Epistemological risk aspects

The paper considers risk in the context of the main characteristics of non-classical epistemology. It states that non-classical epistemology is characterized by transformation, according to which the major priority of cognitive activity shifts the focus from the present to the past. In this situation a subject is keen not on what he or she has learnt but on what can be learnt. Truth being a crucial criterion of scientific knowledge is becoming of less priority, while risk is becoming more and more significant and acts as one of the major epistemology measurements. Risk is gaining the status of epistemological phenomenon, which shows a growing degree of uncertainty as a cognitive process background and the necessity for a subject to learn the world (make decisions) under the conditions of uncertainty degree strengthening. The author states that risk is a comprehensive notion and it obtains a base value for all other aspects of its application, specifically, in the role of epistemological phenomenon

Star formation around the H II region Sh2-235

We present a picture of star formation around the H ii region Sh2-235 (S235) based upon data on the spatial distribution of young stellar clusters and the distribution and kinematics of molecular gas around S235. We observed 13CO (1-0) and CS (2-1) emission toward S235 with the Onsala Space Observatory 20-m telescope and analysed the star density distribution with archival data from the Two Micron All-Sky Survey (2MASS). Dense molecular gas forms a shell-like structure at the southeastern part of S235. The young clusters found with 2MASS data are embedded in this shell. The positional relationship of the clusters, the molecular shell and the H ii region indicates that expansion of S235 is responsible for the formation of the clusters. The gas distribution in the S235 molecular complex is clumpy, which hampers interpretation exclusively on the basis of the morphology of the star-forming region. We use data on kinematics of molecular gas to support the hypothesis of induced star formation, and distinguish three basic types of molecular gas components. The first type is primordial undisturbed gas of the giant molecular cloud, the second type is gas entrained in motion by expansion of the H ii region (this is where the embedded clusters were formed) and the third type is a fast-moving gas, which might have been accelerated by winds from the newly formed clusters. The clumpy distribution of molecular gas and its kinematics around the H ii region implies that the picture of triggered star formation around S235 can be a mixture of at least two possibilities: the 'collect-and-collapse' scenario and the compression of pre-existing dense clumps by the shock wave. Journal compilation © 2008 RAS

Star formation around the H II region Sh2-235

We present a picture of star formation around the H ii region Sh2-235 (S235) based upon data on the spatial distribution of young stellar clusters and the distribution and kinematics of molecular gas around S235. We observed 13CO (1-0) and CS (2-1) emission toward S235 with the Onsala Space Observatory 20-m telescope and analysed the star density distribution with archival data from the Two Micron All-Sky Survey (2MASS). Dense molecular gas forms a shell-like structure at the southeastern part of S235. The young clusters found with 2MASS data are embedded in this shell. The positional relationship of the clusters, the molecular shell and the H ii region indicates that expansion of S235 is responsible for the formation of the clusters. The gas distribution in the S235 molecular complex is clumpy, which hampers interpretation exclusively on the basis of the morphology of the star-forming region. We use data on kinematics of molecular gas to support the hypothesis of induced star formation, and distinguish three basic types of molecular gas components. The first type is primordial undisturbed gas of the giant molecular cloud, the second type is gas entrained in motion by expansion of the H ii region (this is where the embedded clusters were formed) and the third type is a fast-moving gas, which might have been accelerated by winds from the newly formed clusters. The clumpy distribution of molecular gas and its kinematics around the H ii region implies that the picture of triggered star formation around S235 can be a mixture of at least two possibilities: the 'collect-and-collapse' scenario and the compression of pre-existing dense clumps by the shock wave. Journal compilation © 2008 RAS

The link between gas and stars in the S254-S258 star-forming region

The paper aims to study relation between the distributions of the young stellar objects (YSOs) of different ages and the gas-dust constituents of the S254-S258 star formation complex. This is necessary to study the time evolution of the YSO distribution with respect to the gas and dust compounds that are responsible for the birth of the young stars. For this purpose, we use correlation analysis between different gas, dust, and YSO tracers. We compared the large-scale CO, HCO+, near-IR extinction, and far-IR Herschel maps with the density of YSOs of the different evolutionary classes. The direct correlation analysis between these maps was used together with the wavelet-based spatial correlation analysis. This analysis reveals a much tighter correlation of the gas-dust tracers with the distribution of class I YSOs than with that of class II YSOs. We argue that class I YSOs that were initially born in the central bright cluster S255-IR (both N and S parts) during their evolution to class II stage (similar to 2 Myr) had enough time to travel through the whole S254-S258 star formation region. Given that the region contains several isolated YSO clusters, the evolutionary link between these clusters and the bright central S255-IR (N and S) cluster can be considered. Despite the complexity of the YSO cluster formation in the non-uniform medium, the clusters of class II YSOs in the S254-258 star formation region can contain objects born in the different locations of the complex.Peer reviewe

Unmanned aerial vehicles: potential for use in the storage systems of industrial companies

In the article, the authors investigate the problem of using unmanned aerial vehicles (drones) in company warehouses and consider their use as one of the ways to optimize the logistics business processes of companies. Technologies are considered, on the basis of which modern unmanned aerial vehicles, drone models of various companies, the main functionality of drone’s work. The authors high-light the strengths and weaknesses of unmanned aerial vehicles, key factors determining the success of the use of drones, and favorable conditions for their use in warehouses. The authors are considering the possibility of sharing drones and RFID technology. Barriers to the active introduction of drones into the logistics business processes of warehousing systems and requirements for warehouse complexes planning the use of unmanned aerial objects have been identified. Promising areas of application of technology in warehouse logistics are also considered: creation of anti-theft and fire protection systems, using drones to read CIS marks. The authors used data from analytical reports and data collected by the authors themselves, as well as empirical research methods

The Link between Gas and Stars in the S254-S258 Star-forming Region

The paper aims to study relation between the distributions of the young stellar objects (YSOs) of different ages and the gas-dust constituents of the S254-S258 star formation complex. This is necessary to study the time evolution of the YSO distribution with respect to the gas and dust compounds that are responsible for the birth of the young stars. For this purpose, we use correlation analysis between different gas, dust, and YSO tracers. We compared the large-scale CO, HCO+, near-IR extinction, and far-IR Herschel maps with the density of YSOs of the different evolutionary classes. The direct correlation analysis between these maps was used together with the wavelet-based spatial correlation analysis. This analysis reveals a much tighter correlation of the gas-dust tracers with the distribution of class I YSOs than with that of class II YSOs. We argue that class I YSOs that were initially born in the central bright cluster S255-IR (both N and S parts) during their evolution to class II stage (∼2 Myr) had enough time to travel through the whole S254-S258 star formation region. Given that the region contains several isolated YSO clusters, the evolutionary link between these clusters and the bright central S255-IR (N and S) cluster can be considered. Despite the complexity of the YSO cluster formation in the non-uniform medium, the clusters of class II YSOs in the S254-258 star formation region can contain objects born in the different locations of the complex. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.The work of DAL and SAK on correlation analysis in Section 4 was supported by the Russian Science Foundation (RSF) grant 19-72-10012. The work of MSK in the Section 2.1 was supported by the Russian Foundation for Basic Research (RFBR) grant 20-02-00643. The work by DAL in Section 3 was supported by the Russian Ministry of Science and Higher Education, No. FEUZ-2020-0030. The work of AMS in Section 5 was supported by the Large Scientific Project of the Russian Ministry of Science and Higher Education 'Theoretical and experimental studies of the formation and evolution of extrasolar planetary systems and characteristics of exoplanets' (No. 075-15-2020-780, contract 780-10). VO was supported by the Collaborative Research Centre 956, sub-project C1, funded by the Deutsche Forschungsgemeinschaft (DFG), project ID 184018867. The authors acknowledges support from Onsala Space Observatory for the provisioning of its facilities/observational support. The Onsala Space Observatory national research infrastructure is funded through Swedish Research Council grant No. 2017-00648

ИЗУЧЕНИЕ КОЛЛЕКЦИИ АРБУЗА И ДЫНИ ОТЕЧЕСТВЕННОЙ СЕЛЕКЦИИ В УСЛОВИЯХ ЮЖНОЙ ЗОНЫ АМУРСКОЙ ОБЛАСТИ

Melon crops have long been non-traditional crops in the Amur region, being grown in small quantities in household plots, while the climatic conditions of Southern Priamurie are favorable for their large-scale cultivation. The results of the study of 10 samples of watermelon and 4 samples of melons of domestic selection in the conditions of the southern zone of Amurskaya Oblast are presented. According to the evaluation of the collection, 7 samples of watermelon are selected: Start, Graal F1, Fronder, Vektor, Skorik, Rapid, Foton, and 2 samples of melon: Alisa F1 and Lolita. They are characterized by sufficiently early ripeness, high and stable yield of marketable fruits of good taste. These varieties and hybrids are promising for cultivation in the south of Amurskaya Oblast. The characteristics of these varieties are summarized and recommendations for their cultivation are offered.В Амурской области бахчевые культуры долгое время являлись нетрадиционными и произрастали в небольших количествах на приусадебных участках, хотя климатические условия южной зоны Амурской области благоприятны для их массового выращивания. Представлены результаты изучения 10 образцов арбуза и 4 образцов дыни отечественной селекции в условиях данной зоны Амурской области. По результатам оценки коллекции выделены 7 образцов арбуза: Старт, Грааль F1, Фрондер, Вектор, Скорик, Рапид, Фотон и 2 образца дыни: Алиса F1 и Лолита. Они отличаются достаточной скороспелостью, высоким выходом товарных плодов хороших вкусовых качеств и стабильной урожайностью. Эти сорта и гибриды являются перспективными для выращивания в условиях юга Амурской области. Составлена характеристика данных сортов и представлены рекомендации по их выращиванию.

Physical parameters of molecular clumps in the S254—S258 star formation region

Работа посвящена исследованию физических параметров газопылевых сгустков в области звездообразования S254—S258. Были определены лучевые концентрации молекулярного газа, массы сгустков и оптические толщины линий-трассеров плотного газа. Для вычисления физических параметров использованы различные линии молекулы CO, излучение в континууме на 1.1 мм и карты поглощения в ближнем ИК-диапазоне. Дополнительно использованы данные по излучению молекул CS и HCO+, охватывающие часть изучаемой области. В работе сделаны выводы о распределении плотного газа в области звездообразования. Значения физических параметров, полученных в разных трассерах газа и пыли, имеют различия, причины которых рассмотрены в работе.This research is focusing on studying of physical parameters in the S254—S258 star-formation complex. The following parameters were derived: column densities, clump masses, and highdensity tracers optical depth, including CS and HCO+ molecules. Different gas and dust tracers maps were used, including CO molecular lines, Bolocam 1.1 mm continuum emission and near-infrared extinction map. We also used the available CS and HCO+ data, which cover part of the S254-S258 region to make conclusions regarding the distribution of highdensity gas. The resulted values of physical parameters obtained through different tracers are slightly different. The discussion about the possible reason for the difference is provided.Работа выполнена при поддержке гранта РФФИ №18-02-00917

The simulation of molecular clouds formation in the Milky Way

Using 3D hydrodynamic calculations we simulate formation of molecular clouds in the Galaxy. The simulations take into account molecular hydrogen chemical kinetics, cooling and heating processes. Comprehensive gravitational potential accounts for contributions from the stellar bulge, two and four armed spiral structure, stellar disk, dark halo and takes into account self-gravitation of the gaseous component. Gas clouds in our model form in the spiral arms due to shear and wiggle instabilities and turn into molecular clouds after t\simgt 100 Myr. At the times $t\sim 100 - 300$ Myr the clouds form hierarchical structures and agglomerations with the sizes of 100 pc and greater. We analyze physical properties of the simulated clouds and find that synthetic statistical distributions like mass spectrum, "mass-size" relation and velocity dispersion are close to those observed in the Galaxy. The synthetic $l-v$ (galactic longitude - radial velocity) diagram of the simulated molecular gas distribution resembles observed one and displays a structure with appearance similar to Molecular Ring of the Galaxy. Existence of this structure in our modelling can be explained by superposition of emission from the galactic bar and the spiral arms at $\sim$3-4 kpc.Comment: 10 pages, 8 figure