Некоторые аспекты участия экспертов и специалистов в производстве по уголовным делам в Республике Казахстан

The article considers particular reasons for the start of a pre-trial investigation, which are associated with the participation of persons having specialized knowledge in the proceedings.By using a number of methods of cognition of the circumstances of reality, the authors identify the issues that require resolution at the intersectoral level. Among the problematic aspects that cause the violation of citizens’ rights, there is a premature start of the pre-trial investigation, which is also due to the inconsistency and unreliability of the conclusions of experts and specialists involved both before and during the pre-trial investigation.To improve the studied sphere of public relations, proposals are made on overcoming of organizational and legal shortcomings of operational investigative activities, reasons for starting a pre-trial investigation, as well as filling the gaps in the current legislation, in terms of bringing experts and specialists to administrative and criminal responsibility.В статье рассматриваются отдельные поводы начала досудебного расследования, которые связаны с участием в производстве лиц, обладающих специальными либо специально научными знаниями.С применением ряда методов познания обстоятельств действительности авторы устанавливают вопросы, требующие разрешения на межотраслевом уровне. Среди проблемных аспектов, которые влекут нарушение прав граждан, отмечается преждевременное начало досудебного расследования, что также обусловлено несоответствием и недостоверностью заключений экспертов и специалистов, привлекаемых как до начала, так и в ходе проведения досудебного расследования.Для совершенствования исследуемой сферы общественных отношений вносятся предложения по организационно-правовым недостаткам оперативно-розыскной деятельности, поводам для начала досудебного расследования, а также пробелам действующего законодательства в части привлечения экспертов и специалистов к административной и уголовной ответственности

Nonthermal Emission from a Supernova Remnant in a Molecular Cloud

In evolved supernova remnants (SNRs) interacting with molecular clouds, such as IC 443, W44, and 3C391, a highly inhomogeneous structure consisting of a forward shock of moderate Mach number, a cooling layer, a dense radiative shell and an interior region filled with hot tenuous plasma is expected. We present a kinetic model of nonthermal electron injection, acceleration and propagation in that environment and find that these SNRs are efficient electron accelerators and sources of hard X- and gamma-ray emission. The energy spectrum of the nonthermal electrons is shaped by the joint action of first and second order Fermi acceleration in a turbulent plasma with substantial Coulomb losses. Bremsstrahlung, synchrotron, and inverse Compton radiation of the nonthermal electrons produce multiwavelength photon spectra in quantitative agreement with the radio and the hard emission observed by ASCA and EGRET from IC 443. We distinguish interclump shock wave emission from molecular clump shock wave emission accounting for a complex structure of molecular cloud. Spatially resolved X- and gamma- ray spectra from the supernova remnants IC 443, W44, and 3C391 as might be observed with BeppoSAX, Chandra XRO, XMM, INTEGRAL and GLAST would distinguish the contribution of the energetic lepton component to the gamma-rays observed by EGRET.Comment: 14 pages, 4 figure, Astrophysical Journal, v.538, 2000 (in press

Star formation in M33: Spitzer photometry of discrete sources

Combining the relative vicinity of the Local Group spiral galaxy M33 with the Spitzer images, we investigate the properties of infrared (IR) emission sites and assess the reliability of the IR emission as a star formation tracer. The mid- and far-IR emission of M33 was obtained from IRAC and MIPS images from the Spitzer archive. We compared the photometric results for several samples of three known types of discrete sources (HII regions, supernovae remnants and planetary nebulae) with theoretical diagnostic diagrams, and derived the spectral energy distribution (from 3.6 to 24 micron) of each type of object. Moreover, we generated a catalogue of 24 micron sources and inferred their nature from the observed and theoretical colours of the known type sources. We estimated the star formation rate in M33 both globally and locally, from the IR emission and from the Halpha emission line. The colours of the typical IR emissions of HII regions, supernovae remnants and planetary nebulae are continuous among the different samples, with overlapping regions in the diagnostic diagrams. The comparison between the model results and the colours of HII regions indicates a dusty envelope at relatively high temperatures ~600 K, and moderate extinction Av < 10. The 24 micron sources IR colours follow the regions observationally defined by the three classes of known objects but the majority of them represent HII regions. The derived total IR luminosity function is in fact very similar to the HII luminosity function observed in the Milky Way and in other late type spirals. Even though our completeness limit is 5x10^37 ergs s-1, in low density regions we are able to detect sources five times fainter than this, corresponding to the faintest possible HII region. [abridged]Comment: 19 pages, 18 figures (low resolution), accepted for publication by A&A; corrected typo

Game theory for computer games design

Designing and developing computer games can be a complex activity that may involve professionals from a variety of disciplines. In this article, we examine the use of game theory for supporting the design of game play within the different sections of a computer game, and demonstrate its application in practice via adapted high-level decision trees for modelling the flow in game play and payoff matrices for modelling skill or challenge levels

Galactic and Extragalactic Samples of Supernova Remnants: How They Are Identified and What They Tell Us

Supernova remnants (SNRs) arise from the interaction between the ejecta of a supernova (SN) explosion and the surrounding circumstellar and interstellar medium. Some SNRs, mostly nearby SNRs, can be studied in great detail. However, to understand SNRs as a whole, large samples of SNRs must be assembled and studied. Here, we describe the radio, optical, and X-ray techniques which have been used to identify and characterize almost 300 Galactic SNRs and more than 1200 extragalactic SNRs. We then discuss which types of SNRs are being found and which are not. We examine the degree to which the luminosity functions, surface-brightness distributions and multi-wavelength comparisons of the samples can be interpreted to determine the class properties of SNRs and describe efforts to establish the type of SN explosion associated with a SNR. We conclude that in order to better understand the class properties of SNRs, it is more important to study (and obtain additional data on) the SNRs in galaxies with extant samples at multiple wavelength bands than it is to obtain samples of SNRs in other galaxiesComment: Final 2016 draft of a chapter in "Handbook of Supernovae" edited by Athem W. Alsabti and Paul Murdin. Final version available at https://doi.org/10.1007/978-3-319-20794-0_90-

Dust in Historical Galactic Type Ia Supernova Remnants with Herschel

The origin of interstellar dust in galaxies is poorly understood, particularly the relative contributions from supernovae and the cool stellar winds of low-intermediate mass stars. Here, we present Herschel PACS and SPIRE photometry at 70-500um of the historical young supernova remnants: Kepler and Tycho; both thought to be the remnants of Type Ia explosion events. We detect a warm dust component in Kepler's remnant with T = 82K and mass 0.0031Msun; this is spatially coincident with thermal X-ray emission optical knots and filaments, consistent with the warm dust originating in the circumstellar material swept up by the primary blast wave of the remnant. Similarly for Tycho's remnant, we detect warm dust at 90K with mass 0.0086Msun. Comparing the spatial distribution of the warm dust with X-rays from the ejecta and swept-up medium, and Ha emission arising from the post-shock edge, we show that the warm dust is swept up interstellar material. We find no evidence of a cool (25-50 K) component of dust with mass >0.07Msun as observed in core-collapse remnants of massive stars. Neither the warm or cold dust components detected here are spatially coincident with supernova ejecta material. We compare the lack of observed supernova dust with a theoretical model of dust formation in Type Ia remnants which predicts dust masses of 0.088(0.017)Msun for ejecta expanding into surrounding densities of 1(5)cm-3. The model predicts that silicon- and carbon-rich dust grains will encounter the interior edge of the observed dust emission at 400 years confirming that the majority of the warm dust originates from swept up circumstellar or interstellar grains (for Kepler and Tycho respectively). The lack of cold dust grains in the ejecta suggests that Type Ia remnants do not produce substantial quantities of iron-rich dust grains and has important consequences for the 'missing' iron mass observed in ejecta.Comment: 17 pages, 14 figures, accepted for publication in MNRAS, final version including corrected typos and reference

Dust in Supernovae and Supernova Remnants I : Formation Scenarios

Supernovae are considered as prime sources of dust in space. Observations of local supernovae over the past couple of decades have detected the presence of dust in supernova ejecta. The reddening of the high redshift quasars also indicate the presence of large masses of dust in early galaxies. Considering the top heavy IMF in the early galaxies, supernovae are assumed to be the major contributor to these large amounts of dust. However, the composition and morphology of dust grains formed in a supernova ejecta is yet to be understood with clarity. Moreover, the dust masses inferred from observations in mid-infrared and submillimeter wavelength regimes differ by two orders of magnitude or more. Therefore, the mechanism responsible for the synthesis of molecules and dust in such environments plays a crucial role in studying the evolution of cosmic dust in galaxies. This review summarises our current knowledge of dust formation in supernova ejecta and tries to quantify the role of supernovae as dust producers in a galaxy.Peer reviewe

Assessment of bioclimatic change in Kazakhstan, end 20th—middle 21st centuries, according to the PRECIS prediction

We evaluate bioclimatic changes in Kazakhstan from the end of the 20th century until the middle of the 21st century to offer natural resource managers a tool that facilitates their decision-making on measures to adapt agriculture and environmental care to foreseeable climate change. We use climatic data from the “Providing REgional Climates for Impact Studies” (PRECIS) prediction and study them following the Worldwide Bioclimatic Classification System (WBCS) of Rivas-Martı´nez. For three 25-year intervals (1980–2004, 2010–2034 and 2035–2059), we identify the continentality, acrobioclimates, bioclimates, bioclimatic variants, thermotypes, ombrotypes and isobioclimates of the study area. The results of the work allow us to: locate the territories where bioclimatic conditions will change, quantify the magnitude of the predicted climate changes, and determine the trends of predictable climate change. We present the results in maps, tables and graphs. For the 80-year interval, we identify 3 macroclimates, 3 bioclimatic variants, 10 bioclimates, 11 thermotypes, 10 ombrotypes and 43 isobioclimates. Some of those found bioclimates, thermotypes, ombrotypes and isobioclimates are only located in the E, SE and S mountains, where they occupy very small areas, that decrease in a generalized way as the 20th century progresses. Comparing the three successive periods, the following trends are observed: 36.2% of the territory increases in thermicity; 7.3% of the territory increases in continentality; 9.7% of the territory increases in annual aridity; 9.5% of the territory increases in summer aridity or mediterraneity; and generalized losses occur in the areas of all mountain sobioclimates. The climate change foreseen by the PRECIS model for the middle of the 21st century leads to bioclimatic homogenization, with 20.8% losses in bioclimatic diversity. We indicate on maps the locations of all the predicted bioclimatic changes; these maps may provide decision makers with a scientific basis to take necessary adaptation measures

The influence of the synergistic anion on iron chelation by ferric binding protein, a bacterial transferrin

Although the presence of an exogenous anion is a requirement for tight Fe(3+) binding by the bacterial (Neisseria) transferrin nFbp, the identity of the exogenous anion is not specific in vitro. nFbp was reconstituted as a stable iron containing protein by using a number of different exogenous anions [arsenate, citrate, nitrilotriacetate, pyrophosphate, and oxalate (symbolized by X)] in addition to phosphate, predominantly present in the recombinant form of the protein. Spectroscopic characterization of the Fe(3+)/anion interaction in the reconstituted protein was accomplished by UV-visible and EPR spectroscopies. The affinity of the protein for Fe(3+) is anion dependent, as evidenced by the effective Fe(3+) binding constants (K′(eff)) observed, which range from 1 × 10(17) M(−1) to 4 × 10(18) M(−1) at pH 6.5 and 20°C. The redox potentials for Fe(3+)nFbpX/Fe(2+)nFbpX reduction are also found to depend on the identity of the synergistic anion required for Fe(3+) sequestration. Facile exchange of exogenous anions (Fe(3+)nFbpX + X′ → Fe(3+)nFbpX′ + X) is established and provides a pathway for environmental modulation of the iron chelation and redox characteristics of nFbp. The affinity of the iron loaded protein for exogenous anion binding at pH 6.5 was found to decrease in the order phosphate > arsenate ∼ pyrophosphate > nitrilotriacetate > citrate ∼ oxalate ≫ carbonate. Anion influence on the iron primary coordination sphere through iron binding and redox potential modulation may have in vivo application as a mechanism for periplasmic control of iron delivery to the cytosol