Local disturbances of lightning and seismic origin in the radiation belt

The results from observing bursts of high-energy charged particle fluxes in near-Earth space, caused by local disturbances of the radiation belt and particles precipitating from it, in the ARINA (on board the RESURS-DKI satellite since 2006) and VSPLESK (on board the International Space Station since 2008) satellite experiments are presented. New features were revealed in the geographic distribution of particle bursts, indicating that most high-energy electron bursts are interrelated with thunderstorm and seismic activities, at that some bursts are observed in regions of tectonic faults. Results from observing high-energy electron precipitation from the radiation belt over Japan during the powerful seismic event that began on March 11, 2011, are analyzed.     

Observation of solar-magnetospheric and geophysical effects on the electron and proton fluxes detected by the satellite-borne ARINA instrument

New results are presented on the observations of bursts and variations in high-energy charged-particle fluxes in the near-Earth space by the ARINA instrument operated onboard the Resurs-DK1 satellite since 2006.     

GAMMA-400 Gamma-Ray Observations in the GeV and TeV Energy Range

Physics of Atomic Nuclei - The future space-based GAMMA-400 $$\gamma$$ -ray telescope will operate onboard the Russian astrophysical observatory in a highly elliptic orbit during 7 years. Observing...     

Precision Measurements of High-Energy Cosmic Gamma-Ray Emission with the GAMMA-400 Gamma-Ray Telescope

The GAMMA-400 γ-ray telescope installed at the Russian space observatory is intended for precision measurements in the energy range of 20 MeV–1000 GeV of γ-ray emission (with the angular and energy resolutions several times better than that of current γ-ray telescopes) from discrete sources; measurement of the energy spectra of Galactic and extragalactic diffuse γ-ray emission; studies of γ-ray emission from the active Sun; and measurements of fluxes of γ-ray emission and electron–positron cosmicray component, which are probably associated with the annihilation or decay of dark-matter particles.     

Antiphase boundary formation energies in L10 and L11 superstructures

We described an approach suitable for obtaining an analytical expression for the energy of an antiphase boundary in an ordered alloy in the hard sphere model using pair interatomic interaction potentials. Depending on the orientation of the antiphase boundary, the crystal is subdivided into two-dimensional monatomic packings parallel to the defect, and its energy is determined by the sum of the energies of the two-dimensional packings. The results of the calculations for antiphase boundaries of different orientations are given in the form of matrix expressions for each of the considered superstructures.Altai Polytechnical Institute. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 3, pp. 68–72, March, 1993.     

Stripping of fast oxygen ions colliding with atoms of light elements

Based on the available experimental data and the results of calculations carried out in this paper, cross sections are estimated for single-electron stripping of O ^Z+ (Z=1–7) ions with energies in the range E=0.5–200 MeV/u due to collisions with H, He, N, O, or Ar atoms. Analytical approximations of the cross sections are presented.     

Gammas and Charged Particles Identification in Lateral and Additional Apertures of GAMMA-400

Physics of Atomic Nuclei - The GAMMA-400 (Gamma Astronomical Multifunctional Modular Apparatus) will be a new generation satellite gamma-observatory. The gamma-ray telescope GAMMA-400 consists of...     

The Anticoincidence System of Space-Based Gamma-Ray Telescope GAMMA-400, Test Beam Studies of Anticoincidence Detector Prototype with SiPM Readout

Physics of Atomic Nuclei - The GAMMA-400 gamma-ray telescope is planned for the launch at the end of 2026 on the Navigator service platform designed by Lavochkin Association on an elliptical orbit...     

Array of scintillation detectors for the MONICA spectrometer

An array of scintillation detectors of the MONICA Spectrometer, whis is aimed at investigating fluxes of cosmic-ray ions (from H to Ni) in the extraterrestrial space within the energy range from 10 to 300 MeV per nucleon, is considered. The basic goal of the MONICA experiment is the measurement of the ionic and isotopic composition of cosmic rays of the galactic and solar origin, as well as the measurement of their energy spectrum. This problem was intensely studied by numerous investigators [1–10]; nevertheless, a lot of questions remain unsolved up to now, in this field of science. The array of scintillation detectors plays the important role in achieving the goals of the MONICA experiment. The composition of the array, tuning procedure, and characteristics of scintillation detectors are discussed in detail.     

Capabilities of the Gamma-400 Gamma-ray Telescope for Observation of Electrons and Positrons in the TeV Energy Range

The space-based GAMMA-400 gamma-ray telescope will measure the fluxes of gamma rays in the energy range from ∼20 MeV to several TeV and cosmic-ray electrons and positrons in the energy range from several GeV to several TeV to investigate the origin of gamma-ray sources, sources and propagation of the Galactic cosmic rays and signatures of dark matter. The instrument consists of an anticoincidence system, a converter-tracker (thickness one radiation length, 1 X₀), a time-of-flight system, an imaging calorimeter (2 X₀) with tracker, a top shower scintillator detector, an electromagnetic calorimeter from CsI(Tl) crystals (16 X₀) with four lateral scintillation detectors and a bottom shower scintillator detector. In this paper, the capability of the GAMMA-400 gamma-ray telescope for electron and positron measurements is analyzed. The bulk of cosmic rays are protons, whereas the contribution of the leptonic component to the total flux is ∼10⁻³ at high energy. The special methods for Monte Carlo simulations are proposed to distinguish electrons and positrons from proton background in the GAMMA-400 gamma-ray telescope. The contribution to the proton rejection from each detector system of the instrument is studied separately. The use of the combined information from all detectors allows us to reach a proton rejection of up to ∼1 × 10⁴.