Table of contents

1. Preface

The 3rd International Conference on Particle Physics and Astrophysics (ICPPA-2017) was held in Moscow, Russia, from October 2 to 5, 2017. The conference is organized by the National Research Nuclear University "MEPhI". The aim of the Conference is to promote contacts between scientists and to develop new ideas in fundamental research. We bring together experts and young scientists working on experimental and theoretical aspects of particle physics on the Earth and in the Space and cosmology (figure 1). The conference covers a wide range of topics such as accelerator physics, (astro) particle physics, cosmic rays, cosmology and methods of experimental physics: detectors and instruments. These directions are unified by development of the Standard Model which is evidently not complete. There are deviations from the Standard Model: neutrino oscillations, the dark matter existence, which are main subjects of the Conference. Various aspects of Standard Model testing and search for new phenomena are main subjects of the conference. Among them: flavor physics (LHCb, Belle, BESIII and other experiments), precision multi-boson production measurements (ATLAS, CMS and other experiments), dark matter searches. Electroweak interaction was discussed in the talks given by participants of neutrino physics experiments (Borexino, Neutrino-4, SOX, T2K and others).

Lists of committees are available in this pdf.

All papers published in this volume of Journal of Physics: Conference Series have been peer reviewed through processes administered by the proceedings Editors. Reviews were conducted by expert referees to the professional and scientific standards expected of a proceedings journal published by IOP Publishing.

A brief overview of recent results from accelerator and reactor neutrino experiments and future prospects are presented. The experimental status of sterile neutrinos is also discussed.

The NA62 experiment at CERN collected a large sample of charged kaon decays in ight with a minimum bias trigger in 2007. Upper limits on the rate of the charged kaon decay into a muon and a heavy neutral lepton (HNL) obtained from this data are reported for a range of HNL masses. The NA62 experiment has collected further data in 2015 with a completely new and improved detector. New limits on heavy neutrinos from kaon decays into electron and HNL will be presented.

The third phase of the Borexino experiment that's referred to as SOX is devoted to test the hypothesis of the existence of one (or more) sterile neutrinos at a short baseline (~5–10m). The experimental measurement will be made with artificial sources namely with a ¹⁴⁴Ce–¹⁴⁴Pr antineutrino source at the first stage (CeSOX) and possibly with a ⁵¹Cr neutrino source at the second one. The fixed ¹⁴⁴Ce–¹⁴⁴Pr sample will be placed beneath the detector in a special pit and the initial activity will be about 100 – 150 kCi. The start of data taking is scheduled for April 2018. The article gives a short description of the preparation for the first stage and shows the expected sensitivity.

Low energy threshold reactor experiments have the potential to give insight into the light sterile neutrino signal provided by the reactor antineutrino anomaly and the gallium anomaly. In this work we analyze short baseline reactor experiments that detect by elastic neutrino electron scattering in the context of a light sterile neutrino signal. We also analyze the sensitivity of experimental proposals of coherent elastic neutrino nucleus scattering (CENNS) detectors in order to exclude or confirm the sterile neutrino signal with reactor antineutrinos.

The iDREAM (industrial Detector for reactor antineutrino monitoring) project is aimed at remote monitoring of the operating modes of the atomic reactor on nuclear power plant to ensure a technical support of IAEA non-proliferation safeguards. The detector is a scintillator spectrometer. The sensitive volume (target) is filled with a liquid organic scintillator based on linear alkylbenzene where reactor antineutrinos will be detected via inverse beta-decay reaction. We present first results of laboratory tests after physical launch. The detector was deployed at sea level without background shielding. The number of calibrations with radioactive sources was conducted. All data were obtained by means of a slow control system which was put into operation.

The results of the research in the field of neutrino physics obtained at Kalinin nuclear power plant during 15 years are presented. The investigations were performed in two directions. The first one includes GEMMA I and GEMMA II experiments for the search of the neutrino magnetic moment, where the best result in the world on the value of the upper limit of this quantity was obtained. The second direction is tied with the measurements by a solid scintillator detector DANSS designed for remote on-line diagnostics of nuclear reactor parameters and search for short range neutrino oscillations. DANSS is now installed at the Kalinin Nuclear Power Plant under the 4-th unit on a movable platform. Measurements of the antineutrino flux demonstrated that the detector is capable to reflect the reactor thermal power with an accuracy of about 1.5% in one day. Investigations of the neutrino flux and their energy spectrum at different distances allowed to study a large fraction of a sterile neutrino parameter space indicated by recent experiments and perform the reanalysis of the reactor neutrino fluxes. Status of the short range oscillation experiment is presented together with some preliminary results based on about 170 days of active data taking during the first year of operation.

The transition and survival probabilities for the different light neutrinos are calculated and displayed with account of the contributions of heavy neutrinos. It is shown that in the case of the mixing matrix of a definite type the explanation of the neutrino anomalies at short distances is possible. A new parametrization and a certain form of the mixing matrix for light and heavy neutrinos are used with allowance for the possible violation of CP invariance.

The high-energy conventional atmospheric neutrino fluxes are calculated with the hadronic interaction models: Kimel & Mokhov, QGSJET II-03(04), SIBYL 2.1(2.3), EPOS LHC. The influence of hadron-nuclear interactions on the neutrino flux ratios, $v/\bar{v},({v}_{\mu }+{\bar{v}}_{\mu })/({v}_{e}+{\bar{v}}_{e})$, is studied. A comparison of calculations obtained with use of two different approaches, ${\mathscr{Z}}(E,h)$ -functions method and the Matrix Cascade Equations (MCEQ), demonstrates close agreement in whole but some of partial contrubutions. The comparison of calculated muon neutrino spectra with the latest experimental data justifies reliability of performed computation which describes correctly the atmospheric neutrino production. The calculation made with the model EPOS LHC, combined with Hillas & Gaisser parametrization of the cosmic ray spectrum, is in close agreement with the best fit of IceCube for energy spetrum of atmospheric muon neutrinos in the energy range 1–500 TeV.

A high statistics data sample of the K⁺ → μ⁺ν_μ decay was recorded in 2012 by the OKA collaboration. The missing mass analysis was performed to search for a decay channel K⁺ → μ⁺ν_H with a stable heavy neutrino in the final state. The obtained missing mass spectrum did not reveal statistically significant peaks corresponding to stable heavy neutrinos in the mass range (220 < m_νH < 375) MeV/c². Instead, we update upper limits on the branching ratio and on the value of the mixing element |U_μH|².

The main goal of experiment "Neutrino-4" is to search for the oscillation of reactor antineutrino to a sterile state. Experiment is conducted on SM-3 research reactor (Dimitrovgrad, Russia). Data collection with full-scale detector with liquid scintillator volume of 3m³ was started in June 2016. We present the results of measurements of reactor antineutrino flux dependence on the distance in range 6– 12 meters from the center of the reactor. At that distance range, the fit of experimental dependence has good agreement with the law 1/L². Which means, at achieved during the data collecting accuracy level oscillations to sterile state are not observed. In addition, the spectrum of prompt signals of neutrino-like events at different distances have been presented.

The Hydride Earth model predictions of geoneutrino flux and intrinsic Earth heat flux are discussed. The geoneutrino flux predicted by the model can be adjusted to the experimental one. The predicted intrinsic Earth heat flux is significantly larger than model dependent experimental value obtained under assumption that the main heat transfer mechanism is a thermal conductivity. We introduce an additional mechanism of heat transfer in the Earth's crust, namely the energy transfer by hot gases produced in the Earth crust at great depths. The experimental data supporting this idea, in particular the temperature profiles measured in the Kola super deep borehole, are discussed.

We calculate beta spectrum of Ce-Pr-144 taking into account several types of corrections. The result is compared with the experimental data obtained at NRC Kurchatov Institute. Using this comparison we estimate the reliability of theoretical calculations for electron and antineutrino spectra from beta decay.

The compact 2.45 MeV fast neutron generator with a reduced supply voltage for calibration of low-background neutrino and dark matter detectors was tested. The generator is based on an array of carbon nanotubes. Neutron generation is carried out by applying a high voltage in the range of +10 to + 25 kV to a nanotube array, which cause an ionization of deuterium molecules with the following acceleration of ions in the direction of the grounded target covered by a deuterated polyethylene film. The d(d,n)³He nuclear reaction happens as the result of ions collisions with the target. The dependences of the neutron yield as functions of the applied voltage were obtained for two different types of carbon nanotubes array. It is shown that the type of nanotubes array does not influence significantly on the neutron yield.

In 2008, the PAMELA magnetic spectrometer has discovered unpredicted abundance of the ratio of the galactic positron flux to the total positron and electron flux at high energies. It does not agree with the cosmic-ray fluxes calculated using the GALPROP code. This abundance was called the "PAMELA anomalous effect" and one of the explanations of this effect was the appearance of the additional electron and positron flux due to annihilation or decay of the dark matter particles. Later the precision PAMELA results were confirmed by the Fermi-LAT gamma-ray telescope and the AMS-02 magnetic spectrometer. Currently, the new GAMMA-400 project is being developed. The one of its main goals is to search for signatures of dark matter particles, which produce gamma rays. The GAMMA-400 gamma-ray telescope will have unprecedented angular and energy resolutions. PAMELA and GAMMA-400 are the instruments with the best characteristics for their time, which will improve our understanding of the nature of dark matter. At present, the problem of the nature of dark matter still remains the main challenge in high-energy astrophysics.

The DArk Matter Particle Explorer (DAMPE) is a space mission within the strategic framework of the Chinese Academy of Sciences, resulting from a collaboration of Chinese, Italian, and Swiss institutions, and is a new addition to the growing number of particle detectors in space. It was successfully launched in December 2015 and has commenced nominal science operations since shortly after launch. Lending technologies from its predecessors such as AMS and Fermi-LAT, it features a powerful segmented electromagnetic calorimeter which thanks to its 31 radiation lengths enables the study of charged cosmic rays in the energy domain of up to 100 TeV and gamma rays of up to 10 TeV. The calorimeter is complemented with a silicon-tungsten tracker converter which yields a comparable angular resolution as current space-borne pair-conversion gamma-ray detectors. In addition, the detector features a top anti-coincidence shield made of segmented silicon plastic scintillators and a boron-doped plastic scintillator on the bottom of the instrument to detect delayed neutrons arising from cosmic ray protons showering in the calorimeter. An overview of the mission and a summary of the latest results in the domain of charged cosmic rays, gamma rays and heavy ions will be presented.

The Large Area Telescope (LAT) onboard the Fermi satellite is a pair-conversion telescope for high-energy gamma rays of astrophysical origin. Although it was designed to be a high-sensitivity gamma-ray telescope, the LAT has proved to be an excellent electron/positron detector. It has been operating in low Earth orbit since June 2008 and has collected more than 16 million cosmic-ray electron and positron (CRE) events in its first seven years of operation. The huge data sample collected by the LAT enables a precise measurement of the CRE energy spectrum up to the TeV region. A search for anisotropies in the arrival directions of CREs was also performed. The upper limits on the dipole anisotropy probe the presence of nearby young and middle-aged CRE sources.

The recent results of the very precise measurements of the primary cosmic protons and helium nuclei energy spectra by AMS-02 and some rather accurate estimates of these energy spectra generated in SNR allow us to elaborate the new approximation of the pimary nucleon energy spectra. As the acuracy of this approximation is rather high we can use it to test various models of hadronic interactions with the help of atmospheric muon energy spectra. The atmospheric vertical muon energy spectra have been calcullated in terms of the EPOS LHC, QGSJET01, QGSJETII-03 and QGSJETII-04 models in the energy range 10² ÷ 10⁵ GeV with help of the CORSIKA package and this new approximation of the primary nucleon spectrum. The comparison of calculations with the muon spectra observed by collaborations L3+Cosmic, LVD and MACRO has shown that all models predict approximately two times lower intensity of the muon energy spectra. As these muons are products of decays of the most energetic π^± and K^± mesons in the atmosphere, we can conclude that production of these π^± and K^± mesons is underestimated by EPOS LHC, QGSJET01, QGSJETII-03 and QGSJETII-04 models.

A search for resonant absorption of the solar axion by ⁸³Kr nuclei was performed using the proportional counter installed inside the low-background setup at the Baksan Neutrino Observatory. The obtained model independent upper limit on the combination of isoscalar and isovector axion-nucleon couplings |g₃ − g₀| ≤ 8.4 × 10⁻⁷ allowed us to set the new upper limit on the hadronic axion mass of m_A ≤ 65 eV (95% C.L.) with the generally accepted values S=0.5 and z=0.56.

An approach to calculate the flux of cosmicgenic muons detected by Muon Monitor experiment in lab LAB2400 of the Underground Laboratory in Canfranc (LSC) is described. The measuring apparatus consists of three layers of SC16 scintillation matrix detectors. The hardware function of the detector assembly was determined using computer simulation. Obtained value of the total muon ux turned out to be equal to (4.35 ± 0.2) × 10⁻³m⁻²s⁻¹.

The models of self-interacting dark matter (DM) are popular now, in particular dark matter with Coulomb-like interaction. It leads to enhancement of annihilation in Galaxy what helps to explain cosmic ray puzzles, e.g. positron anomaly. Though such models get constraints from cosmic microwave background (CMB), large scale structure. The constrained region of model parameters can be essentially enlarged if to take into account possibility of much stronger enhanced annihilation of dark matter particles due to their recombination accounted for by a classical dipole radiation. The given constraints are considered for dark disk model with self-interaction.

When seen in gamma rays, the Moon appears brighter than the Sun. Gamma rays emitted by the Moon mostly originate from the decays of neutral pions produced by the interactions of cosmic rays with the lunar surface. Using the data collected by the Fermi Large Area Telescope (LAT) in its first seven years of operation, we measured the gamma-ray emission spectrum of the Moon in the energy range from 30MeV up to a few GeV and we studied its time evolution, finding a correlation with the solar activity. We also developed a full Monte Carlo simulation based on the FLUKA code, which describes the production of gamma rays in the cosmic-ray interactions with the Moon. We used the simulation results to infer the cosmic-ray proton and helium spectra near the Earth from the lunar gamma-ray data.

At present an experiment for measuring the flux of cosmic diffuse gamma rays with energy higher than 100 TeV (experiment "Carpet-3") is being prepared at the Baksan Neutrino Observatory of the Institute for Nuclear Research, Russian Academy of Sciences. The preparation of the experiment implies considerable enlargement of the area of both muon detector and surface part of the shower array. At the moment the plastic scintillation counters with a total continuous area of 410 m² are installed in the muon detector (MD) underground tunnels, and they are totally equipped with electronics. Adjusting of the counters and their electronic circuits is in progress. Six modules of shower detectors (out of twenty planned to be installed) have already been placed on the surface of the MD absorber. A new liquid scintillation detector is developed for modules of the ground –surface part of the array, whose characteristics are presented. It is shown that the "Carpet-3" air shower array will have the best sensitivity to the flux of primary gamma rays with energies in the range 100TeV – 1PeV, being quite competitive in gamma-ray astronomy at such energies.

We discuss ultra-high energy cosmic rays from minor sources and their possible contribution to the extragalactic diffuse gamma-ray emission. As an illustration of minor sources we consider the possible specific type of active galactic nuclei in which supermassive black hole is surrounded by a super strong magnetic field of 10¹⁰-10¹¹ Gs. In this model we have calculated cosmic ray energy spectra at the Earth and intensity of cascade quanta produced by cosmic rays in extragalactic space. Proceeding from numerical results and the data by Pierre Auger Observatory and Telescope Array it is shown that these active galactic nuclei make a negligible contribution to the cosmic ray flux at the Earth. However cosmic rays from these active galactic nuclei produce significant gamma-ray flux as compared to extragalactic diffuse gamma-ray emission measured by Fermi LAT. We conclude that ultra-high energy cosmic rays from minor sources contribute noticeably to extragalactic diffuse gamma-ray emission.

A search for dark matter particle candidates produced in association with a Z boson in proton-proton collisions at the total center-of-mass energy of 13 TeV is presented. The search uses 36.1 inverse femtobarn of data collected by the ATLAS experiment at the Large Hadron Collider in 2015 and 2016. Events with large missing transverse momentum and consistent with the decay of a Z boson into oppositely charged electron or muon pairs were selected in the analysis. Background estimates and corresponding systematic uncertainties are shown. Exclusion limits on the dark matter candidate and mediator masses are reported.

The TOTEM collaboration at the LHC has measured the elastic, inelastic and total proton-proton cross sections at several center of mass energies and is carrying on a rich program of measurements of diffractive physics together with the CMS collaboration. The talk will review the TOTEM measurements mainly focusing on the newest and most significant ones. The status of the experimental apparatus, its latest changes and the current and future technological challenges will be discussed as well.

We present the results for multi-quark exotic states search from D0 Collaboration at the FNAL Tevatron. This includes an evidence for a ${B}_{s}^{0}{\pi }^{\pm }$ state (X(5568)) with hadronic decays of B_s meson, a confirmation of the X(5568) state with semileptonic decays of B_s meson, and a search for exotic baryons decaying to J/ψΛ pairs.

Results of study of the K⁺ → π⁰e⁺ν_eγ decay at OKA setup are presented. 13118 events of this decay have been observed. The branching ratio with cuts ${E}_{\gamma }^{* }\gt 10\,{\rm{MeV}},0.6\lt {cos}{\Theta }_{e\gamma }^{* }\lt 0.9$ , is calculated $R=\frac{Br({K}^{+}\to {\pi }^{0}{e}^{+}{v}_{e}\gamma )}{Br({K}^{+}\to {\pi }^{0}{e}^{+}{v}_{e})}=(0.59\pm 0.02(stat.)\pm 0.03(syst.))\times {10}^{-2}$. For the asymmetry A_ξ we get A_ξ = −0.019±0.020(stat.)±0.027(syst.)

Separation of electroweak component from strong component of associated Z_γ production on hadron colliders is a very challenging task due to identical final states of such processes. The only difference is the origin of two leading jets in these two processes. Rectangular cuts on jet kinematic variables from ATLAS/CMS 8 TeV Z_γ experimental analyses were improved using machine learning techniques. New selection variables were also tested. The expected significance of separation for LHC experiments conditions at the second datataking period (Run2) and 120 fb⁻¹ amount of data reaches more than 5σ. Future experimental observation of electroweak Z_γ production can also lead to the observation physics beyond Standard Model.

The top quark is the heaviest known fundamental particle. As it is the only quark that decays before it hadronizes, it allows us to probe the properties of bare quarks at the Large Hadron Collider. Highlights of a few recent precision measurements by the ATLAS Collaboration of the top quark using 13 TeV and 8 TeV collision data will be presented: top-quark pair and single top production cross sections including differential distributions will be presented alongside measurements of top-quark properties, including results using boosted top quarks, probe our understanding of top-quark production in the TeV regime. Measurements of the top-quark mass and searches for rare top quark decays are also presented.

After the Higgs boson discovery at the LHC, a lot of additional measurements should be performed to understand in details the properties of the observed particle. These measurements include cross sections measurements, couplings measurements, studies of the interaction vertex structures etc. One of the most perspective subjects to study is the kinematics of the production jets, associated with the Higgs boson. It is demonstrated, that the kinematic correlations of such jets can be used to distinguish different production channels of Higgs boson: gluon-gluon fusion (ggF) and vector boson fusion (VBF). Such separation plays an important role because possible beyond the Standard Model contributions in ggF and VBF channels lead to different effects, which should be taken into account in searches for BSM physics.

The NA48/2 experiment presents a final result of the charged kaon semileptonic decays form factors measurement based on 4.28 million $K_{e3}^{\pm }$ and 2.91 million $K_{{\mu}3}^{\pm }$ selected decays collected in 2004. The result is competetive with other measurements in $K_{{\mu}3}^{\pm }$ mode and has a smallest uncertainty for $K_{e3}^{\pm }$, that leads to the most precise combined $K_{l3}^{\pm }$ result and allows to reduce the form factor uncertainty of |V_US|. The NA48/2 experiment at CERN collected a very large sample of charged kaon decays into multiple final states. From this data sample we have reconstructed about 1663 events of the very rare decay K^± → μ^±νe⁺e⁻ over almost negligible background in the region with m(e⁺e⁻) above 140 MeV, which is of great interest in Chiral Perturbation Theory. We present the m_ee spectrum and a model-independent measurement of the decay rate for this region.

We study a model described by a single real scalar field in the two-dimensional space-time. The model is specified by a potential which is non-polynomial and supports analytical kink-like solutions that are similar to the standard kink-like solutions that appear in the φ⁴ model when it develops spontaneous symmetry breaking. We investigate the kink-antikink scattering problem in the non-polynomial model numerically and highlight some specific features, which are not present in the standard case.

We have calculated the masses of different states of bottomonia in the framework of potential non-relativistic QCD, non-perturbatively. The potential consists of two terms, a static term incorporating Coulombic plus confinement part along with a constant and a relativistic correction term classified in powers of the inverse of heavy quark mass O(1/m). Spin-spin interaction has been considered to calculate the masses of the singlet and the triplet states of bottomonia. The Schrödinger equation is solved numerically to obtain the masses from 1S to 6S states, the calculated masses for η_b(1S) is 9.390 GeV and for ϒ(1S) is 9.459 GeV and is found to be in good accordance with the experimental results.

We give a retrospective overview of the conceptual content of the strong interaction scattering at high energies with account of the latest experimental findings made at the LHC.

Ω_ccc, Ω_bbb, Ω_bcc and Ω_ccb baryons are considerable theoretical interest in a baryonic analogue of heavy quarkonium because of the color-singlet bound state of three heavy quark (c,b) combination inside. Regge trajectories are concerned with the mass spectrum of the particles so that the present study exhibits the regge trajectories obtained from excited states of four experimentally unknown triply heavy Ω baryons. The trajectories are plotted in (n, M²) and (J, M²) planes which are helpful to determine the unknown quantum number and J^P values. The calculations have computed in Hypercentral Constituent Quark Model with hyper coulomb plus linear potential.

Spectroscopic parameters of heavy-light flavoured D meson are obtained within the framework of phenomenological quark-antiquark potential (Coulomb plus linear confinement) model using the Gaussian wave function. We incorporated ${\mathcal{O}}$(1/m) corrections to the potential energy term and relativistic corrections to the kinetic energy term of the hamiltonian. We obtain the radiative (electric and magnetic) transitions and the mixing parameters of the DâĹŠ${\bar{D}}$ oscillation. The results are compared with various experimental measurement as well as other theoretical predictions.

The Galactic Center (Sgr A*) is a peculiar place in our Galaxy (Milky Way). Our Solar system is located at a distance around 8 kpc from the Galactic Center (GC). There were a number of different including exotic ones such as boson stars, fermion balls, neutrino balls, a cluster of neutron stars. Some of these models are significantly constrained with consequent observations and now supermassive black hole with mass around 4 × 10⁶M_⊙ is the preferable model for GC. Moreover, one can test alternative theories of gravity with observations of bright stars near the Galactic Center and and observations of bright structures near the black hole at the Galactic Center to reconstruct shadow structure around the black hole with current and future observational VLBI facilities such as the Event Horizon Telescope. In particular, we got a graviton mass constraint which is comparable and consistent with constraints obtained recently by the LIGO-Virgo collaboration.

We present a simple cosmological model where the quantum tunneling of a scalar field rearranges the energetics of the matter sector, sending a stable static ancestor vacuum with positive spatial curvature into an inating solution with positive curvature. This serves as a proof of principle that an observation of positive spatial curvature does not falsify the hypothesis that our current observer patch originated from false vacuum tunneling in a string or field theoretic landscape. This poster submission is a summary of the work, and was presented at the 3rd annual ICPPA held in Moscow from October 2 to 5, 2017, by Prof. Rostislav Konoplich on behalf of the author.

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 modified Lane-Emden equations are derived for the special ansatz for the anisotropy parameter Δ in the form of the differential relation between Δ and the metric function ν. The analytical solutions of the obtained equations are found for incompressible fluid stars. The dynamical stability of incompressible anisotropic fluid stars against radial oscillations is studied.

A model describing the formation of protogalaxies is developed. Compact supermassive clusters of primordial black holes assumed to act as a nuclei for the galaxy formation. The mechanism of PBH formation based on a collapse of massive walls of scalar field due to second order phase transition. Mass spectra of PBH are obtained analytically and shown possibility of the formation of PBH clusters with a total mass of ∼ 10⁵ – 10⁸M_⊙, having a size of ∼ 10 parsec, in an amount of ∼ 10¹¹, which corresponds to observational data on the value of galaxies on the visible Universe. The primary fractal structure of galaxies is naturally explained through the mechanism. Proposed approach is the cornerstone for a principally new scenario of the galaxy formation in the early Universe.

One important result from recent large integral field spectrograph (IFS) surveys is that the intrinsic velocity dispersion of galaxies increases with redshift. Massive, rotationdominated discs are already in place at z ∼ 2, but they are dynamically hotter than spiral galaxies in the local Universe. Although several plausible mechanisms for this elevated velocity dispersion (e.g. star formation feedback, elevated gas supply, or more frequent galaxy interactions) have been proposed, the fundamental driver of the velocity dispersion enhancement at high redshift remains unclear. We investigate the origin of this kinematic evolution using a suite of cosmological simulations from the FIRE (Feedback In Realistic Environments) project. These simulations reproduce the observed trends between intrinsic velocity dispersion (σ_intr), SFR, and z. In both the observed and simulated galaxies, σ_intr is positively correlated with SFR. σ_intr increases with redshift out to z ∼ 1 and then flattens beyond that. In the FIRE simulations, σ_intr can vary significantly on timescales of ≲ 100 Myr. These variations closely mirror the time evolution of the SFR and gas inflow rate ( _gas). By cross-correlating pairs of σ_intrgas, and SFR, we show that the increased gas inflow leads to subsequent enhanced star formation, and enhancements in σ_intr tend to temporally coincide with increases in _gas and SFR.

We study the evolution of magnetic fields in turbulent hot plasma of the early Universe accounting for the chiral magnetic effect. The magnetohydrodynamic turbulence is modeled by replacing the matter velocity in the advection term in the Faraday equation with the Lorentz force. The system of the kinetic equations for the spectra of the densities of the magnetic helicity and the magnetic energy, as well as for the chiral imbalance, is derived. The amplification of the magnetic field is shown to result from the presence of the chiral magnetic effect solely. The system of the kinetic equations is solved numerically in primordial plasma after the electroweak phase transition. The inuence of the matter turbulence on the magnetic field evolution is examined for different seed magnetic fields.

In the present talk, we consider the existence of the two degenerate universal vacua: a) the first Electroweak vacuum at v = 246 GeV - "true vacuum", and b) the second Planck scale "false vacuum" at v₂ ∼ 10¹⁸ GeV. In these vacua, we investigated the different topological defects. The main aim of this paper is an investigation of the hedgehog's configurations as defects of the false vacuum. In the framework of the f(R) gravity, suggested by authors in their Gravi-Weak Unification model, we obtained a black hole solution, which corresponds to a "hedgehog" - global monopole, "swallowed" by a black-hole with mass ∼ 10¹⁹ GeV. These black-holes form a lattice-like structure of the vacuum at the Planck scale. Considering the results of the hedgehog lattice theory in the framework of the SU(2) Yang-Mills gauge-invariant theory with hedgehogs in the Wilson loops, we have used the critical value of temperature for the hedgehog's confinement phase. This result gave us the possibility to conclude that there exist triplet Higgs fields which can contribute to the SM at the energy scale ≃ 10⁴ ∼ 10⁵ GeV. Showing a new physics at the scale 10÷100 TeV, these triplet Higgs particles can provide the stability of the EW-vacuum of the SM.

The Event Horizon Telescope team intends by the 2020 to resolve the shadow of supermassive black hole SgrA* in the Galactic Center. It would be the first attempt for direct identification of the enigmatic black hole. In other words, it would be the first experimental verification of the General Relativity in the strong field limit. There is a chance to find a star moving on the relativistic orbit close to this black hole. We present the animated numerical model of the gravitational lensing of a star (or any other lighting probe), moving around rotating Kerr black hole in the Galactic Center and viewed by the distant observer.

The high temperature (high energy) limit of the Standard Model is developed with the help of contractions its gauge groups. The elementary particles evolution in the early Universe from Plank time up to several milliseconds is deduced from this limit theory. Particle properties at the infinite temperature look very unusual: all particles are massless, only neutral Z-bosons, u-quarks, neutrinos and photons are survived in this limit. The weak interactions become long-range and are mediated by neutral currents, quarks have only one color degree of freedom.

We study formation and evolution of solitons within a model with two real scalar fields with the potential having a saddle point. The set of these configurations can be split into disjoint equivalence classes. We give a simple expression for the winding number of an arbitrary closed loop in the field space and discuss the evolution scenarios that change the winding number. These non-trivial field configurations lead to formation of the domain walls in the three-dimensional physical space.

A topological geon is the quotient manifold M/Z₂ where M is a static spherically symmetric wormhole having the reflection symmetry with respect to its throat. We distinguish such asymptotically at solutions of the Einstein equations according to the form of the time-time metric function by using the quadrature formulas of the so-called inverse problem for self-gravitating spherically symmetric scalar fields. We distinguish three types of geon spacetimes and illustrate them by simple examples. We also study possible observational effects associated with bounded geodesic motion near topological geons.

The non-standard Reichenbach's synchronization is necessary for the coincidence of the numerical values of the integrals of the conserved quantities in two different inertial frames of reference, thereby ensuring an integral covariant formulation of the laws of conservation of physical quantities. The inclined axes of time in Minkowski's space have a physical meaning of time with non-standard clock synchronization according to Reichenbach.

In recent years, developments of gaseous detectors based on a combination of electron multiplication gap in the gas and pixel readout chips as a part of the anode plane (GasPixel detectors) reached a level where they can offer unique opportunities for particle detection. Transition radiation (TR) detectors based on this technology can be one of the possible applications. In this work, measurements of energy spectra and angular distributions of transition radiation photons produced by particles with different gamma factors made with a GridPix detector prototype are presented. The observed results are compared with theoretical predictions.

The SHiP experiment is designed to search for very weakly interacting particles beyond the Standard Model which are produced in a 400 GeV/c proton beam dump at the CERN SPS. The critical challenge for this experiment is to keep the Standard Model background level negligible. In the beam dump, around 10¹¹ muons will be produced per second. The muon rate in the spectrometer has to be reduced by at least four orders of magnitude to avoid muoninduced backgrounds. It is demonstrated that new improved active muon shield may be used to magnetically deflect the muons out of the acceptance of the spectrometer.

In the Endcap regions, CMS Muon spectrometer is using Cathode Strip Chambers (CSCs) as muon tracking and trigger detectors, also Resistive Plate Chambers (RPCs) serve as dedicated trigger detectors and improve the muon reconstruction by providing the excellent timing resolution for identification of muon particles. At the present, the four Endcap discs are not fully equipped: RPCs are covering only Endcap disks up to |ŋ| = 1.8. During the Long Shutdown 3 (from 2023 to 2026) of the Large Hadron Collider, Endcap stations 3 and 4 will be further instrumented with new improved RPCs (iRPCs) that will be covering the pseudorapidly region 1.8 < |ŋ| < 2.4, increasing the redundancy in this region. Nowadays, the final design of RPC chambers has been developed and the RPC double gap prototypes with a gas thickness 1.4mm are being tested. The performance and stability of iRPCs at the future HL-LHC upgrades have been studied (detection efficiency, cluster size, rate capability) at the Gamma-Irradiation Facility (GIF++) at CERN, where high energy charged particle beams (mainly muons) are combined with gammas from a 14 TBq 137Cesium source which simulates the background expected at the CMS experiments. In this paper, the main results obtained during the test at GIF ++ are presented.

The upgrades of the LHC planned in the next years will increase the instantaneous luminosity up to 5 × 10³⁴cm⁻²s⁻¹ after Long Shutdown 3, a value about five times higher than the nominal one for which the CMS experiment was designed. The resulting larger rate of interactions will produce a higher pileup environment that will challenge the trigger system of the CMS experiment in its original configuration, in particular in the endcap region. As part of the upgrade program of the CMS muon endcaps, additional muon detectors based on Gas Electron Multiplier (GEM) technology will be installed, in order to be able to sustain a physics program during high-luminosity operation without performance losses. The installation of the GE1/1 station is scheduled for Long Shutdown 2 in 2019–2020; already a demonstrator composed of five superchambers has been installed during the Extended Year-End Technical Stop at the beginning of 2017. Its goal is to test the system's operational conditions and also to demonstrate the integration of the GE1/1 chambers into the CMS online system. The status of the installation and commissioning of the GE1/1 demonstrator is presented.

Measurements of hadron production in the TeV energy range are one of the tasks of the future studies at the Large Hadron Collider (LHC). The main goal of these experiments is a study of the fundamental QCD processes at this energy range, which is very important not only for probing of the Standard Model but also for ultrahigh-energy cosmic particle physics. One of the key elements of these experiments measurements are hadron identification. The only detector technology which has a potential ability to separate hadrons in this energy range is Transition Radiation Detector (TRD) technology. TRD prototype based on straw proportional chambers combined with a specially assembled radiator has been tested at the CERN SPS accelerator beam. The test beam results and comparison with detailed Monte Carlo simulations are presented here.

The influence of a sampling rate of ADC on the efficiency of the pulse shape discrimination procedure (PSDP) developed for gamma-neutron discrimination was studied. Pu-Be neutron source and two types of digitizers (CAEN DT5730 and CAEN DT5743) were used. Both digitizers together with application software allow to store sequences of waveforms from a scintillation detector. The functional features of the CAEN DT5730 and CAEN DT5743 are described, and experimental characteristics of their operation are compared. Experimental values of an efficiency of neutron/gamma signal discrimination using two ADCs with different sampling frequencies are presented.

DANSS is a highly segmented plastic scintillator detector, which uses scintillator strips with a Gd-loaded reflective cover to detect reactor antineutrino by inverse beta-decay. Light is collected with wave length shifting fibers (3 per strip) placed in grooves. Therefore the distribution of light output could be significantly non-uniform. Transverse profile of light output was studied in ITEP at a test bench consisting of proportional chambers and scintillator strips. Tracks of cosmic particles, which crossed chambers, were reconstructed with high accuracy, whereby transverse profiles of light output were built with step 1 mm for six scintillator strips. This result is important for calibration of DANSS and the method could be useful in constructing similar detectors.

Here we present the specifications of the newly developed beta-spectrometer based on thick full absorption Si(Li) detector. The spectrometer was designed for precision measurements of various beta-spectra, namely for the beta-spectrum shape study of ¹⁴⁴Pr, which is considered to be one of the most promising anti-neutrino source for sterile neutrino searches.

In the presented work, we investigated several digital methods of a discrimination signals from fast neutrons and gamma quanta. The experimental setup consists of a Pu-Be neutron source, a scintillation detector with an organic para-terphenyl monocrystal, and a digitizer (CAEN DT5730, 500 MS/s). Mixed waveform sequences were stored and then separated by pulse shape. Four methods were used for signals separation. Comparison of the traditional and the new methods of Figure of Merit (FOM) calculation is given. FOM = 1.5 was obtained in our setup for the minimum threshold value. A scintillation detector with a para-terphenyl crystal was used to measure neutron yield in the neutron generator with carbon nanotubes.

Preliminary results of measurements of the total reaction cross sections σ_R and neutron removal cross section σ_-xn for weakly bound ⁶He, ⁸Li, ⁹Be and ¹⁰Be nuclei at energy range (20-35) A MeV with ²⁸Si target is presented. The secondary beams of light nuclei were produced by bombardment of the ²²Ne (35 A MeV) primary beam on Be target and separated by COMBAS fragment-separator. In dispersive focal plane a horizontal slit defined the momentum acceptance as 1% and a wedge degrader of 200 μm Al was installed. The Bρ of the second section of the fragment-separator was adjusted for measurements in energy range (20-35) A MeV. Two-neutron removal cross sections for ⁶He and ¹⁰Be and one –neutron removal cross sections ⁸Li and ⁹Be were measured.

We study the scattering of the φ⁸ kinks with power-law asymptotics. We found two critical values of the initial velocity, ${v}_{{\rm{cr}}}^{(1)}$ and ${v}_{{\rm{cr}}}^{(2)}$, which separate different regimes of the kink-antikink collision. At the initial velocities ${v}_{{\rm{in}}}\lt {v}_{{\rm{cr}}}^{(1)}$ kinks can not collide due to repulsive force between them. At ${v}_{{\rm{in}}}\gt {v}_{{\rm{cr}}}^{(2)}$ the kinks escape to spatial infinities after one collision. In the range ${v}_{{\rm{cr}}}^{(1)}\le {v}_{{\rm{in}}}\le {v}_{{\rm{cr}}}^{(2)}$ we observed kinks capture and formation of their bound state. Besides that, at these initial velocities we found resonance phenomena — escape windows.