Annotation of the results obtained in 2019
I. Instruments of the Project During the report period, we carried out work on the development and functional tests of the prototypes of three instruments for measuring and monitoring space plasma and corpuscular radiation of the Sun: (a) PICA Plasma Ion Compact Analyzer, (b) ECOS Electron Compact Spectrometer, (c) TSEP Telescope for Solar Energetic Particles. I.a. PICA Plasma Ion Compact Analyzer The laboratory prototype was manufactured and passed functional tests, analytical characteristics of the created laboratory prototype were determined. The manufactured prototype includes: a compact velocity filter (Wien filter), an electrostatic cylindrical analyzer, a detector based on a channel electron multiplier (ВЭУ-6) equipped with an electronics board with a charge-sensitive amplifier. The tests showed that the energy resolution of the device is 10%, the mass resolution of the device M / ΔM depends on the recorded particle energy and varies from 10 for 500 eV to 3.5 for 5000 eV. The manufactured prototype has dimensions 93x93x51 mm and weight of 365g. The tests showed the feasibility and operability of the proposed electron-optical circuit. The manufactured prototype of the device has the necessary characteristics to register protons and alpha particles of the solar wind with sufficient resolution. The obtained characteristics can be improved by using an electrostatic analyzer with a narrower energy resolution ΔЕ / Е. I.b. ECOS Еlectron COmpact Spectrometer The laboratory prototype of the electron spectrometer prototype was assembled from parts manufactured according to the previously developed models, its detector passed a series of tests, the instrument properties were adjusted and functional tests were carried out to establish the main analytical characteristics of the laboratory prototype. Verification of the functioning of the position-sensitive detector of the prototype showed that the manufactured detector allows you to resolve ~ 10 lines in each of the measurements. The energy resolution of the manufactured laboratory prototype of the device was ~ 30%, which corresponds to the computer model of the device. The range of simultaneously recorded energies ranged from Eo to 4.5Eo, where Eo is the minimum energy of particles recorded by the detector of the device at given potentials in optics. These results also correspond to the parameters obtained by computer simulation. The analysis of experimental data showed that the characteristics achieved on the manufactured prototype make it possible to analyze the electron flux with the accuracy necessary to fit instruments main purpose. At the same time, the analytical characteristics of the device can be improved by increasing the accuracy of manufacturing parts of the energy analyzer. I.c. TSEP Telescope of Solar Energetic Particles During the report period, the prototype of the Telescope of Solar Energetic Particles was assembled and its functioning was tested using laboratory electronics. The tests were based on registration of cosmic ray muons and analysis of measurement results. Two measurement techniques were developed: differential (single particle count) and integral (signal accumulation for a certain time interval) modes. The differential mode offers two possibilities: 1) determination of the full waveform of the signal, 2) determination of the pulse width of the signal. Application of the developed methods to the analysis of the obtained data demonstrated the correct functioning of the manufactured prototype. The prototype can measure protons and electrons in ~10-100 and ~1-10 MeV energy ranges respectively. It is shown that the relative accuracy of determination of particle energy in the differential mode is 5%, in the integral 7%. Preliminary analysis shows that the accuracy of determining the energy of particles while registering protons and electrons simultaneously should not be lower than 10%, which meets the initial requirements for the prototype. New electronic boards for the prototype were developed, manufactured and proved correct registration of signals from scintillation detectors of the telescope during tests. The electronic boards included a set of silicon photomultipliers (SiPMs) connected to charge-sensitive amplifiers, and a system of charge-sensitive amplifiers with comparators to amplify the signal from SiPM and to digitize and determine the pulse duration using laboratory ADCs and digital input devices. Laboratory tests of electronic circuit boards have shown their operability and the possibility of application as part of the device under development. In addition, the development of dimensional drawings of the TSEP was carried out in a possible compact design, including its own electronics package. Based on these drawings, it was concluded that it is possible to manufacture a compact device weighing up to 800 g with dimensions of 93.4x85.0x84.0 mm. Such mass-dimensional characteristics allow the further accomodation of the flight model of the instrument on micro- and nanosatellites, including the Cubesat platform. II. Research part During the report period, a number of research works were carried out and the following new scientific results were obtained in studying flare-active regions of the Sun: II.a. We continued a detailed study of the solar flare on March 15, 2015 (see Sharykin et al., ApJ, 2018, 2020) to determine the possible causes of suppression of eruption and the absence of coronal mass ejection (CME) A technique has been developed for identifying magnetic flux ropes (MFRs) in the solar flare region based on extrapolation of the magnetic field to the corona in the nonlinear force-free approximation using 135-second HMI/SDO vector photospheric magnetograms. The technique is based on the construction and analysis of maps of the magnetic twist function and 3D visualization of magnetic field lines and areas of increased electric current. The calculated maps on the photosphere made it possible to identify 6 regions of increased twist (> 1.5), which were able to be associated with three MFRs. The dependence of average twist on time at the foot of each MFR was studied. The 3D reconstruction of the magnetic field lines determined the height of the MFRs. It was found that long (>1 h) before the flare, the heights of all three MFRs did not exceed 12 Mm above the photosphere. About half an hour before the start of the flare impulsive phase, one of the MFRs increased its height to 21 Mm, which was accompanied by the appearance of a “hot channel” in EUV AIA/SDO images above the magnetic polarity inversion line (PIL) in the pre-impulsive phase of the flare. After the flare, the lengths of the MFRs only slightly changed relative to the original ones (7, 9 and 16 Mm), which indicates the absence of eruption. As was shown in the works by (Sharykin et al., 2018, 2020, ApJ) carried out in the previous stages of the Project, the interaction of two of these MFRs above the PIL through the tether-cutting magnetic reconnection (TCMR) initiated a flare energy release process. Based on the extrapolation of the magnetic field in the potential approximation, the decay index (nd) of the horizontal field component in the entire region was calculated for all moments of the flare with a time step of 135 s. Based on the analysis of the decay index, we came to the conclusion that the torus instability of the MFRs did not occur, since all the time the MFRs were below the surface nd=1.3, while the most optimistic estimates show that the critical decay index for the development of instability should exceed 1.35. II.b. Investigation of the density distributions of photospheric vertical electric currents in the flare-active regions of the Sun studied previously in (Zimovets et al., 2020, ApJ) We performed an analysis of the probability density function (PDF) of the absolute value of the density of photospheric vertical electric currents, PVECs, (| jr |) in 48 active regions from 2010 to 2015, studied at the previous stage of the Project (Zimovets et al., ApJ, 2020), at time before and after the flares. Calculation of | jr | performed by applying the differential form of the magnetic field circulation theorem (Ampere's law) to the photospheric vector magnetograms of the HMI/SDO instrument. It is shown that for all studied active regions, PDF (| jz |), to a first approximation, can be approximated by a model consisting of a folded normal distribution in the region of low values (| jr | < 9000 statampere / cm2) and a decreasing power-law function at higher values. Using the least squares method, the model parameters are obtained, histograms of their distribution are constructed, mathematical expectations and standard deviations are calculated for all events. No systematic changes in model parameters during the flare were detected. An explicit connection between the parameters and the flare class, as well as with the Hale magnetic class, was not found within the framework of the approach used for the considered limited sample of flares and active regions. Arguments are presented in favor of the assumption that the folded normal distribution in the low-value region represents noise in the data, while the power-law “tail” may reflect the nature of the current generation processes in the active regions of the Sun.

 

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Annotation of the results obtained in 2017
I. Works and results on the development of solar wind ion analyzer: The physical concept of a solar wind ion analyzer was developed as a computer model. We conducted a series of the computer model tests to check its performance and properties such as energy range and resolution, transmission at different energies, mass separation. The results of these tests indicate that actual measurement properties match the target properties. Energy range is 500 to 10000 eV, energy resolution dE/E~5% (target 10%), availability to measure separately protons, alphas, and O+6 oxygen. The model is capable of measurements of higher masses with higher analyzer voltage that is not provided for current model but can become possible after a slight construction reworking if necessary. Based on the initial data of the computer model, a design model of the laboratory model of the ion analyzer was created. The laboratory model is the physical equivalent of the instrument, conducting the same measurement, consisting of the same principal elements, but laboratory power supplies will be used to supply potentials, and laboratory facilities will also be used for data processing. The layout assumes the use of accessible and simple elements that do not require special treatment or special precision of manufacturing. It is proposed to use magnets from the NdFeB alloy available on the market, as well as the serial channel multiplier VEU-6M as a detector. The use of ready-made solutions will significantly simplify the development of the entire device as a whole, as well as reduce the time and cost of manufacturing. The layout provides the possibility of dismantling separate analysis elements for their checks or additional tests outside the composition of the layout. The layout will be equipped with additional apertures to select the optimum sensitivity ratios and energy resolution. The preliminary estimate of the mass of the model is about 400 g. and will be specified at the manufacturing stage. The preliminary dimensions of the layout are 130x79x50.5 mm on the protruding parts and will also be specified at the manufacturing stage. On the design model was issued a complete set of design documentation, ready for transfer to production for the manufacture of parts and assembly of the layout. As part of the work on the preliminary design of electronics boards, assembly drawings of the board for the detector of the model based on the VEU-6M have been issued. The board is made in a miniature design, which will save the compact size of the layout. The board electronics are based on affordable and inexpensive elements of the Industrial category, which allows to reduce the cost and shorten the production time. A part of the materials was purchased to start the production of the model, namely, AMg6 alloy was purchased to make the case and a number of components of the mock-up components, and polyacetal was purchased for manufacturing the insulator parts required in the device, since the device's physical analysis scheme involves high voltage operation. In addition, preliminary tests of the functioning of the measurement scheme were carried out. From the available elements, similar to those designed after the modifications, an equivalent circuit was built, powered with laboratory sources. The scheme was first tested in a vacuum chamber on ions of different masses with an energy of 1 keV. The tests were carried out with residual gas, helium, nitrogen, carbon dioxide and with argon injected under the control of the Extorr laboratory mass spectrometer. The assembled scheme allowed to determine each of the types of gas and showed full efficiency and the prospect of further work on miniaturization and the creation of a compact laboratory model on the issued documentation. Based on the results of the work, an article by Shestakov A.Yu., Moiseenko D.A., Vaisberg O.L., Zhuravlev R.N., Shuvalov S.D., Zimovets I.V. “Modeling a miniature solar wind ion analyzer for future space missions” was prepared and submitted to the editorial board of Advances in Space Research. II. Works and results on the development of of solar wind electron analyzer: To analyze the parameters of solar wind electrons, the design of a compact and light device was developed, its electronic-optical scheme is based on electrostatic analysis of charged particles. The electron spectrometer being developed allows detecting particles in the energy range from 30 to 10,000 eV and will allow fast analysis of energy distribution of electron flux due to the large area of the entrance window and the possibility of simultaneous registration of a wide range of energies. Estimated resolution ΔE/E ≤ 13%, depending on the energy and angle of arrival of the particle. Measurements of electron fluxes conducted by the instrument over a wide energy range will provide important information for analyzing the dynamics of solar flares, corotating fluxes, particle acceleration on interplanetary shocks, and a variety of other phenomena in the solar wind. The work on the development of a computer model of the instrument and the design model of its laboratory prototype was conducted in accordance with the principles of miniaturization of the entire product and minimization of the structural mass, while maintaining the necessary stiffness and screening properties of key nodes In the process of development of a compact spectrometer for solar wind electrons analysis, a computer model of the instrument was developed, its operational properties were modeled, key parameters were determined: energy range, resolution ΔE / E, fields of view, requirements for the design model of the laboratory prototype of the device. Based on these requirements, a design model of a laboratory instrument was created, an estimate of the weight and consumption of the device being created. The estimated parameters of the electron spectrometer: - The field of view in azimuth angle is ± 26 °; - The field of view in polar angle is ± 10 °; - Resolution ΔE / E ≤ 15%; - Weight less than 1 kg; - Consumption less than 5 watts. The performed simulations show that the claimed characteristics are achievable, this allows us to proceed with the manufacture of the analyzer mock-up. Also, the work carried out confirms that the device concept will allow to analyze solar wind fluxes for solving solar activity and space weather monitoring problems. III. Works and results on the development of the telescope of energetic particles: The concept of a compact lightweight sectional scintillation telescope for detecting solar energetic particles has been developed. Works on modeling (in Geant4) of the detector part of the telescope have been performed and estimates of its sensitivity for various particles in different energy ranges have been made. Preliminary results show that with a mass of up to 1 kg and compact dimensions up to 40 mm x 40 mm x 70 mm (without taking into account the electronics block), the telescope allows measurement of the energy spectrum of protons in the range from 5 to 100 MeV and electrons from 1 to 10 MeV with energy resolution of 1% to 5%. An important advantage of the telescope is the ability to work both in the counting mode of individual particles and in the integral mode, when individual particles are not registered, but an analysis of the total spatial (along the telescope axis) energy loss spectrum is carried out. Integral mode allows to work at high counting rates and limited telemetry rate capabilities, while ensuring a fairly good (about 5%) accuracy of restoring the original spectrum and the composition of energetic particles. IV. Works and results on the determination of additional criteria for the realization of sporadic phenomena in the active regions of the Sun (flares, CMEs) based on the systematic study of the characteristics of the magnetic field and electric currents in the photosphere and its dynamics using HMI/SDO observational data: IV.1. Statistical study of the relation between vertical electric currents on the photosphere and flare hard X-ray sources: Based on the systematic analysis of 47 flares (from C3.0 to X3.1) observed in the central part of the solar disk in 2010-2016, using the data of the RHESSI and HMI/SDO space instruments, it has been established that at least one hard X-ray (HXR; >50 keV) source in each flare is in the vicinity of a region of strong vertical electric currents, which has the form of a ribbon (79% of cases) or an island (21% of cases). The ribbons differ from the islands by the presence of elongation along some direction (usually along the magnetic polarity inversion line - PIL). Integral vertical currents in such sources have values in the range 10-10000 GA, and current density in the range 0.01-1.0 A/m^2. There is no significant correlation between the intensity of the the HXR sources and the density of the vertical current below them. By comparing the post-flare and preflare vertical currents, no evidence has been found for a significant dissipation of the currents in the regions corresponding to the HXR sources. In some cases, amplification of vertical currents during and/or after the flare is detected. The results show that, on the whole, there is a connection between flare chromospheric HXR sources and vertical currents in the photosphere, namely, HXR sources tend to be located on the periphery of regions of strong vertical currents. The presence of such currents in the active region can be used as an additional criterion for predicting flares accompanied by electron acceleration and generation of HXRs. However, our results do not support the concept of electron acceleration by a longitudinal electric field, which might be generated directly at the foot of current-carrying loops due to some instabilities, since there is no significant correlation between the intensity of the HXR sources and the density of the vertical currents below them, as would be expected within the framework of such a concept. IV.2. A detailed study of the energy release and acceleration of electrons in the vicinity of the magnetic polarity inversion line (PIL) of the solar flare: On the base of a detailed analysis of multiwavelength observations of a solar flare of the moderate X-ray class (M1.2, March 15, 2015) by the ground and space telescopes we established that the effective acceleration of electrons with the most hard spectrum occurred during the flare period accompanied by the formation of super-hot plasma with temperature up to 40 MK. It is found that the population of accelerated electrons was inside a thin (up to 0.5 Mm) elongated along the PIL (up to 10 Mm) twisted magnetic structure with a very high field up to 1.2 kG. The plasma beta in this structure was less than 0.01, in spite of the super-high plasma temperature in it. The concentration of accelerated electrons was about 10^9 cm^-3, which is much lower than the concentration of the surrounding super-hot plasma. The energy flux density of the accelerated electrons reached the value 2x10^12 erg/cm^2/s. This is much more than in the available radiation hydrodynamics models currently used in the physics of flares. Consequently, this result shows that it is necessary to expand the capabilities of these models to account for such high energy densities of nonthermal electrons. In general, the results of this work indicate the need for the development of three-dimensional models of flare energy release in the vicinity of the PIL, taking into account the strong longitudinal component of the magnetic field, filamentation and the fine spatial structure of the energy release region, the formation of populations of accelerated electrons with very high energy density and heating the plasma to the super-hot temperatures. Based on the results of the work, an article by Sharykin I.N., Zimovets I.V., Myshyakov I.I., Meshalkina N.S. "Flare Energy Release in the Magnetic Field Polarity Inversion Line During M1.2 Solar Flare of March 15, 2015. Paper I. Onset of Plasma Heating and Electrons Acceleration" (https://arxiv.org/abs/1805.05792) was prepared and submitted to the editorial board of the Astrophysical Journal. IV.3. Estimation of the total number and energy of accelerated electrons in a giant solar flare: An estimate of the total number and energy of nonthermal electrons in a giant >X17 solar flare on October 28, 2003 is made by spectral analysis of the hard X-ray radiation measured by the high-energy neutron detector (HEND) onboard the Mars Odyssey spacecraft. As a result of the investigation, it is found that, depending on the model used and the low energy cutoff of the spectrum of nonthermal electrons, the value of its total energy can vary from 1.6x10^32 to 5.7x10^33 ergs. The lower estimate is obtained for the thick target model and at a fixed low energy cutoff of 46 keV. This estimate is comparable within the factor 2 with the estimate obtained by the RHESSI measurements. In this case, around 40% of the total energy of nonthermal electrons of the entire flare was released in the flare impulsive peak missed by RHESSI. Our upper estimate roughly corresponds to the estimate obtained earlier for another giant solar flare on November 4, 2003, which occurred in the same active region. This estimate seems to be overestimated, since it exceeds the estimate of the free magnetic energy (2.9x10^33 ergs) contained in the flare region, and also estimates of the total bolometric luminosity of the sun during the flare 4-6x10^32 ergs. Also, based on the measurement of the peak spectrum of energetic electrons at the Lagrangian point L1 of the Sun-Earth system by means of detectors onboard the Wind spacecraft, an estimate is obtained of the number and energy of the accelerated electrons emitted by the Sun during the flare. This number turned out to be several times smaller than the number of the HXR emitting electrons in the flare region, which does not contradict the estimates obtained for other events. Thus, it can be concluded that, despite its overall enormous energy, the giant solar flare considered is not out of the general solar flare concept. Apparently, the stored magnetic energy in the flare region was sufficient to explain its transformation into other energy channels, in particular, to the kinetic energy of the accelerated electrons (5-10% of the total flare). The information obtained about the fluxes of energetic electrons in the interplanetary medium in this giant event is used by us in modeling the telescope of solar energetic particles developed within the framework of the project. Based on the results of the work, an article by Sharykin I.N., Zimovets I.V., Myshyakov I.I., Meshalkina N.S. "Flare Energy Release in the Magnetic Field Polarity Inversion Line During M1.2 Solar Flare of March 15, 2015. Paper I. Onset of Plasma Heating and Electrons Acceleration" (https://arxiv.org/abs/1805.05792) was prepared and submitted to the editorial board of the Astrophysical Journal.

 

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Annotation of the results obtained in 2018
During second year we have manufactured and successfully verified operational status of the PICA ion analyzer prototype. During preliminary tests we checked the detector performance and estimated electrostatic analyzer ΔE/E energy resolution, which was 10% that corresponds to model parameters. During manufacture of the prototype we managed to fit target parameters of sizes and mass. Laboratory prototype mass (including minimum required electronics and cables) is 365g. Dimensions of the prototype are 92x97x76 mm, however it is worth to mention that a flight configuration requires additional electronics such as DC-DC voltage converters, interface and control circuit boards. Although there still remains some space within the prototype case that may be used for placing of some electronic parts. Some spatial resources may be also retrieved by cost of extension of instrument’s hight, this makes possible placing full electronics package within the instruments case and still remain within sizes suitable for the CubeSat-1U standard. The prototype of the ECOS electronic analyzer has been manufactured and passed the preliminary operability tests. During these tests we checked the operation of the position-sensitive detector and determined its spatial resolution. Spatial resolution of detector was estimated as 11 lines, which will allow to achieve the required analytical characteristics of the instrument. During development of the prototype we managed to reduce its mass and dimensions. The mass of the laboratory prototype (with electronics for the detector and technological cables) is estimated at 450g and will be specified after the next stage of preliminary tests. Prototype dimensions are 95x72x57 mm. Flight configuration of the instrument must be equipped with additional electronic boards with power supplies, interface and control circuits which will increase the height and width of the unit. However final dimensions of flight instrument will allow to fit it in the CubeSat-1U nanosatellite. The original software has been developed in order to facilitate the processes of setting up laboratory prototypes and simplify the determination of analytical characteristics. This software allows to control the components of the workstation for functional tests of the PIСA and ECOS prototypes and perform tests in an automated mode. The prototype of the proton part of the telescope of solar energetic particles (PPP-TSEP) has been manufactured. We tested several options for the geometry of the groove for attaching the optical fiber to the scintillator plates. The scintillator plates have been manufactured and tested. The measurements of the uniformity of light collection and light output were carried out. The temperature dependence of the registration efficiency of the silicon photomultipliers (SiPM) was studied. We built the calibration curves to adjust the offset voltage. A number of software tools based on CERN ROOT and Pandas for reading and processing measurement results has been developed. The PPP-TSEP was tested on cosmic muons and at a source of beta radiation. All tests were carried out in a thermostatted box, isolated from external lighting. In measurements on cosmic muons, a uniform distribution of the number of events and the energy release per event in different layers of the detector was obtained. This result is consistent with expectations, since high-energy cosmic muons are minimally ionizing particles and pass the detector through without significant energy loss. When measuring energetic electrons (laboratory source Sr-90, maximum energy 2.8 MeV), characteristic amplitude spectra were obtained in the input layer. Preliminary tests show the good performance of the prototype. The first observational statistical study of the relationship between flare sources of hard X-ray (HXR; ≥50 keV) emission observed by RHESSI and photospheric vertical electric currents (PVEC) calculated using 720-second HMI/SDO vector magnetograms has been finished for the 24th solar activity cycle. On a sample of 48 flares (from C3.0 to X3.1) observed on the solar disk by both instruments in 2010–2017, it was found that in 88% of events at least one HXR source is on the periphery of a strong region (jr>10^4 statampere/cm^2) PVEC in the form of ribbons, stretched mainly along the magnetic polarity inversion line (PIL), or islands. The values of the maximum PVEC density under the HXR sources in all the studied regions were in the range (0.03-2)x10^5 statamper/cm^2. No significant correlation was found between the intensity of HXR sources, PVEC density, and total PVEC below them. By comparing the post-flare and pre-flare maps of PVEC, no evidence was found of significant dissipation of PVEC in the regions corresponding to the HXR sources. In some cases, an enhancement of PVEC was detected during the flare. The results confirm the findings of earlier studies that the HXR sources tend to be located predominantly on the periphery of the strong PVEC areas. Taken together, the results do not support the concept of electron acceleration by a longitudinal electric field induced at the foot of the flare loops. The presence of ribbons and islands of supra-background PVEC indicates the presence of “bunches” of free magnetic energy in active regions. The flare energy release and acceleration of particles occurs in the vicinity of these “bunches”. However, how exactly this happens remains to be a puzzle requiring further investigation. We made detailed analysis of the confined (without fully developed eruption) solar flare of M1.2 class, which occurred on March 15, 2015 and was accompanied by electron acceleration (up to energy ~ 0.1–1.0 MeV) and plasma heating (up to ~ 40 MK) in a sheared magnetic arch extended along the photospheric magnetic polarity inversion line (PIL). The aim of the work was to determine the physical conditions of the flare energy release region based on the analysis of the dynamics of the magnetic field and electric currents in the impulsive phase of the flare near the PIL and the regions of precipitation of accelerated electrons into dense layers of the solar atmosphere. For the analysis, new vector magnetograms of HMI/SDO with a cadence of 135 s were used, which allowed the study of the magnetic field dynamics on the time scales of the flare impulsive phase. Previously, these data were not used for this purpose. It is shown that during the development of the flare energy release, the horizontal component of the magnetic field and the total photospheric vertical electric current (PVEC) near the PIL were amplified. An increase in the area of strong PVEC was observed, while the average (over the area) PVEC density decreased in this case. Sources of optical and hard X-ray (HXR) flare radiation were located near areas of strong horizontal magnetic field, strong PVEC, and a gradient of the vertical component of the magnetic field (> 1 kG / Mm). It is shown that the motion of the flare ribbons visible in the AIA/SDO 1700A ultraviolet channel corresponds to the appearance of new areas of strong PVEC. When expanding, the flare ribbons entered the regions with a more vertical magnetic field. Using the results of the extrapolation of the magnetic field within the nonlinear force-free field (NLFFF) approximation, we were able to establish the following. First, before the flare, the configuration of the magnetic field in the area under study was a system of highly sheared (up to 80 degrees) crossed over the PIL magnetic loops, some of which reconnected during the flare and formed a twisted structure like a magnetic flux-rope. Secondly, some of the magnetic field lines closest to the PIL became shorter during the development of the flare. Based on these results, it was concluded that the detected dynamics of the magnetic field, electric currents and sources of electromagnetic radiation from the flare are the result of a magnetic reconnection in the current layer with a strong (about 1200 Gauss) longitudinal component of the magnetic field above the photospheric PIL. The physical characteristics of the current sheet, in particular, the electric field in it, are estimated. It is established that the acceleration of electrons to the observed energies could well be carried out by this electric field. The reason for containment of the magnetic flux-rope eruption in this flare region requires further investigation. At the moment, 4 papers with the results of the project have been published in the journals indexed by WoS or Scopus, and, in addition, 2 papers are being reviewed by the journal within the WoS and Scopus database. During the presentation of the achieved results of the project at scientific conferences, several organizations, in particular, the Astronomicon Laboratory and the Samara National Research University, have shown interest in installing the developed prototypes of PICA and ECOS devices on the nanosatellites they create. Currently, negotiations are underway on the technical possibilities for the implementation of this task.

 

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