The main goal of the Vernov mission is the study of magnetospheric relativistic electron precipitation and its possible influence on the upper atmosphere as well as the observation of Transient ...Luminous Events (TLE) and Terrestrial Gamma Flashes (TGF) across a broad range of the electromagnetic spectrum.
The RELEC (Relativistic Electrons) instrument complex onboard the Vernov spacecraft includes two identical X- and gamma-ray detectors of high temporal resolution and sensitivity (DRGE-1 and DRGE-2), three axis position detectors for high-energy electrons and protons (DRGE-3), a UV TLE imager (MTEL), a UV detector (DUV), a low frequency analyser (LFA), a radio frequency analyser (RFA), and AN electronics module responsible for control and data collection (BE).
The RELEC mission conducts the following experiments:
–simultaneous observations of high-energy electron and proton fluxes (within the energy range of ∼0.1–10.0MeV) and low-frequency (∼0.1–10kHz) electromagnetic wave field intensity variations with high temporal resolution (∼1ms);–fine time structure (∼1μs) measurements of transient atmospheric events in UV, X- and gamma rays with an optical imaging capability with a resolution of ∼1km in wide field of view (FOV);–measurements of electron flux pitch-angle distributions in dynamical ranges from ∼0.1 up to 105 part/cm2/s;–monitoring of charged and neutral background particles in different areas of near-Earth space.
The Ionosphere missions are the part of Ionosond-2025 space project, which main scientific objectives are monitoring of physical processes in the Earth upper atmosphere, ionosphere and magnetosphere, ...as well as of solar activity. Within the framework of the Ionozond-2025 project, it is planned to launch four spacecraft Ionosphere and one satellite Zond. The Zond satellite is planned to be launched in 2025. The main task of Zond mission is patrol of solar activity. The launch of the first pair of spacecraft is planned in early 2022, the second pair - late 2022 or early 2023. In case of successful implementation of the program of experiments on the Ionosphere satellites, control of the physical parameters of electromagnetic fields and corpuscular radiation in the near-Earth space will be provided, new information will be obtained on the geophysical processes occurring in the magnetosphere, ionosphere and upper atmosphere in their connection with solar activity.
The complex geoecological works carried out in the St. Anna Trough resulted in the detailed investigation of the water-sediment barrier zone. The physicomechanical properties such as the moisture, ...the moisture at the flowing boundary, the sedimentation rates, and the strength of the sediments measured and calculated for the upper 10-cm-thick layer of the bottom sediments were used as the main parameters characterizing the barrier zone. These data served as a basis for developing the model of the barrier zone with defining the lithogenesis stages: protosyngenesis—syngenesis—protodiagenegis—early diagenesis. The quantitative estimates of the environmental physicochemical properties presented in this work characterize each of these stages.
We developed an X-ray detector using 36 arrays, each consisting of a 64-pixellated yttrium oxyorthosilicate (YSO) scintillation crystal and a 64-channel multi-anode photomultiplier tube. The X-ray ...detector was designed to detect X-rays with energies lower than 10 keV, primarily with the aim of localizing gamma-ray bursts (GRBs). YSO crystals have no intrinsic background, which is advantageous for increasing low-energy sensitivity. The fabricated detector was integrated into UBAT, the payload of the Ultra-Fast Flash Observatory (UFFO)/Lomonosov for GRB observation. The UFFO was successfully operated in space in a low-Earth orbit. In this paper, we present the responses of the X-ray detector of the UBAT engineering model identical to the flight model, using 241Am and 55Fe radioactive sources and an Amptek X-ray tube. We found that the X-ray detector can measure energies lower than 5 keV. As such, we expect YSO crystals to be good candidates for the X-ray detector materials for future GRB missions.
Solar hard X-ray and gamma-ray emission was measured by BDRG instrument, the part of set of instruments operated on board the Russian satellite Lomonosov from April 2016 until now (solar-synchronous ...orbit with altitude 490 km, inclination of 97.6 degrees). Lomonosov measurements (11 flares with the X-ray energy more than 10 keV, and more than half of them have class in soft X-rays less than C2) were compared to the data obtained by RHESSI and Fermi space observatories as well as the Nobeyama Radioheliograph operating at the same time. The quasi-periodicity with different periods were found in some of them.
The new space project of M. V. Lomonosov Moscow State University on elaboration of multiple satellites for real time monitoring in the near-Earth space of radiation environment, natural (asteroids, ...meteoroids) and artificial (space debris) potentially dangerous objects, electromagnetic transients, such as cosmic gamma ray bursts, terrestrial gamma ray flashes, optical and ultraviolet bursts in the Earth atmosphere is presented. It is intended to install on the satellites the following instruments for space monitoring of dangerous objects and hazards: spectrometers of electrons and protons, complex of instruments for study of transient electromagnetic phenomena including gamma ray spectrometer, detectors of ultraviolet and optical emission and wide-field optical cameras. Successful implementation of the project for the first time in the world allows realization of a space system prototype for monitoring and preventing of space hazards for both ongoing and planned space missions, and also for aircraft flying in the upper atmosphere. There are also discussed results of experiments on-board Lomonosov in view of good experience of wide field camera use for monitor observations in space. These results formed the base of scientific program for the new project Universat- SOCRAT.
Astron.Astrophys. 399 (2003) L39-L42 The possibilities of observing some nonlinear electrodynamic effects, which
can be manifested in hard emission of X-ray, gamma ray pulsars and magnetars by
X-ray ...and gamma ray astronomy methods are discussed. The angular resolution and
sensitivity of modern space observatories give the opportunity to study the
nonlinear electrodynamic effects, which can occur in very strong magnetic
fields of pulsars ($B\sim 10^{12}$ G) and magnetars ($B\sim 10^{15}$ G). Such
magnetic field magnitudes are comparable with the typical value of magnetic
field induction necessary for manifestation of electrodynamics non-linearity in
vacuum. Thus, near a magneticneutron star the electromagnetic emission should
undergo nonlinear electrodynamic effects in strong magnetic fields (such as
bending of rays, fluxes dispersing, changing of spectra and polarization
states). Manifestations of these effects in detected hard emission from
magnetic neutron stars are discussed on the base of nonlinear generalizations
of the Maxwell equation in vacuum. The dispersion equations for electromagnetic
waves propagating in the magnetic dipole field were obtained in the framework
of these theories.The possibility of observing the bending of a ray and gamma
ray flux dispersing in the neutron star magnetic field are analyzed. The only
nonlinear electrodynamicseffect, which can be measured principally, is the
effect of gamma ray flux dispersion by the neutron star magnetic field.
Studying this effect we can also obtain information on the nonlinear
electrodynamics bending of a ray in the source. The main qualitative difference
in predictions of different nonlinear electrodynamics theories are discussed.
The possibilities of observing some nonlinear electrodynamic effects, which can be manifested in hard emission of X-ray, gamma ray pulsars and magnetars by X-ray and gamma ray astronomy methods are ...discussed. The angular resolution and sensitivity of modern space observatories give the opportunity to study the nonlinear electrodynamic effects, which can occur in very strong magnetic fields of pulsars (\(B\sim 10^{12}\) G) and magnetars (\(B\sim 10^{15}\) G). Such magnetic field magnitudes are comparable with the typical value of magnetic field induction necessary for manifestation of electrodynamics non-linearity in vacuum. Thus, near a magneticneutron star the electromagnetic emission should undergo nonlinear electrodynamic effects in strong magnetic fields (such as bending of rays, fluxes dispersing, changing of spectra and polarization states). Manifestations of these effects in detected hard emission from magnetic neutron stars are discussed on the base of nonlinear generalizations of the Maxwell equation in vacuum. The dispersion equations for electromagnetic waves propagating in the magnetic dipole field were obtained in the framework of these theories.The possibility of observing the bending of a ray and gamma ray flux dispersing in the neutron star magnetic field are analyzed. The only nonlinear electrodynamicseffect, which can be measured principally, is the effect of gamma ray flux dispersion by the neutron star magnetic field. Studying this effect we can also obtain information on the nonlinear electrodynamics bending of a ray in the source. The main qualitative difference in predictions of different nonlinear electrodynamics theories are discussed.
Dokl.Akad.Nauk.Ser.Fiz.380:435,2001 It was shown that according to the non-linear electrodynamics of vacuum
electromagnetic rays should bend in the field of magnetic dipole. The angles of
ray bending ...in the gravitational and magnetic fields of pulsars and magnetars
were obtained. In the case of pulsars with $b\sim R\sim $ 100 km, $B_0\sim
10^{13} G$ the value of the angle of non-linear electrodynamic bending of a ray
in the Heisenberg-Euler theory will reach the value of $\delta \psi_{NED}\sim
30'',$ and in the case of a magnetar with $B_0\sim 10^{15} G$ the angle $\delta
\psi_{NED}$ will increase to $\delta \psi_{NED}\sim 1 rad\sim 60^\circ .$ The
angle of gravitational bending of a ray at neutron star with $r_g$ = 3 km in
the same conditions will be equal to $\delta \psi_g\sim 0.06$ rad $\sim 4^\circ
>.$ Observations can only be made in X- rays and gamma-rays, for which the
agnetosphere is quite opaque. Because the distance from the Earth to the
well-known pulsars and magnetars is too large to observe the pure effect of a
ray bending. The non-linear electrodynamic bending of a ray as well as the
gravitational bending will be revealed in the effect of lensing.
It was shown that according to the non-linear electrodynamics of vacuum electromagnetic rays should bend in the field of magnetic dipole. The angles of ray bending in the gravitational and magnetic ...fields of pulsars and magnetars were obtained. In the case of pulsars with \(b\sim R\sim \) 100 km, \(B_0\sim 10^{13} G\) the value of the angle of non-linear electrodynamic bending of a ray in the Heisenberg-Euler theory will reach the value of \(\delta \psi_{NED}\sim 30'',\) and in the case of a magnetar with \(B_0\sim 10^{15} G\) the angle \(\delta \psi_{NED}\) will increase to \(\delta \psi_{NED}\sim 1 rad\sim 60^\circ .\) The angle of gravitational bending of a ray at neutron star with \(r_g\) = 3 km in the same conditions will be equal to \(\delta \psi_g\sim 0.06\) rad \(\sim 4^\circ >.\) Observations can only be made in X- rays and gamma-rays, for which the agnetosphere is quite opaque. Because the distance from the Earth to the well-known pulsars and magnetars is too large to observe the pure effect of a ray bending. The non-linear electrodynamic bending of a ray as well as the gravitational bending will be revealed in the effect of lensing.
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