The PAMELA experiment is a satellite-borne apparatus designed to study charged particles in the cosmic radiation with a particular focus on antiparticles. PAMELA is mounted on the Resurs DK1 ...satellite that was launched from the Baikonur cosmodrome on June 15th 2006. The PAMELA apparatus comprises a time-of-flight system, a magnetic spectrometer, a silicon–tungsten electromagnetic calorimeter, an anticoincidence system, a shower tail catcher scintillator and a neutron detector. The combination of these devices allows antiparticles to be reliably identified from a large background of other charged particles. This paper reviews the design, space qualification and on-ground performance of PAMELA. The in-orbit performance will be discussed in future publications.
We compare the quasi-biennial variations and Rieger-type variations (on a timescale of less than 1 year) in solar activity, interplanetary magnetic field, and galactic cosmic-ray flux modulation. We ...show that, in comparison with the 11-year cycle, the quasi-biennial variations are less suppressed in the interplanetary medium than on the Sun. Although the Rieger-type variations are adjacent in frequency to the quasi-biennial variations, they differ noticeably from them in the degree of reproduction in the interplanetary medium and the influence on the cosmic-ray modulation.
Since the International Geophysical Year (1957), the Lebedev Physical Institute performs the regular measurements of charged particle fluxes in the Earth's atmosphere (from the ground level up to ...30–35km) at several latitudes. The unique experimental data base obtained during 58 years of cosmic rays observations in the atmosphere allows to investigate temporal, spatial and energetic characteristics of galactic and solar cosmic rays as well as the role of charged particles in the atmospheric processes. Analysis of this data base also revealed a special class of numerous events caused by energetic electron precipitation recorded in the atmosphere at polar latitudes. In this paper we present Catalogue of electron precipitation events observed in the polar atmosphere during 1961–2014 and briefly outline the previous results of this data set analysis.
•Regular measurements of cosmic rays in the Earth's atmosphere (0–35km) since 1957.•A special class of events caused by energetic electron precipitation at polar latitudes is defined.•More than 550 events of precipitating electron events are recorded during 58 years of observations.•Characteristics of precipitating electron spectra are determined.•We present the Catalogue of electron precipitation events observed during 1961–2014.
The future space-based GAMMA-400 gamma-ray telescope will operate onboard the Russian astrophysical observatory in a highly elliptic orbit during 7 years to observe Galactic plane, Galactic Center, ...Fermi Bubbles, Crab, Vela, Cygnus X, Geminga, Sun, and other regions and measure gamma- and cosmic-ray fluxes. Observations will be performed in the point-source mode continuously for a long time (∼100 days). GAMMA-400 will measure gamma rays in the energy range from ∼ 20 MeV to several TeV and cosmic-ray electrons + positrons up to several tens TeV. GAMMA-400 instrument will have very good angle and energy resolutions, high separation efficiency of gamma rays from cosmic-ray background, as well as electrons + positrons from protons. The main feature of GAMMA-400 is the unprecedented angular resolution for energies > 30 GeV better than the space-based and ground-based gamma-ray telescopes by a factor of 5–10. GAMMA-400 observations will permit to resolve gamma rays from annihilation or decay of dark matter particles, identify many discrete sources, clarify the structure of extended sources, specify the data on cosmic-ray electron + positron spectra.
The future space-based GAMMA-400
-ray telescope will operate onboard the Russian astrophysical observatory in a highly elliptic orbit during 7 years. Observing
-ray sources from Galactic plane,
-ray ...bursts,
-ray diffuse emission,
rays from the Sun, and
rays from dark matter particles will be performed uninterruptedly for a long time (
100 days) in point-source mode in contrast to scanning mode for Fermi-LAT and other space- and ground-based instruments. GAMMA-400 will measure
rays in the energy range from
20 MeV to several TeV units, have the unprecedented angular (
at
GeV) and energy (
at
GeV) resolutions better than for Fermi-LAT, as well as ground-based
-ray facilities, by a factor of 5–10, and perfectly separate
rays from cosmic-ray background.
•The GAMMA-400 gamma-ray telescope performance for lateral aperture.•Detection of GRB from the lateral aperture in the energy range from ∼ 10 to ∼ 100 MeV.•The problem of connection between high- and ...low-energy gamma-ray emissions of GRBs.
The currently developing space-based gamma-ray telescope GAMMA-400 will measure the gamma-ray and electron + positron fluxes using the main top-down aperture in the energy range from ∼ 20 MeV to several TeV in a highly elliptic orbit (without shading the telescope by the Earth and outside the radiation belts) continuously for a long time. The instrument will provide fundamentally new data on discrete gamma-ray sources, gamma-ray bursts (GRBs), sources and propagation of Galactic cosmic rays and signatures of dark matter due to its unique angular and energy resolutions in the wide energy range. The gamma-ray telescope consists of the anticoincidence system (AC), the converter-tracker (C), the time-of-flight system (S1 and S2), the position-sensitive and electromagnetic calorimeters (CC1 and CC2), scintillation detectors (S3 and S4) located above and behind the CC2 calorimeter and lateral detectors (LD) located around the CC2 calorimeter.
In this paper, the capabilities of the GAMMA-400 gamma-ray telescope to measure fluxes of GRBs from lateral directions of CC2 are analyzed using Monte-Carlo simulations. The analysis is based on off-line second-level trigger construction using signals from S3, CC2, S4 and LD detectors. For checking the numerical algorithm the data from space-based GBM and LAT instruments of the Fermi experiment are used, namely, three long bursts: GRB 080916C, GRB 090902B, GRB 090926A and one short burst GRB 090510A. The obtained results allow us to conclude that from lateral directions the GAMMA-400 space-based gamma-ray telescope will reliably measure the spectra of bright GRBs in the energy range from ∼ 10 to ∼ 100 MeV with the on-axis effective area of about 0.13 m2 for each of the four sides of CC2 and total field of view of about 6 sr.
A new source type of galactic cosmic rays Sinitsyna, V.G.; Sinitsyna, V.Y.; Stozhkov, Yu. I.
Journal of physics. Conference series,
02/2020, Volume:
1468, Issue:
1
Journal Article
Peer reviewed
Open access
Experimental data of PAMELA and AMS-02 on proton and helium spectra at high and very high energies as well as the excess of 10 - 300 GeV positron flux cannot be explained using the diffusive models ...of propagation of cosmic-rays accelerated at the supernova shocks and require the existence of nearby sources of cosmic rays at the distances less than one kpc. We consider active dwarf stars as possible sources of galactic cosmic rays in the energy range up to ˜ 1014 eV. The generation of high-energy cosmic rays should be accompanied by high-energy γ-ray emission, which may be detected. Here we present the SHALON long-term observation data aimed to search for γ-ray emission above 800 GeV from the active red dwarf stars: V962 Tau, V780 Tau, V388 Cas, V1589 Cyg, GJ 1078 and GL 851.1. The TeV gamma-ray emission mostly of aring type from these sources was detected. This result confirms that active dwarf stars are also the sources of high-energy galactic cosmic rays.
The description and technical characteristics of the gamma-spectrometer installation for the detection of cosmic rays, as designed at the Dolgoprudny scientific station of the Lebedev Physical ...Institute in cooperation with the Mackenzie University (Sao Paulo, Brazil), are presented. This installation has operated continuously in the CASLEO astronomical complex since 2015. The detector modules of the setup are based on the NaJ (Tl) scintillator, which is 76.2 mm × 76.2 mm high, a Hamamatsu R1307 photomultiplier tube, a high voltage power supply, and a preamplifier. The technique of the experimental calibration of the spectrometer is also presented.
—
The Galactic Cosmic Rays (GCR) portable scientific instrument was developed in 2022 by the Dolgoprudny Scientific Station of the Lebedev Physical Institute for detecting the charged component of ...cosmic rays. Its description and performance characteristics are presented. STS-6 gas-discharge counters arranged in two layers with five counters in each are used as detecting elements. The layers of the upper and lower counters are separated by a 7-mm-thick aluminum filter. This instrument is intended for the TI3GER international experiment (Technological Innovation Into Iodine and GV Environmental Research), which is aimed at studying the effect of iodine oxides on the reduction of the ozone layer.
—
This paper presents a description of the new CARPET facility for detecting the charged component of cosmic rays, as well as its technical characteristics; it was designed and installed at the ...Dolgoprudny Scientific Station of the Lebedev Physical Institute (DNS of the Lebedev Physical Institute). The detecting base of the CARPET facility consists of STS-6 gas-discharge counters combined in 12 units with ten counters in each. The upper counter layer is separated from the lower counter layer by an aluminum filter with a thickness of 7 mm. The integration time of these counters is 1 ms. Continuous monitoring of meteorological data and data on the state of the supply voltage of the facility occur. The results of determining the barometric coefficient for the CARPET and analysis of the first experimental data are also presented.
PDF
