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The whole world has battled with multiple waves of coronavirus disease 2019 (COVID-19) pandemic caused by severe acute respiratory syndrome coronavirus 2 virus. However, the second wave of COVID-19 had caused a worldwide havoc in terms of disease transmissibility, severity, and mortality. India has been among the worst hit countries during the second wave, which substantially overburdened and overwhelmed the Indian health care system. While secondary infections and co-infections among COVID-19 patients were increasingly being reported, COVID-19-associated mucormycosis (CAM) emerged as a new challenge particularly from India and became a matter of immediate concern. The most common causes attributed to the rise of CAM were undiagnosed/uncontrolled diabetes mellitus, excessive use of corticosteroids, and prolonged hospital stay, all of which create a perfect environment for mucormycosis infection to set in. [ABSTRACT FROM AUTHOR]

The whole world has battled with multiple waves of coronavirus disease 2019 (COVID-19) pandemic caused by severe acute respiratory syndrome coronavirus 2 virus. However, the second wave of COVID-19 had caused a worldwide havoc in terms of disease transmissibility, severity, and mortality. India has been among the worst hit countries during the second wave, which substantially overburdened and overwhelmed the Indian health care system. While secondary infections and co-infections among COVID-19 patients were increasingly being reported, COVID-19-associated mucormycosis (CAM) emerged as a new challenge particularly from India and became a matter of immediate concern. The most common causes attributed to the rise of CAM were undiagnosed/uncontrolled diabetes mellitus, excessive use of corticosteroids, and prolonged hospital stay, all of which create a perfect environment for mucormycosis infection to set in.

Applies the philosophy of Georg Wilhelm Friedrich Hegel to The Violet Apple, a posthumously published novel by David Lindsay, whose A Voyage to Arcturus is frequently cited as an influence on Lewis's Out of the Silent Planet. [ABSTRACT FROM AUTHOR]

This publication presents the results of two studies of astroarchaeological monuments in North Khakassia confirming the existence of Siberia stellar astronomy in the Bronze age (andronovo culture, Khakassia, mid-II millennium BC). It is proved that in the study area ("Sunduki") Arcturus - the brightest star in the northern sky - was purposefully observed in conjunction with the stars of the Orion constellation (in particular Betelgeuse - the brightest star of the constellation). In both investigated monuments of the Bronze Age were found man-made objects specifying astronomically important areas - a kind of tools to monitor these stars. Because there is no any written source the observed stars and epoch of observation were identified by geodetic measurements and astronomical calculations. This era is XIV-XIII centuries BC which corresponds to the archaeological dating of these objects defined in terms of style and semantics of petroglyphic images marking astronomically significant azimuths. The work confirms the hypothesis of tracking the heliacal and acronycal passages of Arcturus by Andronov priests (the first in the morning and the last in the night) in predetermined directions. Arcturus was observed by priests to determine the winter solstice, the middle of the spring and summer seasons. This revealed the specifications of observing of the heliacal and acronychal passages of stars with a naked eye such as a weakening of the apparent brightness of stars near the horizon at dusk and full moon, as well as the loss of light depending on the angular distance from the sun. Because of these features the first and the last star passages of the year through a given direction can be observed in the time interval up to ten days. The conclusion about the features of the observation of Arcturus by andronovo culture priests confirms and explains the perfection and precision of their lunar-solar calendar systems revised in such a way from the observations of the stars. No less important was the fact that figuring out a direct connection of different types of okunev and andronovo anthropomorphic petroglyphs with astronomically significant directions. This allows us to judge more reliably the semantics of certain images of okunev and andronovo cultures. Due to the fact that until recently Arcturus took a very important place in the astral mythology of indigenous peoples of Siberia the problem of reconstruction of stellar components of andronovo mythology in Khakassia becomes more perspective to solve. The obtained results allow us to consider the whole astronomical dating from observations of stars as a reliable and highly accurate (+- 50 years) instrument of ancient man-made structures' dating which was used with different cultures in the cult practice of astronomical observations.

The treasure of Aliseda was discovered by chance in the place of El Ejido ninety five years ago. However, the eventful character of the discovery and the circumstances that wrapped it left without answer multiple questions and, among them the archeological context where the emplacement belongs. The ritual building (6th century BC), found and excavated about 180 m away, is associated to the protohistoric settlement of La Sierra del Aljibe, and not only does it show a simple metric and geometry, but fascinating as well, beside incorporating a singular element, which until now remains unknown if exist any parallel within any contemporary construction in the territory. We are alluding to the vertical opening in the center of the most northern wall, and that allow to define a precise orientation. On a hand, it's been verified the use of a measurement unit based upon the human foot, in which there has been in use a foot of 0.275 m. On the other hand, the building is totally unoccupied, without any archaeological findings that indicates the execution of any activity, and with an elegant soil of red clay, which it proportionality is 2:1. Finally, as a fundamental characteristic, the NNE direction of it's main axis, and without any remarkable topographic element in whole the northern horizon, which aims, with a stunning precision, to the place in the horizon in which Arcturus rised in the time of the construction. It could be possible to affirm that the constructors would look for in this astral direction for the announcement of the spring equinox when it is possible to verify the apparent Heliacal rising of Arcturus some days before this moment of the year. Added to this astral direction, another astronomical situation is verified. It's dimensions, the propose opening in the Northern wall and it's orientations, cause that the sunrays never enter to the opposite wall. Only in the most northern positions of the Sunrise, summer solstice, the sunlight enters across the opening to leave in the right shade the opposite wall. [ABSTRACT FROM AUTHOR]

Abundance of iron in the atmosphere of Arcturus has been determined from the profiles or regions of the profiles of the weak lines sensitive to iron abundance. The selected lines of Fe I and Fe II were synthesized with the MARCS theoretical models of the atmosphere. From the observed profiles of lines available with a high spectral resolution in the atlas by Hinkle and Wallace (2005), the values of the iron abundance A = 6.95 ± 0.03 and the radial-tangential macroturbulent velocity 5.6 ± 0.2 km/s were obtained for Arcturus. The same physical quantities were found for the Sun as a star; they are 7.42 ± 0.02 and 3.4 ± 0.3 km/s, respectively. For Arcturus, the iron abundance relative to the solar one was determined with the differential method as [Fe/H] =-0.48 ± 0.02. [ABSTRACT FROM AUTHOR]

The article offers the author's insights on Boötes constellation, which stretches from Draco to Virgo constellations. Topics discussed include the constellation is home to various galaxies, as well as galaxy clusters, the Arcturus group of stars, and the NGC 5466 is a globular cluster in the constellation Boötes.

The wide range of results of demand response initiatives has led some observers to conclude that we still don’t know whether customers respond to DR. However, an analysis of the Arcturus database of dynamic pricing and time-of-use pricing studies finds that much of the discrepancy in results goes away when DR is expressed as a function of the peak to off-peak price ratio, and that customers do indeed respond to rising prices by lowering their peak demand in a consistent fashion. This supports the case for rollout of dynamic pricing wherever advanced metering infrastructure is in place. [ABSTRACT FROM AUTHOR]

A brief overview of the results of the study of the red giant Arcturus is given. One-dimensional LTE modeling of the atmospheres of Arcturus and the Sun as a star is carried out on the basis of calculation of the extended wings of the H and K Ca II lines. It is found that the local continuum in this spectral region is underestimated by an average of 12% in the atlases of Arcturus. The average deficit in UV absorption amounts to 43% (Arcturus) and 9% (the Sun). The correction factor to the opacity in continuum for the wavelengths of 390.0, 392.5, 395.0, 398.0, and 400.0 nm equals 2.20, 1.90, 1.70, 1.55, and 1.45 (Arcturus) and 1.20, 1.20, 1.20, 1.17, and 1.15 (the Sun), respectively. Model calculations agree completely with the estimates of the parameters of the Arcturus atmosphere ( T = 4286 K and log g = 1.66) and the elemental abundances that were presented by Ramirez and Allende Prieto [56]. The obtained model of the atmosphere of Arcturus is presented in tabular form. [ABSTRACT FROM AUTHOR]

Context. We re-analyzed the carbon and oxygen isotopic ratios in the atmospheres of the two bright K giants Arcturus (α Boo) and Aldebaran (α Tau). Aims. These stars are in the evolutionary stage following the first dredge-up (FDU). Previous determinations (dating back more than 20 years) of their 16O/18O ratios showed a rough agreement with FDU expectations; however, the estimated 16O/17O and 12C/13C ratios were lower than in the canonical predictions for red giants. Today these anomalies are interpreted as signs of the occurrence of non-convective mixing episodes. We therefore re-investigated this problem to verify whether the observed data can be reproduced in this scenario and if the fairly well determined properties of the two stars can help us in fixing the uncertain parameters that characterize non-convective mixing and in constraining its physical nature. Methods. We used high-resolution infrared spectra from the literature to derive the 12C/13C and 16O/17O/18O ratios from CO molecular lines near 5 μm, using the local termodynamic equilibrium (LTE) spectral synthesis method. We made use of the recently published ACE-FTS atlas of the infrared solar spectrum for constructing an updated atomic and molecular line lists in this spectral range. We also reconsidered the determination of the stellar parameters to build the proper atmospheric and evolutionary models. Results. We found that both the C and the O isotopic ratios for the two stars considered actually disagree with pure FDU predictions. This reinforces the idea that non-convective transport episodes occurred in these stars. By reproducing the observed elemental and isotopic abundances with the help of parametric models for the coupled occurrence of nucleosynthesis and mass circulation, we derived constraints on the properties of non-convective mixing, providing information on the so far elusive physics of these phenomena. We find that very slow mixing, like that associated to diffusive processes, is incapable of explaining the observed data, which require a fast transport. Circulation mechanisms with speeds intermediate between those typical of diffusive and convective mixing are necessary. We conclude with a word of caution on the conclusions possible at this stage however, as the parameters for the mass transport are fairly sensitive to the stellar mass and initial composition. At least for α Boo, reducing the uncertainty still remaining on these data would be highly desirable. [ABSTRACT FROM AUTHOR]

We derive a self-consistent set of atmospheric parameters and abundances of 17 elements for the red giant star Arcturus: Teff = 4286 ± 30 K, log g = 1.66 ± 0.05, and [Fe/H] = -0.52 ± 0.04. The effective temperature was determined using model atmosphere fits to the observed spectral energy distribution from the blue to the mid-infrared (0.44 to 10 µm). The surface gravity was calculated using the trigonometric parallax of the star and stellar evolution models. A differential abundance analysis relative to the solar spectrum allowed us to derive iron abundances from equivalent width measurements of 37 FeI and 9 FII lines, unblended in the spectra of both Arcturus and the Sun; the [Fe/H] value adopted is derived from FeI lines. We also determine the mass, radius, and age of Arcturus: M = 1.08 ± 0.06 M⊙, R = 25.4 ± 0.2 R⊙, and Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed Gyr. Finally, abundances of the following elements are measured from an equivalent width analysis of atomic features: C, O, Na, Mg, Al, Si, K, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, and Zn. We find the chemical composition of Arcturus typical of that of a local thick-disk star, consistent with its kinematics. [ABSTRACT FROM AUTHOR]

In this essay we present a tentative archaeoastronomical analysis of the Moxos' Lagoons, a controversial and huge geographical network in the landscape of the Bolivian Amazon. In the late 1990s, a preliminary analysis of the orientation of a comprehensive and statistically significant number of lagoons showed that only human action could explain the peculiarities of their geometry, and especially their orientation according to a main axis aligned to an azimuth of 50° and its complementary angle. Since then, there has been an open debate on how these orientations could have been determined in practice. The absence of distinctive geographical features on the horizon strongly suggests that this peculiar pattern must have an astronomical justification. This short report presents a first approximation to the problem, suggesting that the lagoons could have been deliberately orientated in accordance with certain stellar positions which may have marked selected moments in the local climatic or economic cycle, a fact that could be corroborated by ethnohistoric references. The implications for new ethnographical research in the region are self-evident. [ABSTRACT FROM PUBLISHER]

This study resolves a discrepancy in the abundance of Zr in the 47 Tucanæ asymptotic giant branch (AGB) star Lee 2525. This star was observed using the echelle spectrograph on the 2.3-m telescope at Siding Spring Observatory. The analysis was undertaken by calibrating Lee 2525 with respect to the standard giant star Arcturus. This work emphasizes the importance of using a standard star with stellar parameters comparable to the star under analysis rather than a calibration with respect to the Sun as in Koch & McWilliam . Systematic errors in the analysis process are then minimized due to the similarity in atmospheric structure between the standard and programme stars. The abundances derived for Lee 2525 were found to be in general agreement with the Brown & Wallerstein values except for Zr. In this study Zr has a similar enhancement ( dex) to another light s-process element, Y ( dex), which reflects current theory regarding the enrichment of s-process elements by nuclear processes within AGB stars. This is contrary to the results of Brown & Wallerstein where Zr was underabundant ( dex) and Y was overabundant ( dex) with respect to Fe. [ABSTRACT FROM AUTHOR]

The article focuses on the calculation of the dates when stars and constellations would rise and set. It notes that the knowledge of calculating the rising and setting of stars is important in understanding poetry. It details the problems that could arise during the calculation process including the lack of awareness of the necessary variables and the variety of uncertainties after the result. Also presented are the calculated dates of regulus and arcturus.

We have modeled absorption lines of the 12CO and 13CO (Δ υ = 2) molecular bands at λλ 2.29–2.45 µm in the spectrum of Arcturus (K2III). A grid of model atmospheres and synthetic spectra were computed for the red giant using T eff = 4300, log g = 1.5, and the elemental abundances of Peterson et al. (1993), with the exception of the abundances of carbon, log N(C), and oxygen, log N(O) and the carbon isotopic ratio, 12C/13C, which were varied in our computations. The computed spectra were compared to the observed spectrum of Arcturus from the atlas of Hinkle et al. (1976). The best fit between the synthetic and observed spectra is achieved for log N(C) = −3.78, 12C/13C = 8 ± 0.5. We discuss the dependence of 12C/13C on log N(C) and log N(O) in the atmosphere of the red giant. [ABSTRACT FROM AUTHOR]

We present here near-infrared spectroscopy in the H and K bands of a selection of nearly 80 stars that belong to various asymptotic giant branch (AGB) types, namely S type, M type and SR type. This sample also includes 16 post-AGB (PAGB) stars. From these spectra, we seek correlations between the equivalent widths of some important spectral signatures and the infrared colours that are indicative of mass-loss. Repeated spectroscopic observations were made on some PAGB stars to look for spectral variations. We also analyse archival Spitzer mid-infrared spectra on a few PAGB stars to identify spectral features due to polycyclic aromatic hydrocarbon (PAH) molecules providing confirmation of the advanced stage of their evolution. Further, we model the spectral energy distributions (SEDs) of the stars (compiled from archival data) and compare circumstellar dust parameters and mass-loss rates in different types. Our near-infrared spectra show that in the case of M- and S type stars, the equivalent widths of the CO(3–0) band are moderately correlated with infrared colours, suggesting a possible relationship with mass-loss processes. A few PAGB stars revealed short-term variability in their spectra, indicating episodic mass-loss: the cooler stars showed in CO first overtone bands and the hotter ones showed in H i Brackett lines. Our spectra on IRAS 19399+2312 suggest that it is a transition object. From the Spitzer spectra, there seems to be a dependence between the spectral type of the PAGB stars and the strength of the PAH features. Modelling of SEDs showed among the M and PAGB stars that the higher the mass-loss rates, the higher the [ K− 12] colour in our sample. [ABSTRACT FROM AUTHOR]

Abstract: The isolation and molecular analysis of highly purified cell populations from complex, heterogeneous tissues has been a challenge for many years. Spermatogenesis in the testis is a particularly difficult process to study given the unique multiple cellular associations within the seminiferous epithelium, making the isolation of specific cell types difficult. Laser-capture microdissection (LCM) is a recently developed technique that enables the isolation of individual cell populations from complex tissues. This technology has enhanced our ability to directly examine gene expression in enriched testicular cell populations by routine methods of gene expression analysis, such as real-time RT-PCR, differential display, and gene microarrays. The application of LCM has however introduced methodological hurdles that have not been encountered with more conventional molecular analyses of whole tissue. In particular, tissue handling (i.e. fixation, storage, and staining), consumables (e.g. slide choice), staining reagents (conventional H&E vs. fluorescence), extraction methods, and downstream applications have all required re-optimisation to facilitate differential gene expression analysis using the small amounts of material obtained using LCM. This review will discuss three critical issues that are essential for successful procurement of cells from testicular tissue sections; tissue morphology, capture success, and maintenance of molecular integrity. The importance of these issues will be discussed with specific reference to the two most commonly used LCM systems; the Arcturus PixCell IIe and PALM systems. The rat testis will be used as a model, and emphasis will be placed on issues of tissue handling, processing, and staining methods, including the application of fluorescence techniques to assist in the identification of cells of interest for the purposes of mRNA expression analysis. [Copyright &y& Elsevier]

Abstract: Introduction: Affymetrix oligonucleotide microarrays are widely used in basic and applied research (). The need for a significant amount of starting RNA has limited its use in applications where the amount of RNA is limiting, such as with Laser Captured Microdissection (LCM), small biopsies, or peripheral blood in rodent models. To overcome this limitation, various RNA amplification and labeling methods have been described, however, further optimization and validation of these methods are needed. Methods: Here we reported using the Arcturus technology to optimize amplification and labeling of small amounts of RNA for Affymetrix microarray studies. We assessed the technical feasibility and variation introduced by differences in starting RNA quantity and differences in technical performance by microarray hybridization. Results: We demonstrated that the current approach is reliable to amplify as little as 40 ng total RNA, and it is suitable for Affymetrix studies yielding satisfactory quantitative chip performance. We also showed that differences in labeling methods contribute more to variation than the differences in starting RNA quantity per se. As a model, we studied the well-documented TNF-induced inflammatory responses in cultured human vascular endothelial cells. We were able to recapitulate the TNF-induced responses using small RNA sample profiling. [Copyright &y& Elsevier]

The influence of the blanketing effect on the intensities of Fe I lines in solar and stellar atmospheres is investigated. More than 18,000 spectral lines of 14 elements were taken into account. It was demonstrated that ignoring the line-blanketing effect produces an error in the estimation of iron abundance of 0.04 dex in the case of the Sun and solar-type stars. (The iron abundance is given in the logarithmic scale and dex means the decimal logarithm estimation error.) [ABSTRACT FROM AUTHOR]

The Holidoteidae Wägele, 1989, a family of three genera confined to southern Africa, are reviewed. Diagnoses are given for Austroarcturus Kensley, 1975, Holidotea Barnard, 1920 and Neoarcturus Barnard, 1914. Their type species are re-illustrated. Keys and brief diagnoses are provided to the six species of Austroarcturus, all from shelf depths (A. africanus Kensley, A. foveolatus Kensley, A. laevis (Kensley), A. quadriconis (Kensley), A. dayi (Kensley), A. similes (Kensley)) and the nine species of Neoarcturus, from slope depths (N. barnardi (Kensley), N. biserialis (Kensley), N. halei (Kensley), N. kensleyi n. sp., N. longispinus (Kensley), N. nordenstami (Kensley), N. ornatus (Kensley), N. oudops Barnard, N. youngi (Kensley)). Holidotea is monotypic, H. unicornis inhabiting the lower shelf. Southern African species of 'Microarcturus' Nordenstam, 1933, a generic name without type species and therefore a nomen nudum, are placed in Austroarcturus or Neoarcturus. Non-southern African species (mostly Antarctic or subantarctic) assigned to 'Microarcturus' or described as species of it are placed in other genera in Antarcturidae, Austrarcturellidae, Pseudidotheidae and Rectarcturidae. 'Microarcturus' mawsoni Hale, Arcturus hirticornis Monod and A. patagonicus Ohlin which were included in 'Microarcturus' by Nordenstam, and 'M.' rugosus Nordenstam (herein redescribed) are placed in Fissarcturus Brandt. Three others are assigned to Mixarcturus Brandt: 'Microarcturus' abnormis Kussakin, Arcturus acanthurus Monod; and 'Microarcturus' digitatus Nordenstam (herein rede-scribed). The following, also from Antarctic and subantarctic waters, have also been placed in 'Microarcturus' at various times and are reallocated to other genera: Antarcturus kilepoae Kussakin, Litarcturus stebbingi (Beddard); Rectarc-turus kophameli (Ohlin); Austrarcturella oculata (Beddard); and Pseudidothea scutata (Stephensen). Four poorly known Australian species described by Whitelegge and... [ABSTRACT FROM AUTHOR]