Observation of Terrestrial gamma-ray flashes in the RELEC space experiment on the <Emphasis Type="Italic">Vernov</Emphasis> satellite

The RELEС scientific payload of the Vernov satellite launched on July 8, 2014 includes the DRGE spectrometer of gamma-rays and electrons. This instrument comprises a set of scintillator phoswich-detectors, including four identical X-ray and gamma-ray detector with an energy range of 10 kev to 3 MeV with a total area of ~500 cm² directed to the atmosphere, as well as an electron spectrometer containing three mutually orthogonal detector units with a geometric factor of ~2 cm² sr. The aim of a space experiment with the DRGE instrument is the study of fast phenomena, in particular Terrestrial gamma-ray flashes (TGF) and magnetospheric electron precipitation. In this regard, the instrument provides the transmission of both monitoring data with a time resolution of 1 s, and data in the event-by-event mode, with a recording of the time of detection of each gamma quantum or electron to an accuracy of ~15 μs. This makes it possible to not only conduct a detailed analysis of the variability in the gamma-ray range, but also compare the time profiles with the results of measurements with other RELEC instruments (the detector of optical and ultraviolet flares, radio-frequency and low-frequency analyzers of electromagnetic field parameters), as well as with the data of ground-based facility for thunderstorm activity. This paper presents the first catalog of Terrestrial gamma-ray flashes. The criterion for selecting flashes required in order to detect no less than 5 hard quanta in 1 ms by at least two independent detectors. The TGFs included in the catalog have a typical duration of ~400 μs, during which 10–40 gamma-ray quanta were detected. The time profiles, spectral parameters, and geographic position, as well as a result of a comparison with the output data of other Vernov instruments, are presented for each of candidates. The candidate for Terrestrial gamma-ray flashes detected in the near-polar region over Antarctica is discussed.     

High-Precision Space Astrometry of Gamma-Ray Bursts: II. Relativistic Corrections in Converting the Time Scales

A technique for the determination of cosmic gamma-ray burst coordinates by measuring the time lag between gamma-ray burst signals on different spacecraft in the near-Sun orbits is developed. On the basis of the well-known relativistic time transformation between barycentric, geocentric, and instrumental coordinate frames of reference, the time corrections for specific spacecraft systems are calculated. Among various relativistic corrections, those are determined that are significant for the method in question.     

F－12芳纶纤维缠绕壳体水压实验AE检测及剩余强度预报

采用声发射仪，对Ｆ－１２芳纶纤维缠绕复合材料壳体水压实验过程进行了低压ＡＥ检测，选用设计爆破压强的４３％以下的ＡＥ数据，建立了一个低压下的ＡＥ参量与爆玻压力之间的多元线性回归方程式。该方程式对壳体爆破压力的预测值与实测值符合较好，从而为降低复合材料壳体水压安全评定实验压强提供了新途径。它既保证了经过水压实验后的复合材料壳体有足够的承载能力，又能可靠地预报其爆破压强。     

High-energy gamma radiation of solar flares as an indicator of acceleration of energetic protons

Using the SONG detector onboard the CORONAS-F satellite, gamma-ray emission of high energies (>100 MeV) was recorded during four solar flares. In the sequential spectra of gamma rays the peculiarity caused by generation and decay of neutral pions was isolated, which made it possible to determine with a high accuracy the moments of appearance in the solar atmosphere of protons accelerated up to energies above 300 MeV.     

Experiment on the <Emphasis Type="Italic">Vernov</Emphasis> satellite: Transient energetic processes in the Earth’s atmosphere and magnetosphere. Part I: Description of the experiment

The program of physical studies on the Vernov satellite launched on July 8, 2014 into a polar (640 × 830 km) solar-synchronous orbit with an inclination of 98.4° is presented. We described the complex of scientific equipment on this satellite in detail, including multidirectional gamma-ray detectors, electron spectrometers, red and ultra-violet detectors, and wave probes. The experiment on the Vernov satellite is mainly aimed at a comprehensive study of the processes of generation of transient phenomena in the optical and gamma-ray ranges in the Earth’s atmosphere (such as high-altitude breakdown on runaway relativistic electrons), the study of the action on the atmosphere of electrons precipitated from the radiation belts, and low- and high-frequency electromagnetic waves of both space and atmospheric origin.     

SIGMA: Projet d'Observatoire spatial a haute resolution angulaire pour les sources de rayons gamma

(SIGMA: Project of a high resolution space observatory for gamma rays sources)—The SIGMA space observatory is designed to obtain images of the sky in the hard X-ray/low energy gamma-ray domain (30–2000 keV range), with an angular accuracy of a few are min, within a field of ～7° × 7°, and a sensitivity for point sources down to a level of a few 10^?6 photons cm^?2s^?1keV^?1 (exposure 24 hr). The instrument is designed using the principle of the coded aperture mask telescope with a position sensitive detector derived from the Anger gamma-camera which is used in nuclear medicine. The pseudo-images of the sky are accumulated on board and transmitted to the ground stations for decoding processing. The gross weight of the instrument is 750 kg and its overall dimensions are 3 m long and 1.2 m in diameter.     

Superluminous supernovae: no threat from eta Carinae

Recently, Supernova 2006gy was noted as the most luminous ever recorded, with a total radiated energy of approximately 10(44) Joules. It was proposed that the progenitor may have been a massive evolved star similar to eta Carinae, which resides in our own Galaxy at a distance of about 2.3 kpc. eta Carinae appears ready to detonate. Although it is too distant to pose a serious threat as a normal supernova, and given that its rotation axis is unlikely to produce a gamma-ray burst oriented toward Earth, eta Carinae is about 30,000 times nearer than 2006gy, and we re-evaluate it as a potential superluminous supernova. We have found that, given the large ratio of emission in the optical to the X-ray, atmospheric effects are negligible. Ionization of the atmosphere and concomitant ozone depletion are unlikely to be important. Any cosmic ray effects should be spread out over approximately 10(4) y and similarly unlikely to produce any serious perturbation to the biosphere. We also discuss a new possible effect of supernovae-e-ndocrine disruption induced by blue light near the peak of the optical spectrum. This is a possibility for nearby supernovae at distances too large to be considered "dangerous" for other reasons. However, due to reddening and extinction by the interstellar medium, eta Carinae is unlikely to trigger such effects to any significant degree.     

航天器仪表与照明分系统设计和发展

航天器仪表与照明分系统承担着飞行器与航天员信息交互的任务,为航天员在轨工作、生活提供支持。分系统功能包括信息显示提示、越限报警提示、手动操作、工作生活照明、休闲娱乐等。文章给出了航天器仪表与照明分系统设计思路及分系统设计组成;分析了分系统技术应用情况;对应航天器设计和应用结果,提出了后续航天器的技术发展思路和设想。     

Experiment on the <Emphasis Type="Italic">Vernov</Emphasis> satellite: Transient energetic processes in the Earth’s atmosphere and magnetosphere. Part II. First results

We present the first experimental results on the observation of optical transients, gamma-ray bursts, relativistic electrons, and electromagnetic waves obtained during the experiment with the RELEC complex of scientific equipment on the Vernov satellite.     

Short increases of the fluxes of electrons with energies > 0.08 MeV at low-latitude (<Emphasis Type="Italic">L</Emphasis> < 2) regions of near-Earth space

We present the characteristics of short (duration less than 1 min) increases of the counting rate of electrons with energies >0.08 MeV observed in low-latitude (L < 2.0) regions of near-Earth space in the course of the GRIF experiment on the Spektr module of the Mir orbital station. The measurements were carried out using a set of instruments including X-ray and gamma-ray spectrometers, as well as detectors of electrons, protons, and nuclei with large and small geometrical factors, which allowed one to detect the fluxes of charged particles both in the region of the Earth’s radiation belts and in regions close to the geomagnetic equator. As a result of more than 1.5 years of observation, it is demonstrated that short increases in the intensity of electrons of subrelativistic energies are detected not only in the regions of the near-Earth space known as “precipitation zones” (1.7 < L < 2.5), but in high-latitude regions (up to the geomagnetic equator, L < 1.1) as well. Two types of increases of the electron counting rate are found: either fairly regular increases repeating on successive orbits or increases local in time. The latter type of increases can be caused by a short enhancement of electron flux on a given drift shell. The results of our measurements have shown that the duration of the detected increases in intensity can be rather short, as little as 20–30 s. Therefore, in the case of large amplitudes, such increases of the counting rate of electrons can imitate astrophysical events of the type of cosmic gamma-ray bursts in the detectors of hard X-ray and gamma radiation.     

A Search for Possible Mesolensing of Cosmic Gamma-Ray Bursts: II. Double and Triple Bursts in the BATSE Catalog

The paper is devoted to searching for a possible phenomenon of the gravitational lensing of cosmic gamma-ray bursts on celestial bodies of a globular cluster type (mesolensing). If this phenomenon takes place, gamma-ray bursts should have light curves with two or three similar components whose spectra are identical. These components are separated in time by a few seconds. Using a statistical method developed for comparing the components, we have found in the BATSE catalog 11 candidates of gamma-ray bursts with mesolensing for the entire time of operation of the Compton Gamma-Ray Observatory (1991–2000). Two of these 11 gamma-ray bursts have light curves with three components. The possibility of gravitational mesolensing of these gamma-ray bursts on the King's type bodies is investigated.     

Space experiments aboard the Lomonosov MSU satellite

At present, the Institute of Nuclear Physics of Moscow State University, in cooperation with other organizations, is preparing space experiments onboard the Lomonosov satellite. The main goal of this mission is to study extreme astrophysical phenomena such as cosmic gamma-ray bursts and ultra-high-energy cosmic rays. These phenomena are associated with the processes occurring in the early universe in very distant astrophysical objects, therefore, they can provide information on the first stages of the evolution of the universe. This paper considers the main characteristics of the scientific equipment aboard the Lomonosov satellite.     

Observations of auroral kilometric radio emission on the <Emphasis Type="Italic">Interball-1</Emphasis> satellite in the active Sun period 1999–2000

Results of almost two years (January 1999–October 2000) of continuous observations of auroral kilometric radio emission with the instrument AKR-X onboard the high-apogee satellite of the Earth Interball-1 are presented. The observations were conducted at the growth stage (in 1999) and in the maximum (2000) of solar activity within the 100–1500 kHz frequency band. The results of AKR detection in the vicinity of the maximum of its spectrum at a frequency of 252 kHz are presented. Both similarity (for example, the character of global directivity) and important differences from the AKR emission observed during the solar activity minimum [5] are found. Together with very high sporadicity, strong seasonal changes in the intensity are typical for the emission. It is completely absent in the spring-summer period in the Northern Hemisphere and is strongly suppressed in this period in the Southern Hemisphere. Probable nature of these features of AKR is discussed.     

Investigation of Long-Wave Radio Bursts from Interball-1 Satellite Observations

Long-wave radio bursts recorded on the Interball-1 satellite in the frequency band 100–1500 kHz are analyzed. The events distinguished by large amplitude radio emission fluxes were selected. These bursts were identified with powerful solar flares, during which time fluxes of hard X-ray radiation, meter-wave radio bursts (types II and IV), and coronal transients were observed. Temporal profiles of the bursts are characterized by a quick drift in frequency and are typical for bursts of III and SA types. The instant of long-wave radio burst generation seems to correspond to the expansion phase of a flare.     

Fast measurements of parameters of the Solar Wind using the BMSW instrument

Design of the plasma spectrometer BMSW (Fast Monitor of the Solar Wind, possessing high temporal resolution) is described in the paper, as well as its characteristics and modes of operation. Some examples of measurements of various properties of the solar wind, made with this instrument installed onboard the high-apogee satellite Spektr-R, are presented.     

The neutron,gamma-ray,X-ray spectrometer (NGXS): A compact instrument for making combined measurements of neutrons,gamma-rays,and X-rays

The Neutron, Gamma ray, and X-ray Spectrometer (NGXS) is a compact instrument designed to detect neutrons, gamma-rays, and hard X-rays. The original goal of NGXS was to detect and characterize neutrons, gamma-rays, and X-rays from the Sun as part of the Solar Probe Plus mission in order to provide direct insight into particle acceleration, magnetic reconnection, and cross-field transport processes that take place near the Sun. Based on high-energy neutron detections from prompt solar flares, it is estimated that the NGXS would detect neutrons from 15 to 24 impulsive flares. The NGXS sensitivity to 2.2 MeV gamma rays would enable a detection of ∼50–60 impulsive flares. The NGXS is estimated to measure ∼120 counts/s for a GOES C1-type flare at 0.1 AU, which allows for a large dynamic range to detect both small and large flares.     

贫氧推进剂声发射燃速仪的研制

通过研究贫氧推进剂的燃烧特性。主要是燃烧声信号的频带特性和不稳定特性，采用弱信号检测电路，并结合计算机技术，研制了用于贫氧推进剂燃速测试的新型声发射燃速仪。整机具有自动控制测试、计算各种燃速参数等功能。     

Observation of fast variations of the helium-ion abundance in the solar wind

This paper describes the results of studying the helium component of the solar-wind ion-flux measurement by the BMSW instrument on the Spektr-R satellite with a time resolution of 3 s. In contrast to most previous works that presented values averaged over large (hourly average or daily average) intervals, we have shown that the relative helium-ion abundance in the solar wind experiences considerable (by a few percent and even 10%) variations on such short intervals as 10 seconds or even several seconds.