes automatic control on HVSCS for data taking run. It allows to get the dependence of appropriate detector parameters on the high voltage supply values and to choose its optimal values for FODS detectors. The test run results of the HVPSCS are presented.

It is well-known that there is a trade-off between performance and power consumption in onboard computers. The fault-tolerance is another important factor affecting performance, chip area and power consumption. Involving special SRAM cells and error-correcting codes is often too expensive with relation to the performance needed. We discuss the possibility of finding the optimal solutions for modern onboard computer for scientific apparatus focusing on multi-level cache memory design.

This work considers the technique for modeling of multiple errors caused by charged particles in sub-100 nm devices. This technique estimates the Soft Error Rate taking into account layout of integrated circuit. Comparison of simulated data with data from experiments on testing facilities is provided.

A structure of the analog amplitude shaper for high energy physics instrumentation is presented. The shaper has a function of self-adaption of the shaping time based on the channel occupancy. The spectrometer consists of the filter with maximized signal-to-noise ratio (slow shaper), high-frequency band-pass filter (fast shaper), amplitude and time discriminators, peak detector and signal overlap inspector. Based on the channel occupancy the output of either fast or slow shaper is supplied via the 2-channel multiplexer. At the highest occupancies the inspector fixes the overlap and the signal from the fast shaper is switched to the multiplexer output. In case of overlap absence one can use the output of the slow shaper with higher amplitude resolution. The estimation of the maximum channel hit rate and amplitude resolution and the structure approbation is considered in the paper.

The angular dependence of the cumulative particles production off nuclei near the kinematical boundary for multistep process is defined by characteristic polynomials in angular variables, describing spatial momenta of the particles in intermediate states [1, 2]. Physical argumentation, exploring the small phase space method, leads to the appearance of equations for these polynomials in $cos (\theta/N)$, where $\theta$ is the polar angle defining the momentum of final (cumulative) particle, the integer $N$ being the multiplicity of the process (the number of interactions). It is shown explicitly how these equations aappear, the recurrent relations between polynomials with different $N$ are obtained. Factorization properties of characteristic polynomials found in our previous work [3] are extended, and their connection with known in mathematics Chebyshev polynomials of 2-d kind [4, 5] is established. As a result, differential cross section of the cumulative particle production has characteristic behaviour $d\sigma \sim 1/ \sqrt {\pi - \theta}$ near the strictly backward direction ($\theta = \pi$, the backward focusing effect). Such behaviour takes place for any multiplicity of the interaction, beginning with $n=3$, elastic or inelastic (with resonance excitations in intermediate states) and can be called the nuclear glory phenomenon, or 'Buddha's light' of cumulative particles. 1. V.B. Kopeliovich. Sov.J.Nucl.Phys. 26 (1977) 87 [Yad.Fiz. 26 (1977) 168] 2. V.B. Kopeliovich. Phys. Rept. 139 (1986) 51 3. V.B.Kopeliovich, G.K.Matushko and I.K.Potashnikova J.Phys. G41 (2014) 125107; Vladimir Kopeliovich and Galina Matushko. 'Buddha's light' of cumulative particles. Nuclear Glory Phenomenon. Scholars Press, Saarbruecken, Germany. 2015. ISBN 978-3-639-76496-3. 4. Chebyshev polynomials. https://en.wikipedia.org/wiki/Chebyshevpolynomials 5. Mnogochleny Chebysheva. https://ru.wikipedia.org/wiki/Mnogochleny-Chebysheva