bluuebunny/crossref_metadata_2025 huggingface dataset:
Monitoring of 37C, 90Sr and 40Kin Sod-Podzolic Soils and Plants of Reference Sites of the Ivanovo Region
Authors: Utkin A. A. , Akanova N. I. , Noda I. B.
Published: April 2024

The results of radiation monitoring of sod-podzolic soils of reference agricultural plots of the Ivanovo region, conducted in 2014 and 2021, are presented. Background values of the specific activities of the studied radionuclides in the soils of reference sites have been established. According to the pollution density of the arable horizon of soils 137Cs and 90Sr, the level of the ecological situation was determined, which made it possible to attribute the soils of all reference areas of the region to uncontaminated territories suitable without restrictions for agricultural use. The power of the exposure dose of gamma radiation of soils and the contribution of 40K and 137Cs to the formation of the gamma background of soils were determined. Correlation analysis determined the influence of individual physical and chemical properties of soils on the behavior and distribution of radionuclides in the soil and the relationship between the content of the radionuclides themselves. Based on the values of the specific activity of 137Cs and 90Sr in plant products grown in 2014 and 2021, rows of cultivated plants with a decreasing ability to accumulate these radionuclides from the soil were constructed. All grown plant products of all types of crops fully met the veterinary standards required to limit the content of 137Cs and 90Sr in plant feeds (green mass, straw and feed grain). The coefficients of accumulation and transition of 137Cs and 90Sr from soil to plants are calculated. The coefficients of linear correlation between the values of the specific activity of 137Cs and 90Sr in soils and plants revealed the strength and nature of these dependencies.
Compositions of Fungicides with Growth Regulators which Reduce the Retarding Effect of Crop Protectants
Authors: Zorkina O. V. , Sukhova E. A. , Agapova O. O. , Nefedieva E. E. , Gribust I. R. , Kolotova O. V.
Published: April 2024

One of the reasons for the decrease in the yield of crops is the retardant effect of fungicides. In addition, many fungicides have a toxigenic effect on the mycelium of the fungus. The combination of a fungicide and a plant growth stimulant in a complex preparation can help to reduce the level of the negative effect of the pesticide. It is proposed to introduce individual growth regulators and their combination into the composition of the seed protectant in doses of 50, 100, 200 g/l. The length and the weight of the root and shoot of seedlings under the influence of the seed protectant were less than in the control, and the weight of the endosperm of grain was greater. Under the influence of the seed protectant and gibberellic acid, the length of the shoots corresponded to the control, but their weight was decreased. Indolylbutyric acid, added to the seed protectant, contributed to the effective consumption of spare substances of the endosperm of grain and root growth. Under the influence of the protectant and diphenylurea, the length and the weight of the shoot increased significantly in a balanced manner. The composition of the protectant and the named growth regulators in minimal doses affected the growth of the roots and shoots in the best way of all variants. Preference should be given to low doses of phytohormones and their combination.
Fertility of Leached Chernozem as a Result of 85-Year Application of Fertilizers in Grain-Beet Crop Rotation under Conditions of the Central Black-Earth Region
Authors: Minakova O. A. , Alexandrova L. V. , Podvigina T. N.
Published: April 2024

The use of fertilizers in the grain-beet crop rotation for 85 years significantly changed the agrochemical properties of leached chernozem, which were most pronounced in the optimization of the phosphate regime of the soil and least of all – potash. Fertilization changed the nitrogen regime and physico-chemical properties of the soil to a greater extent in a layer of  20–40 cm than –20 cm. It was found that the content of P2O5 in the soil under crops of grain crops was higher than under sugar beet crops, and K2O and pHKCl were less. The greatest changes in the agrochemical properties of the soil under sugar beet crops were noted when using N190P190K190, cereals – with the aftereffect of N135P135K135 + manure 25 t/ha.
Combined Triazole Disinfectants and Their Influence on the Growth and Development of Spring Wheat Seedlings
Authors: Kekalo A. Yu. , Khalikov S. S. , Ilyin M. M. , Chkanikov N. D. , Zargaryan N. Yu.
Published: April 2024

Seed treatment with fungicides is a crucial link in the plant protection system, and systemic drugs give the best effect. Therefore, it is very important to develop scientific foundations for the preparation of complex preparations with a low rate of consumption of the active substance and the inclusion of plant growth regulators that enhance growth processes and the yield of the main crop. In recent years, the directions of modification of known and practiced fungicides by various methods, including methods of mechanochemistry, have been promising. The problem of creating both new substances and their effective formulations remains urgent. Taking into account the prospects and high efficiency of triazole fungicides in the system of complex plant protection, the creation of multicomponent seed protectants of grain crops is proposed. The purpose of this study was to develop preparations based on tebuconazole (TBC) and propiconazole (PPC) in the form of solid dispersions (SD) and to study their biological activity on spring wheat plants in the conditions of the Trans-Urals. At the same time, the retardant effect of these triazoles was also studied with the help of the domestic growth regulator Floroxan. The use of new preparations on spring wheat made it possible to reduce the damage to the culture by root rot by 85–87%, productive bushiness increased by 6–11% compared to the control without treatment. A reliable increase in crop yield of 2.2 c/ha or 14% was obtained using preparation 2 (TD of the composition TBC : PPC : AG : silica = 1 : 1 : 7 : 1 + Phloroxane when the polysaccharide (AG) and the auxiliary substance of silica are included in the composition). The inclusion of the growth regulator Floroxan in the composition of the mordant mixture reduced the antioxidant effect of tebuconazole and stimulated the growth and development of wheat seedlings. It was proved that such a biological effect was achieved in conditions of drought of varying intensity during the growing season of 2021–2022.
Effect of Bacterial Fertilizers on the Microbiological Activity of Segregated Chernozem in Spring Barley Crops
Authors: Cheverdin A. Y. , Cheverdin Yu. I. , Sautkina M. Y.
Published: April 2024

In the field experiment, in the Voronezh region on the territory of the Voronezh FASC, changes in the microbiological activity of the soil under the influence of bacterial associative biological products and mineral fertilizers during 2021–2022 were studied. Microbial strains were used for pre-sowing seed treatment. The soil of the experimental site is ordinary (segregational) medium–humus heavy loamy chernozem. The availability of available forms of batteries is medium and high. The barley variety is Talovsky 9. The cultivation technology is generally accepted in the zone. The preservation of soil fertility and its rational use due to changes in the direction of microbiological processes in the soil with the use of diazotrophs has been established. Associative preparations slowed down the processes of mineralization of humic substances. The number of bacteria associated with the destruction of organic matter decreased. With the complex use of mineral fertilizers with rhizobacteria, the number of nitrifiers responsible for denitrification processes and losses of soil nitrogen significantly decreased. A significant increase in the natural background of fertilization of the number of soil fungal microflora under the influence of diazotrophs was noted.
Effectiveness of Foliar Top Dressing of Flax with the Drug Controlit-Si on Different Backgrounds of Mineral Nutrition in the Conditions of the Central Non-Chernozem
Authors: Konova A. M. , Gavrilova A. Y. , Samsonova N. E.
Published: April 2024

The responsiveness of flax to mineral fertilizers and foliar top dressing with an aqueous solution of the drug Controlfit-Si on sod-podzolic medium loamy soil was studied. It is shown that the reaction of flax to mineral fertilizers depended on the hydrothermal environmental conditions, doses and the ratio of nutrients. Excessive humidity and arid conditions negatively affected the productivity of crops. Foliar top dressing of plants with the drug Controlfit-Si leveled the negative impact of adverse weather conditions, increased the responsiveness of plants to mineral fertilizers, contributed to a more complete use of nutrients from fertilizers. On average, for 3 years on the backgrounds of full mineral fertilizer, top dressing increased the yield of flax straw by 25–30% with the best effect against the background of N48P48K48 (4.03 t/ha). Top dressing did not have a positive effect on the yield of flax seeds. It took 13.8 kg N, 5.9 kg P2O5 and 10.7 kg K2O to form 1 ton of flax crop with the appropriate amount of seeds, regardless of plant nutrition conditions.
Laboratory Modelling of Solar Wind Interaction with Lunar Magnetic Anomalies
Authors: Rumenskikh M. S. , Chibranov A. A. , Efimov M. A. , Berezutsky A. G. , Posukh V. G. , Trushin P. A. , Zakharov Yu. P. , Boyarintsev E. L. , Miroshnichenko I. B. , Divin A. V. , Shaikhislamov I. F.
Published: April 2024

The paper presents the results of laboratory experiment modeling the interaction between Lunar magnetic anomalies and Solar wind. To model the LMA we use quadrupole magnetic field. The main dimensionless parameter of the problem, the ion inertia length relative to the mini-magnetosphere size, well corresponds between experiment and LMA conditions. The main result is measurement of the magnetically reflected proton fluxes, which show qualitative agreement to available satellite data.
Section “Experimental Laboratory Astrophysics and Geophysics” of the National Center for Physics and Mathematics
Authors: Zelenyi L. M.
Published: April 2024

This issue includes articles devoted to the results of the work of the section “Experimental laboratory astrophysics and geophysics” of the National Center for Physics and Mathematics.
Dust Particles in Space: Opportunities for Experimental Research
Authors: Kuznetsov I. A. , Zakharov A. V. , Zelenyi L. M. , Popel S. I. , Morozova T. I. , Shashkova I. A. , Dolnikov G. G. , Lyash A. N. , Dubov A. E. , Viktorov M. E. , Topchieva A. P. , Klumov B. A. , Usachev A. D. , Lisin E. A. , Vasiliev M. M. , Petrov O. F. , Poroikov A. Yu.
Published: April 2024

Space dust and dusty (complex) plasma are one of the most common manifestations of matter in space. Non-atmospheric bodies of the Solar System, such as the Moon, asteroids, comets, some satellites of the planets, are directly affected by external factors of outer space—solar electromagnetic radiation, interplanetary plasma flows, cosmic rays, micrometeors. Under the influence of these factors, regolith is formed on the surface of bodies during geological epochs. Under the influence of impacts of high-speed micrometeors, dust particles of regolith scatter at different speeds. Most of them return to the surface, but some form dust clouds or lose their gravitational connection with the parent body. Under the action of solar radiation, the surface acquires an electric charge, and dust particles under certain conditions can break away from the regolith surface and levitate. Observational evidence of such dynamic phenomena has been recorded on the Moon and on some asteroids. The study of the physical processes responsible for the activation of dust particles and their dynamics is of great interest for fundamental science and practical purposes. The article discusses the main processes occurring under the influence of outer space factors on regolith, as a result of which dust particles move and a near-surface plasma-dust exosphere is formed. Unresolved issues are discussed. Methods and means of laboratory modeling in studying the activation and dynamics of dust particles are considered.
A Study of Variability of the Stokes Parameters and the Magnetic Field of G43.8–0.1 in the OH Line 1665 MHz
Authors: Ashimbaeva N. T. , Lekht E. E. , Krasnov V. V. , Tolmachev A. M.
Published: April 2024

We present results of the study of maser emission variability in the 1665 MHz OH line in the G43.8–0.1 star formation region based on observations (monitoring) in 2008–2022 at the Large Radio Telescope in Nancy (France). Variability of all polarization parameters of the majority of spectral features, which has a monotonic regular character, has been found. Spatial identification of the main spectral features of the OH 1665 MHz line with maser spots (condensations) on the VLA map has been carried out. For the Zeeman pair VLSR=44.15 km/s, a monotonic change of the splitting with time during 2008–2022 was found and, consequently, a change of the magnitude of the longitudinal magnetic field. According to our calculations, at the end of 2012, the direction of the magnetic field changed to the opposite. Сorrelated with H∥, there were changes in the angle χ and, as a consequence, changes in the direction of the vector of the transverse magnetic field H⊥0. For the maser feature at 44.5 km/s, a change of H⊥ by 180° was found. In 2016–2022, some reorientation of the global magnetic field (H⊥) in G43.8–0.1 occurred. The field became less chaotic: in the eastern part, the field in maser condensations is perpendicular to the arc, and in the western part, it is parallel to the arc. It is assumed that the global magnetic field in the entire U H II region of the G43.8–0.1 source has the same direction: along the axis (northeast)—(southwest).
Star Structure of the Northern Part of the Orion Sword Region
Authors: Vereshchagin S. V. , Chupina N. V.
Published: April 2024

According to the data of the Gaia DR3 catalogs, the belonging of the stars of group 189 ([1]), located in the northern part of the Orion Sword region, to the open star cluster (OSC) NGC 1977 was analyzed. To do this, the revision of the stellar composition of the northern part of the Orion Sword region (around the center of the OSC NGC 1977) was carried out using proper motions (PM) and parallaxes. At the same time, a part of the OSC NGC 1981, also located in the region under consideration, was captured. The presented catalog (n = 1041) includes candidate stars both in NGC 1977 and in NGC 1981 with the corresponding probabilities. The status of the stars of group 189 (Oricat 2836 and Oricat 2914) suggests their contribution to the X-ray radiation detected in this region. The question of the possible gravitational coupling of the NGC 1977–NGC 1981 pair is considered.
Dynamic Study of the Triple Star T Tauri
Authors: Kiyaeva O. V. , Romanenko L. G.
Published: April 2024

The triple system of young stars T Tauri was discovered relatively recently and has attracted the attention of numerous researchers. Many papers have been dedicated to the study of the physical properties of the system’s stars, which are surrounded by a disk of dust and gas. Our work is focused on the astrometric analysis of this triple system using the method of apparent motion parameters (AMP). Currently, the orbit of the inner pair Sa-Sb with a period of 27 years is well-established. Based on the Gaia DR3 parallax, its total mass MSa + Sb=2.49M⊙. Relying on the published high-precision uniform observations with the Keck 1 and VLT telescopes, we employed the AMP method to derive two orbits for the outer pair N-S, one of which is almost circular. For a circular orbit, it is possible to calculate the orbital elements and dynamic parallax for a given mass solely using the apparent motion parameters. This enabled a comparison between the dynamic parallax and the high-precision parallax from the Gaia DR3 catalog, facilitating the calculation of masses of each component based on the mass of the inner subsystem: MN=(2.4±0.2)M⊙, MSa=(2.09±0.05)M⊙, MSb=(0.40±0.05)M⊙. The boundaries for the orbital period were estimated to be 500⩽P⩽700 years.
The Exo-Jupiter Candidate FL Lyr b in Data of Kepler and TESS Space Missions
Authors: Kozyreva V. S. , Bogomazov A. I. , Demkov B. P. , Zotov L. V. , Tutukov A. V.
Published: April 2024

We study the light-time effect in the eclipsing binary system FL Lyr using data of the Kepler and TESS space missions. We demonstrate that the system contains a candidate exo-Jupiter FL Lyr b, its probable orbital period being about 22 years.
Analysis of the Possibilities of Short-Term Prediction of Geomagnetic Perturbations from Observations of Coronal Mass Ejections at the BSA LPI Radio Telescope
Authors: Lukmanov V. R. , Chashei I. V. , Tyul’bashev S. A. , Subaev I. A.
Published: April 2024

From April 2021 to October 2022, in the monitoring data obtained daily at the Big Scanning Antenna radio telescope (BSA LPI), 11 events were identified for which X-ray flares in the solar corona were followed by magnetic storms on Earth. Interplanetary scintillation monitoring data were considered together with data on solar flare activity and a simple kinematic model of ejection propagation. Based on the estimated ejection velocity between the Sun and the probed region, under the assumption of a constant velocity, the time of arrival of the ejection to the Earth was calculated. Of the 11 events considered, 7 are associated with solitary flares followed by a coronal mass ejection (CME) and 4 are more complex and possibly associated with corotating perturbations or a superposition of corotating and flare perturbations. For the entire set of events, the average time of the real onset of a magnetic storm after the time predicted by the model was 3.6 h and the average time between the onset of scintillation enhancement and the onset of a magnetic storm was 20.1 h. For events associated with solitary flares, the magnetic storm began, on average, 0.8 hours after the predicted time and 15.6 hours after the onset of scintillation enhancement. The delay of magnetic storms with respect to the predicted time is apparently related to the deceleration of the ejection between the probed region of the solar wind and the Earth’s orbit.
INVESTIGATION OF THE MAGNETIC FIELD FROM OBSERVATIONS OF THE OH MASER IN THE G10.624–0.385 STAR FORMATION REGION
Authors: Ashimbaeva N. T. , Lekht E. E. , Krasnov V. V. , Tolmachev A. M.
Published: April 2024

The results of a study of the variability of maser emission in OH lines in the 18 cm range in the G10.624–0.385 star formation region from monitoring data performed at the Large Radio Telescope in Nançay (France) in 2008–2023 are presented. It is obtained that for a Zeeman pair in line 1667 MHz splitting (about 1.96 km/s) and, consequently, the magnitude of the longitudinal magnetic field have been stable for more than 25 years. In the satellite lines of 1612 and 1720 MHz, broadband absorption and emission are observed, respectively. Mirrored The profiles of the OH 1612 and 1720 MHz satellite lines indicate that the levels of the corresponding transitions are pumped by IR radiation from a source immersed in a magnetized molecular cloud around the OH maser. Spatial identification of details in both main lines is carried out. It is found that the transverse magnetic field is directed mainly along some organized structure in the form of an arc.
LONG MAGNETIC MINIMUM OF HD 166620 – POSSIBLE BEGINNING OF THE ANALOGUE OF THE MAUNDER MINIMUM
Authors: Savanov I. S.
Published: April 2024

Based on photometric observations published in the literature, the manifestations of the activity of the K2V dwarf HD 166620 were studied. The obtained results are compared with the results of the analysis of the chromospheric activity of the star. HD 166620 is entering in a long magnetic minimum and may be the first reliable candidate for objects that are at a minimum of activity similar to the Maunder minimum (MM) of the Sun. Studies of changes in the magnetic activity of the star were carried out based on the values of the S‑index (1885 measurements in the observation interval for 53.6 years), obtained mainly before its entry into the MM phase, and on photometric measurements of the brightness in the b and y filters covering 17 seasons from 1993 to 2020 obtained with the automatic APT telescope (MM phase and its beginning). It has been established that the Kamogata Wide-field Survey observation data combined into a single array in filters B, V and Ic (about 1400 measurements) convincingly demonstrates the long-term variability of the HD 166620 brightness in the phase of the probable MM state. At the same time, the observations of the Kamogata Wide-field Survey fill the gap in the photometric data of the APT automatic telescope well. The value of the cycle (about 4000 days) is comparable to the duration of observations, with its refinement by according to the data of a larger time interval, it is possible that it will correspond more to the value found from the data on chromospheric activity. The main results of the work should include the cyclic long-term changes in the activity of the star detected by us during the beginning of the MM phase. The question of clarifying the value of the rotation period HD 166620 remains open. There were no significant peaks corresponding to the value P = 45.06 days, previously accepted as the period of rotation of the star, on almost all the power spectra constructed by us. It is noted that further observations are required to establish the full duration of the minimum phase of the star’s activity.
NEW FORMS OF MATTER IN THE UNIVERSE
Authors: Cherepashchuk A. M.
Published: April 2024

The article presents an overview of the development of our ideas about new forms of matter in the Universe.
PROBLEMS OF THE ORIGIN OF THE UNIVERSE
Authors: Novikov I. D.
Published: April 2024

The paper presents an overview of the main foundations of cosmology and its current state.
INFLUENCE OF RADIATION FORCES ON THE OBSERVED POSITION AND EVOLUTION OF THE ORBIT OF SPACE DEBRIS OBJECTS WITH A HIGH AREA-TO-MASS RATIO
Authors: Sannikova T. N.
Published: April 2024

This study is devoted to assessing the effect of light pressure on the observed position and orbital elements of space debris objects with a large area-to-mass ratio \(A{\text{/}}m\) in the region of medium-high, geostationary and highly elliptical orbits over short time intervals (up to 1 year). Numerical integration of the orbits of 78 model objects was performed at 8 values of \(A{\text{/}}m\) from \(0.01\) to \(125\) m2/kg and two values of the reflection coefficient \(k = 1.0\) and 1.44. The maximum (during the given time periods) angular distances relative to the sub-satellite point on the Earth’s surface between the positions found with and without radiation forces, as well as the maximum changes in the semi-major axis, eccentricity and inclination of the orbit under the influence of radiation forces during the integration time, are determined. It is found that for all objects there is a negative drift of the semi-major axis. For models with semi-major axes of 10 000, 15 000, and 20 000km, the inclination variations do not exceed \(15^\circ \). Among other objects, at \(\gamma = kA{\text{/}}m \geqslant 50\) m2/kg, cases of transitions from direct to reverse motion (and vice versa) due to light pressure, were recorded, which indicates the possibility of flips of the orbital plane under the influence of radiation forces even in the short term. The duration of successful integration (the lifetime of an object in orbit) is given; it was less than \(1\) year for most models with \(\gamma \geqslant 50.0\) m2/kg. Also the time intervals during which the displacement of the position perturbed under the influence of radiation forces from the unperturbed one does not exceed \(5\prime \), \(45\prime \), and \(3^\circ \) are presented, depending on the value of \(\gamma \), semi-major axis, and eccentricity in the initial epoch. Based on the results of the article, it is possible to estimate the required frequency of observations of objects with large \(A{\text{/}}m\).
X-RAY ASTRONOMY AND CLOSE BINARY SYSTEMS
Authors: Cherepashchuk A. M.
Published: April 2024

The discovery in 1962 of the compact source Sco X-1, the first X-ray source located outside the Solar System, marked a new (“golden”) era in the study of close binary systems (CBS). Accreting neutron stars and first black hole candidates in close binary systems were discovered. The ability to “weigh” neutron stars and black holes in close binary systems made it possible to distinguish accreting black holes from neutron stars. The theory of accretion onto relativistic objects in close binary systems has been developed, as well as the theory of the evolution of close binary systems with mass exchange up to the latest stages, including binary black holes and neutron stars. Close binary systems have become the cutting edge of astrophysics. Subsequent observations of gravitation waves and observations on the EHT intercontinental radio interferometer with an angular resolution of ~10–5 arcsec made it possible to finally prove the existence of black holes in the Universe. Thus, the modern triumph of black holes has largely been due to the development of the science of close binary systems. The paper is based on a talk presented at the astrophysical memorial seminar “Novelties in Understanding the Evolution of Binary Stars”, dedicated to the 90th anniversary of Professor M.A. Svechnikov.
DEDICATION TO MARIJ ANATOLYEVICH SVECHNIKOV
Authors: Polushina T. S.
Published: April 2024

The paper is dedicated to the memory and scientific heritage of Marij Anatolyevich Svechnikov, an outstanding researcher and teacher, founder of the Ural school of study of close binary systems and author of the classification of eclipsing variable stars. The paper provides a brief overview of the major life events and main scientific achievements of M.A. Svechnikov. The best memory is the continuation and development of those s-cientific directions to which he devoted his scientific activity. The research initiated by M.A. Svechnikov was continued in the works of his apprentices and followers at the Ural State University, Chelyabinsk State University, Chita State University, etc. The paper is based on a talk presented at the astrophysical memorial seminar “Novelties in Understanding the Evolution of Binary Stars”, dedicated to the 90th anniversary of Professor M.A. Svechnikov.
RADIO EMISSION SPECTRUM OF COMPOSITE SUPERNOVA REMNANT G74.9+1.2
Authors: Ivanov V. P. , Ipatov A. V. , Rahimov I. A. , Andreeva T. S.
Published: April 2024

Measurements of the flux densities of the supernova remnant (SNR) G74.9+1.2 (CTB 87) at frequencies of 4840 and 8450 MHz were carried out with the RT-32 radio telescope of the Svetloye observatory of the IAA RAS in 2018–2019. The data obtained contain signs of the presence of a source of a variable component in the radio emission on a time scale of a month or more. The flux densities of G74.9+1.2 over the time interval 1959.7–2010 are determined from published data, which makes it possible to compare the intensities of G74.9+1.2 and standard sources. All data are presented in a single system based on the exact scale of “artificial moon” (AM) fluxes. A refined spectrum of SOS G74.9+1.2 was obtained. The totality of available data is approximated by two power-law sections with different spectral indices: \({{\alpha }_{1}} = 0.31\) at frequencies \(f {{f}_{b}}\) and \({{\alpha }_{2}} = 0.71\) at \(f {{f}_{b}}\). The projections of two power law sections intersect at a frequency \({{f}_{b}} \approx 3409\) MHz. The break in the radio spectrum of the source, taking into account its age (more than 4000 years), could be formed as a result of synchrotron losses. The increase in the steepness of the spectrum close to 0.5 above the frequency \({{f}_{b}}\) is an argument in favor of such an assumption. The totality of data obtained during measurements on the RT-32 and on the basis of published works allows us to state that the variable component in the G74.9+1.2 radio emission on all time scales is much less pronounced compared to younger PWNs. As a possible mechanism for the observed variability, a reconnection of the magnetic field lines in the pulsar magnetosphere is proposed.
TO THE QUESTION OF THE LOCALIZATION OF CME GENERATION ON THE SUN
Authors: Yazev S. A. , Tomozov V. M.
Published: April 2024

The localization of CME occurrence zones on the Sun from November 2006 to February 2007 was studied using the SOHO catalog. A method is described for comparing such zones with active regions (ARs) both in the visible and invisible hemispheres of the Sun. It is shown that a simple linear continuation of the projections of the CME trajectory on the Sun in many cases passes by the AO. 63.5% of CMEs managed to be tied to ARs, 19% failed, and for 17.5% a choice must be made between ARs and flare sites, where spots were observed 1–3 rotations of the Sun earlier. The hypothesis is discussed that the displacement of the beginning of the CME trajectory from the AR centroid is associated with the asymmetry of the location of the magnetic rope, on the basis of which the CME is formed, with respect to the AO: one base of the rope is located near the strong magnetic fields of sunspots, the second is in the region of weak fields on the periphery or outside the AO.
A PLANET OR PRIMORDIAL BLACK HOLE IN THE OUTER REGION OF THE SOLAR SYSTEM AND THE DUST FLOW NEAR EARTH’S ORBIT
Authors: Eroshenko Yu. N. , Popova E. A.
Published: April 2024

In recent years, evidence has been obtained that in the outer region of the Solar System (in the inner Oort cloud) at a distance of ~300–700 AU from the Sun, there may be a captured planet or a primordial black hole. In this paper, we show that the gravitational scattering on this object of dust particles located in the same region can transfer them to new elongated orbits reaching the Earth’s orbit. With the mass of the captured object of the order of 5–10 Earth masses, the calculated dust flow near the Earth is ~0.1–3 μg m–2 year–1 is comparable in order of magnitude with the observed flow. This effect gives a joint restriction on the parameters of the captured object and on the amount of dust in the Oort cloud.
PARAMETERS OF RADIO PULSARS AT DIFFERENT DISTANCES FROM THE “DEATH LINE”
Authors: Ken’ko Z. V. , Malov I. F.
Published: April 2024

Calculations of angles \(\beta \) between magnetic moments and rotation axes have been carried out for radio pulsars located at different distances from the “death line”. It is shown that these angles decrease from 36° to 10° when pulsars move to the “death line”. Such values correspond to kinematic ages from 1 to 10 millions of years. It is detected also that for these ages radio luminosities of pulsars decrease. This means that radio pulsars fade out when their age increases.
RATE OF SOLAR NANOFLARES IN DIFFERENT SPECTRAL RANGES
Authors: Belov S. A. , Zavershinskii D. I. , Bogachev S. A. , Ledentsov L. S.
Published: April 2024

The frequency and rate of solar nanoflares (NF) were measured in 6 coronal spectral ranges (094, 131, 171, 193, 211, 335 Å) and one, related to the transition layer (304 Å). We used SDO/AIA data obtained at solar minimum in May 2019. We analyzed the same region of the Sun, covering \(360\text{\textquotedblleft} \times 720\text{\textquotedblleft}\) field-of-view, in all channels over the same time interval of 1 hour. In all the spectral bands, to search for NF we applied the same algorithm based on the amplitude analysis of fast brightenings in AIA images. The frequency and rate of NF, as can be expected, vary significantly in different wavelengths. For threshold \(5\sigma \), the highest NF frequency, 207 c–1, was measured in 171 Å. The next spectral ranges are 193 Å (85% of 171 channnel), 211 Å (74%), and 131 Å (63%). We have not been able to reliably measure the frequency in channels 094 Å, and 335 Å, but found that it is less than 15% of the frequency in channel 171 Å. In the 304 Å channel, we found a large number of brightenings that do not match any coronal events. However, about 40% of NF in corona have a counterpart in the 304 Å line with an amplitude higher than \(5\sigma \).
SOLAR CYCLE STRUCTURE AND STRUCTURE OF ACTIVITY CYCLES AT LATE TYPE STARES
Authors: Obridko V. N. , Sokoloff D. D. , Katsova M. M.
Published: April 2024

It is shown that the use of a description of the solar cycle that takes into account the odd zonal harmonic of the solar magnetic field allows us to deepen our knowledge of two important aspects of solar activity: first, to clarify and expand predictions for the near future of the evolution of the cyclic activity of the Sun, second, to formulate a program for monitoring the spectrophotometric characteristics of the radiation of stars like the Sun, aimed at obtaining new information about their magnetic fields.
PHYSICAL PROPERTIES AND KINEMATICS OF DENSE CORES ASSOCIATED WITH REGIONS OF MASSIVE STAR FORMATION FROM THE SOUTHERN SKY
Authors: Pirogov L. E. , Zemlyanukha P. M. , Dombek E. M. , Voronkov M. A.
Published: April 2024

The results of spectral observations in the \( \sim {\kern 1pt} 84{\kern 1pt} - {\kern 1pt} 92\) GHz frequency range of six objects from the southern sky having dense cores and associated with massive star and star cluster forming regions are presented. The observations are carried out with the MOPRA-22m radio telescope. Within the framework of the local thermodynamic equilibrium (LTE) approximation, column densities and abundances of the H13CN, H13CO+, HN13C, HC3N, c-C3H2, SiO, CH3C2H and CH3CN molecules are calculated. Kinetic temperatures (\( \sim 30{\kern 1pt} - {\kern 1pt} 50\) K), sizes of emission regions (\( \sim 0.2{\kern 1pt} - {\kern 1pt} 3.1\) pc) and virial mass esimates (\( \sim 70{\kern 1pt} - {\kern 1pt} 4600{\kern 1pt} {{M}_{ \odot }}\)) are obtained. The linewidths in the three cores decrease with increasing distance from the center. Four cores exhibit asymmetry in the profiles of the optically thick HCO+(1–0) and HCN(1–0) lines, indicating the presence of systematic motions in the line of sight. In two cases, the asymmetry can be caused by contraction of gas. The model HCO+(1–0) and H13CO+(1–0) spectral maps obtained within the non-LTE spherically symmetric model are fitted into observed ones. Radial density (\( \propto {\kern 1pt} {{r}^{{ - 1.6}}}\)), turbulent velocity (\( \propto {\kern 1pt} {{r}^{{ - 0.2}}}\)) and contraction velocity (\( \propto {\kern 1pt} {{r}^{{0.5}}}\)) profiles in the G268.42–0.85 core are obtained. The contraction velocity radial profile differs from expected both in the case of free fall of gas onto a protostar (\({{r}^{{ - 0.5}}}\)), and in the case of global core collapse (contraction velocity does not depend on distance). A discussion of the results obtained is provided.
KINEMATICS OF HIGH-SPEED STARS WITHIN 300 PCS FROM THE SUN ACCORDING TO GAIA DR3
Authors: Tutukov A. V. , Chupina N. V. , Vereshchagin S. V.
Published: April 2024

The kinematics of stars from the solar neighborhood with a radius of 300 pc has been studied using the Gaia DR3 data. Our sample includes n = 970 171 stars – AG300 (A – ensemble, G – Gaia, 300 – radius of the studied zone in pc). The kinematics of these stars reflects the morphology of the main stellar populations of the Galaxy: the stellar disk, bulge, halo, and stellar corona of a supermassive black hole (SMBH). The presence of stars in AG300 with velocities exceeding the escape velocity from the Galaxy indicates the presence in the circumsolar space of extragalactic stars belonging to the stellar component of the local cluster of galaxies. It is shown that the known mechanisms of acceleration of the spatial motion of stars make it possible to create a stellar halo of galaxies, a stellar corona of SMBH in its core, an intergalactic stellar medium of galaxy clusters, and spaces between galaxy clusters. The AG300 catalog makes it possible to identify representatives of all named components.
AERONOMIC MODEL OF HYDROGEN-HELIUM UPPER ATMOSPHERES OF HOT GIANT EXOPLANETS
Authors: Zhilkin A. G. , Gladysheva Y. G. , Shematovich V. I. , Bisikalo D. V.
Published: April 2024

The paper presents 1D aeronomic model of hydrogen-helium upper atmospheres of hot giant exoplanets based on the approximation of single-fluid multicomponent hydrodynamics. Chemical reactions and heating-cooling processes are taken into account. Typical hot Jupiter and warm Neptune are considered as an example of the application of the model. Calculations were carried out for various values of gas pressure at the photometric radius of the planet. In the solutions obtained, a transonic planetary wind is formed, leading to a hydrodynamic outflow of the atmosphere with mass loss rates of the order of \(3.5 \times {{10}^{{10}}}\) g/s for hot Jupiter and \(3.7 \times {{10}^{9}}\) g/s for warm Neptune. At the same time, the outer layers of the atmosphere of hot Jupiter are completely ionized, while the atmosphere of warm Neptune mainly consists of neutral gas. In some variants of the hot Jupiter model, instability develops in the deep layers of the atmosphere, which can lead to the formation of a specific cloud layer.
Frequency and time domain characteristics of the insect visual system in optic flow
Authors: Zienko S. I , Zhbanova V. L
Published: April 2024

Frequency and time domain properties of the monochromatic, dichromatic, and trichromatic visual system in an insect have been studied. The research method is based on the representation of the optical flow field of the insect visual system in the form of a dynamic link with an input and output. The Gaussian function was used to approximate the spectral curves. The study of the inertial properties of such a link in the time domain was performed by applying signals to its input in the form of a δ-function or a unit function. The steady-state forced oscillations at the output of the investigated dynamic link are determined when a harmonic effect is applied to the input. A technique for constructing spectral sensitivity curves for monochrome, dichromatic, and trichromatic vision of insects in the frequency domain is proposed; it has been established that the spectra exhibit the properties of ultra wideband signals. It has been found that the dynamic link of the insect visual system is capable of amplifying the optical signal over ultraviolet and blue parts of the spectrum in the time and frequency domain. It has been revealed that at a frequency equal to or higher than the frequency of dielectric relaxation, the optical flow field of the insect's visual system does not sense electromagnetic radiation. This phenomenon is most pronounced in ultraviolet and blue parts of the spectrum. It has been established that the optical signal wideband index μ varies from 0.41 to 1.21; thus, the visual system of an insect has ultra wideband properties. It has been shown that the number of periods of light oscillations in the visual system of insects, which has a spectrum in the form of a Gaussian curve, is related to the exponent μ by a simple relationship. New knowledge gained can be used for creation of matrix solid-state photodetectors in ultraviolet and blue parts of the spectrum.
Numerical modeling of pre-spawning and spawning migrations of the representative of the family hexagrammidae: the case of the arabesque greenling
Authors: Chetirbotsky A. N , Vdovin A. N , Chetirbotsky V. A
Published: April 2024

This paper presents a spatio-temporal model of greenling dynamics during pre-spawning and spawning mass migrations. The developed model is based on original verified long-term observations and data on industrial fishing in the Peter the Great Bay (Sea of Japan), and the equations of the dynamics of the density of males/females and the mass daily movements of fish are written in terms of the transfer equations. These equations are written in the form of the modified Patlak-Keller-Segel equations, according to which the flow of objects/substances is directed along the gradients of stimulus introduced. It is believed that in the pre-spawning season, adaptation in morpho-physiological (biochemical thermoregulation and a number of other endogenous processes) and behavioral responses of fish to sufficiently long and energy-consuming spawning can occur, where the stimulus for mass movements of fish is optimal environmental conditions for spawning events. During the spawning period, selected sites will be found in convenient and well-aerated embayments located at the bottom of reservoir in the coastal area. Modeling of stimuli-related movements is performed based on information about the preferred water depths of the fish's pre-spawning area and relevant features relating to a selection of suitable bedding sites. It is assumed that the intensity of daily motion is proportional to their linear size (the larger the fish becomes, the faster it is). The equations for the spawning stage take into account the spatial competition of males, but in natural conditions it is observed only in the vicinity of spawning areas. Being away from these areas, males continued to look for new sites good for the spawn. For females, their movement is provoked by males that assembled in schools, the signal of which can be certain chemical elements released by males (for example, mucus secretion from males) or visual contact. The diffusion of fish distribution and the viscosity of the habitat (velocity diffusion) are taken into account. The initial distribution of fish is given according to the average distribution of fish in July over a long-term observation period in the Peter the Great Bay.
Cartesian genetic programming for image analysis of the developing drosophila eye
Authors: Danilov N. A , Kozlov K. N , Surkova S. Y , Samsonova M. G
Published: April 2024

Automatic feature extraction methods have gained increasing attention in modern image processing. The confocal images of the single-layered epithelium of the developing Drosophila eye may form an excellent model system to develop methods for complex feature extraction. The aim of this work was to explore Cartesian genetic programming for determination of the boundaries of ommatidia, the light-sensitive units in the presumptive eye region. Application of Cartesian genetic programming for the analysis of Fasciclin III expression has shown good results. This opens interesting perspectives for further use of this technology in the automatic analysis of confocal images.
Luminescent diagnostics and quantitative assessment of malaria based on a lateral flow immunoassay with cdte quantum dots
Authors: Chauhan H. , Jariwala A. , Kheraj V.
Published: April 2024

A lateral flow immunoassay (LFI) is a simple, low-cost and rapid diagnostic tool to identify various diseases by detecting analytes such as antibodies, parasites, or other relevant biomarkers. However, most LFIs can only confirm the presence or absence of a target analyte being applied as qualitative diagnostic tools. In addtion, the conventional LFIs, which require visual inspection of the test line, may demonstrate insufficient sensitivity for the mild form or early detection of infections and for this reason, the result can be falsely negative. This study presents the results of employing thioglycolic acid capped CdTe quantum dots as a probe to enhance luminescence and subsequently detection sensitivity in LFIs for diagnosis of malaria. The chemical route synthesis of thioglycolic acid capped CdTe quantum dots was optimized systematically by probing optical properties of the quantum dots. These optimized quantum dots of thioglycolic acid capped CdTe have been conjugated with the anti-malaria antibodies against HRP2 protein (P. falciparum) and were then incorporated into LFIs. Further, an image processing code has been developed to carry out the quantification of malaria parasites in terms of the ratio on intensities of control and test lines on the LFIs. The results have been compared with those obtained using the standard, colloidal gold based LFIs. It has been demonstrated that sensitivity and lower detection limits of malaria under low parasite concentration increase significantly due to enhanced luminescence of control and test lines under UV light, owing to the presence of thioglycolic acid capped CdTe quantum dots. It has also been shown that the image processing based quantification of malaria will likely minimize the chances of false negative results under low parasite concentration and assist in early diagnosis of malaria.
Age peculiarities in the effect of stimulation of α2-adrenergic receptor on electrical activity of rat cardiomyocytes
Authors: Galieva A. M , Ziyatdinova N. I , Mansour N. , Fashutdinov L. I , Zefirov T. L
Published: April 2024

Clonidine hydrochloride, an agonist of the α2-adrenergic receptor, was tested for its effect on the parameters of the electrical activity of the atrial myocardium induced by pacing. In the experimental rat cardiomyocyte pacing model, clonidine hydrochloride caused a decrease (approximately 50% and 90%) in action potential duration in adult rats. Treatment of one- and three-week-old rats with this agonist led to an increase (around 50% and 90%) in action potential duration
Effect of α1-adrenoreceptors stimulation on electrical activity of rat atria
Authors: Mansour N. , Ziyatdinova N. I , Gallieva A. M , Shakirov R. R , Zefirov T. L
Published: April 2024

The effect of methoxamine, an agonist at α1-adrenergic receptors, on the frequency of spontaneous activity and parameters of the electrical activity of the atrial myocardium was investigated in rats with normal sinus rhythm and in normal rats under continuous electrical pacing. Methoxamine exerted dual effects on the duration of repolarization of working cardiomyocytes. Methoxamine increased the duration of the repolarization phase of the action potential in normal rats under continuous electrical pacing but decreased it in rats with normal sinus rhythm.
Effect of the nitric oxide synthesis inhibitor L-NAME on the isolated rat heart after hypokinesia
Authors: Sungatullina M. I , Zaripova R. I , Ziyatdinova N. I , Yafarova G. G , Andrianov V. V , Gainutdinov Kh. L , Zefirov T. L
Published: April 2024

The effects of a non-selective nitric oxide synthase inhibitor L-NAME on the functional parameters of the isolated rat heart after a 30-day period of hypokinesia were studied. Electron paramagnetic resonance spectroscopy was employed in the analysis of a role for L-NAME in the intensity of nitric oxide production in rat heart tissues. The intensity of nitric oxide synthesis was assessed by the intensity of the signal belonging to the (DETC)2-Fe2+-NO complex. It was found that L-NAME decreased nitric oxide production on average by 69%. The Langendorff isolated perfused heart was used to evaluate cardiac activity, and the following parameters were measured: pressure generated by the left ventricle, heart rate, and coronary flow. Addition of the nitric oxide synthesis inhibitor L-NAME induced an increase in inotropic function and normalization of heart rate.
Radio-mitigation properties of α-lipoic acid when used alone and in combination with metformin or ethylmethylhydroxypyridine succinate (mexidol) in mice after exposure to X-ray radiation
Authors: Karmanova E. E , Chernikov A. V , Usacheva A. M , Bruskov V. I
Published: April 2024

This study explored the radio-mitigation properties of α-lipoic acid and combination of α-lipoic acid with metformin and mexidol in animals during the process of X-ray irradiation. The results of the micronucleus test for measuring radiation-induced DNA damage of polychromatophilic red blood cells in the bone marrow of mice showed that α-lipoic acid has gene-protective and radio-mitigation properties in vivo. A study on the survival rate of the lethal dose-irradiated mice within 30 days confirmed that α-lipoic acid has radio-mitigation properties. The radio-mitigation effect of α-lipoic acid is dose-dependent, the effect increases with decreasing dose. α-lipoic acid in combination with mexidol and metformin exhibited a weaker radio-mitigation effect.