Ways to increase the efficiency of solar panels operating in isolated power supply systems

Abstract To cool solar panels in hot season, it is necessary to use special cooling devices. The most optimal way of cooling is the use of liquid cooling, realized by means of a pump. This article provides an overview and evaluation of ways to cool solar panels using various devices. The relevance of the research is caused by the need to reduce the temperature of solar panels in order to increase the output power in the hot season. The main aim of the research is to compare and choose the most optimal way to cool solar panels. Methods: comparative analysis, mathematical modeling in the ANSYS environment. Results. Comparative characteristic of TEM, radiators, fans and liquid cooling is given, an example of cooling a solar panel using liquid cooling to spray a liquid flow of 29 l/min is calculated. The panels will cool down from 45 to 35 °C in 4,7 minutes. For one EasySunSolar solar panel with a capacity of 100 W, costing $100, taking into account electrical work, an additional heat sink module will cost about$50

Additional spectroscopic redshift measurements for galaxy clusters from the First Planck Catalogue

We present the results of spectroscopic redshift measurements for the galaxy clusters from the first all-sky Planck catalogue of the Sunyaev-Zeldovich sources, that have been mostly identified by means of the optical observations performed previously by our team (Planck Collaboration, 2015a). The data on 13 galaxy clusters at redshifts from z=~0.2 to z=~0.8, including the improved identification and redshift measurement for the cluster PSZ1 G141.73+14.22 at z=0.828, are provided. The measurements were done using the data from Russian-Turkish 1.5-m telescope (RTT-150), 2.2-m Calar Alto Observatory telescope, and 6-m SAO RAS telescope (Bolshoy Teleskop Azimutalnyi, BTA).Comment: published in Astronomy Letter

Observations of GRB 060526 Optical Afterglow with Russian-Turkish 1.5-m Telescope

We present the results of the photometric multicolor observations of GRB 060526 optical afterglow obtained with Russian-Turkish 1.5-m Telescope (RTT150, Mt. Bakirlitepe, Turkey). The detailed measurements of afterglow light curve, starting from about 5 hours after the GRB and during 5 consecutive nights were done. In addition, upper limits on the fast variability of the afterglow during the first night of observations were obtained and the history of afterglow color variations was measured in detail. In the time interval from 6 to 16 hours after the burst, there is a gradual flux decay, which can be described approximately as a power law with an index of -1.14+-0.02. After that the variability on the time scale \delta t < t is observed and the afterglow started to decay faster. The color of the afterglow, V-R=~0.5, is approximately the same during all our observations. The variability is detected on time scales up to \delta t/t =~ 0.0055 at \Delta F_\nu/F_\nu =~ 0.3, which violates some constraints on the variability of the observed emission from ultrarelativistic jet obtained by Ioka et al. (2005). We suggest to explain this variability by the fact that the motion of the emitting shell is no longer ultrarelativistic at this time.Comment: 6 pages, 7 figures, Astronomy Letters, 2007, 33, 797, The on-line data tables and the original text in Russian can be found at http://hea.iki.rssi.ru/grb/060526/indexeng.htm

First hours of the GRB 030329 optical afterglow

We present the first results of the observations of the extremely bright optical afterglow of gamma-ray burst (GRB) 030329 with the 1.5m Russian-Turkish telescope RTT150 (TUBITAK National Observatory, Bakyrlytepe, Turkey). RTT150 was one of the first 1.5m-class telescopes pointed to the afterglow. Observations were started approximately 6 hours after the burst. During the first 5 hours of our observations the afterglow faded exactly as a power law with index -1.19+-0.01 in each of the BVRI Bessel filters. After that, in all BVRI filters simultaneously we observe a steepening of the power law light curve. The power law decay index smoothly approaches the value ~= -1.9, observed by other observatories later. This power law break occurs at t-t_0 =0.57 days and lasts for +-0.1 days. We observe no variability above the gradual fading with the upper limits 10--1% on time scales 0.1--1000s. Spectral flux distribution in four BVRI filters corresponds to the power law spectrum with spectral index \alpha=0.66+-0.01. The change of the power law decay index in the end of our observations can be interpreted as a signature of collimated ultrarelativistic jet. The afterglow flux distribution in radio, optical and x-rays is consistent with synchrotron spectrum. We continue our observations of this unique object with RTT150.Comment: Astronomy Letters, Vol. 29, No. 9, p. 573; 6 pages, 5 figures; pagination corrected; the original Russian version can be found at http://hea.iki.rssi.ru/~br/030329/pfh030329.pd

Validation of a test procedure for determination of specific activity of human recombinant interferon beta (Infibeta®) using various cell/virus combinations

Interferon beta preparations have demonstrated efficacy in the treatment of multiple sclerosis. One of the most important quality attributes that support efficacy and safety of interferon beta preparations is specific antiviral activity. Interferon beta activity is determined by the biological test method which can lead to an erroneous final result due to the system uncertainties that contribute to the overall uncertainty. Accurate assessment of specific activity plays an important role in adequate determination of the product’s therapeutic dose, therefore the test method standardisation and validation are of particular relevance. The aim of the study was to validate a test procedure for assessing specific activity of human recombinant interferon beta preparations, using various cell/virus combinations, as illustrated by the example of Infibeta®. Materials and methods: WISH, Vero, A-549, and MDBK cells in combination with mouse encephalomyocarditis virus were used in the study. The testing was performed using the biological test method based on the interferon ability to suppress virus-induced cytopathic effects in cell cultures. The results were processed using methods of mathematical statistics and the GraphPadPrism, Statistical 2/0 software package. Results: the paper compares the results of specific activity determination of Infibeta® (interferon beta-1b) using various cell/virus combinations. The dose-response curves were used to compare the test results. It was demonstrated that all the tested cell lines could be used in the biological test procedure for determination of interferon beta specific activity. However, the best results were obtained with A-549, WISH cells in combination with mouse encephalomyocarditis virus. The following validation characteristics were determined in the cell/virus systems: specificity, linearity, precision, and robustness. Conclusions: the study validated the test procedure that enables measurement of interferon beta specific activity in the range of 4.8–11.2 IU/mL at a satisfactory accuracy level, which guarantees reliable test results. The study demonstrated robustness, intermediate precision, and reproducibility of the test procedure

New integrable extension of the Hubbard chain with variable range hopping

New integrable variant of the one-dimensional Hubbard model with variable-range correlated hopping is studied. The Hamiltonian is constructed by applying the quantum inverse scattering method on the infinite interval at zero density to the one-parameter deformation of the L-matrix of the Hubbard model. By construction, this model has Y(su(2))$\oplus$Y(su(2)) symmetry in the infinite chain limit. Multiparticle eigenstates of the model are investigated through this method.Comment: 25 pages, LaTeX, no figure

Photometry and spectroscopy of IGR J21247+5058 radiogalaxy with RTT150

We present the results of photometry and spectroscopy of IGR J21247+5058 made by using the 1.5-m optical telescope RTTl50 with Andor CCD and TFOSC instrument. R-band images obtained at 0.8 arcsec seeing conditions have allowed us to separate foreground star from point-like extragalactic source and estimate their brightness separately. Low-resolution but high S/N ratio spectra of this optically combined source confirm the presence of red-shifted H-alpha emission line of extragalactic nature. Physical properties of radio-galaxy are briefly discussed

Observations of the optical afterglow from GRB 060526 with the RTT-150 telescope

Multicolor photometric observations of the optical afterglow from GRB 060526 with the Russian-Turkish 1.5-m RTT-150 telescope (Mount Bakyrlytepe, Turkey) are presented. The afterglow light curve was measured in detail starting from about 5 h after the GRB and over five ensuing nights. In addition, upper limits were obtained on the rapid variability of the afterglow on the first night of observations and the history of afterglow color variations was measured in detail. In the time interval from 6 to 16 h after the burst, the flux gradually decreased approximately as a power law with a slope of -1.14 ± 0.02. Subsequently, variability was observed on a time scale δt < t and the afterglow began to decay much faster. The afterglow color was approximately constant (V-R ≈ 0.5) throughout the observations, despite the flux variability. Variability time scales up to δt/t ≈ 0.0055 were observed at ΔF ν/F ν ≈ 0.3, which violates many constraints on the variability of the observed emission from an ultrarelativistic jet obtained by Ioka et al. (2005). We suggest explaining this variability by the fact that the shell motion is no longer ultrarelativistic at this time. © 2007 Pleiades Publishing, Inc

An experience of scaling and intensifying the industrial production of the Gam-COVID-Vac vector adenovirus vaccine in the limiting conditions of the pandemic

The COVID-19 pandemic has presented a global challenge to the health system. More than 200 years of world epidemiological experience since the first mass use of vaccines have convincingly shown that effective vaccines are the key tools in the fight against dangerous infectious diseases, especially epidemic and pandemic ones. In the context of a rapidly spreading pandemic of a new infectious agent, it is crucial not only to develop fundamentally new vaccines, but also to be able to quickly organise their large-scale production. In the Russian Federation, in 2020, a team of the National Research Centre for Epidemiology and Microbiology named after Honorary Academician N.F. Gamaleya developed an innovative vector vaccine, Gam-COVID-Vaс, for the prevention of coronavirus disease caused by the SARS-CoV-2 virus. A number of pharmaceutical companies faced the challenge of producing the vaccine. The aim of the study was to optimise the production technology of Gam-COVID-Vac for scaling and increasing the production capacity. In the course of the work, the authors established critical quality attributes of the product, optimised analytical methods for their control, identified poorly scalable technological stages, streamlined the technological process before its transfer to production, and modified non-scalable and technologically unfeasible stages. The work resulted in the launch of industrial-scale production of active pharmaceutical ingredients for both components of Gam-COVID-Vac, which made it possible not only to meet the critical need for COVID-19 immunoprophylaxis in the Russian Federation, but also to supply this vaccine to a number of foreign countries

Type Ia supernovae 2014J and 2011fe at the nebular phase

© 2015, Pleiades Publishing, Inc. We present our observations and the results of our analysis of the nebular spectra for two nearby type Ia supernovae (SN 2014J and SN 2011fe). For the overall picture, we have analyzed the nebular spectra of four other type Ia supernovae. All of the investigated supernovae show evidence of a significant shift in the [Co III], [Fe III], [Fe II], and [Ni II] lines (~103 km s−1) at a late nebular phase (t ~ 250−300 days). The shifts in the lines of singly and doubly ionized species differ noticeably, suggesting a difference of the departures from symmetry in the inner and outer ejecta. In SN 2014J, the [Fe III] and [Fe II] line shifts are comparable in absolute value and opposite in sign. This means that the shift in the centroid of the 56Ni distribution is probably small compared to the width of the velocity distribution. The [Ni II]/[Fe II] flux ratio for the six supernovae suggests that, on average, the 58Ni/56Fe ratio for SNe Ia is nearly solar, in agreement with the dominant contribution of SNe Ia to the galactic synthesis of iron-peak elements. The nebular spectra of SN 2014J and SN 2011fe are shown to rule out the presence of stripped hydrogen from the normal companion in the amount predicted by the scenario of a binary system with a normal companion