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The radii of planets serve as significant constraints for their internal structure. Despite the complexity of planetary internal structure compared to stars, substantial advancements have been made in this field. The most critical uncertainties stem from the chemical composition and equation of state of planetary material. Using the MESA code, we construct rotating and non-rotating interior models for Jupiter and Saturn and sought to align these models to the observed radii. Rotation exerts a significant influence on their structures, distorting planetary, and stellar structures in distinct ways. Regarding gas planets' structure, two pivotal uncertain parameters depend on a possible separation between hydrogen and helium in the protosolar disc gas due to unequal evaporation between these two gases. In an extreme scenario where only hydrogen is lost and no heavy elements or helium are lost, Jupiter and Saturn would have a core mass of zero. However, this approach fails to yield a solution for Uranus and Neptune. Instead, our models indicate that hydrogen and helium were likely lost together during the protosolar disc phase, resulting in core masses of approximately 40, 25, 14, and 12 M⊕ for Jupiter, Saturn, Neptune, and Uranus, respectively. These findings are highly compatible with the observed mass–radius relationship of exoplanets, as well as the seismic and Juno data for Jupiter's near-surface temperature. [ABSTRACT FROM AUTHOR]

The observation of an unprecedented number of solar-like oscillating subgiant (SG) stars by the Kepler and TESS missions is crucial for the asteroseismic characterization of these stars, stellar population studies, and the study of stellar evolution theories. Owing to these missions, the fundamental parameters of the solar-like oscillating stars are precisely calculated from the evolution codes using the observed oscillation frequencies. Herein, we considered four solar-like oscillating SG stars. We obtained the fundamental parameters of the SG stars by constructing interior models using asteroseismic and non-asteroseismic observed parameters. The interior models of the four SG stars are constructed using the Modules for Experiments in Stellar Astrophysics code to effectively determine the fundamental properties. Using this method, the four solar-like oscillating SG stars are found to have masses and radii within the ranges of 1.16–1.75 M⊙ and 2.26–3.17 R⊙, respectively. The estimation accuracy of the typical asteroseismic radius, mass, and age is increased by fitting the observed and model reference frequencies. The typical uncertainties of the mass and radius are 3–4 |${{\ \rm per\ cent}}$| and 1–2 |${{\ \rm per\ cent}}$|⁠ , respectively. Furthermore, the observed l  = 1 frequencies, which showed a mixed mode for the first time, were also fitted to the models. Information regarding the gravity and density of the helium core was obtained by examining the mixed modes. Moreover, new asteroseismic methods for determining the age of SG stars are developed for the first time in this study. [ABSTRACT FROM AUTHOR]

This study addresses the assessment of crop water stress index (CWSI) of bell pepper (Capsicum annuum L.) and net income generated under regulated deficit irrigation (RDI), conventional deficit irrigation and partial root-zone drying (PRD) and full irrigation (I100) using surface- and subsurface-drip systems (DI and SDI) during 2016 and 2017 in the Mediterranean region. The experimental design was split-plots with four replications. RDI was supplied with 50% of I100 during vegetative stage until flowering, then received 100% of crop water requirement. PRD50 received 50% of I100, but from alternative laterals each watering. The results revealed that CWSI was correlated significantly (P < 0.01) and negatively with yield, yield per plant, total soluble solid, ETa, fruit weight and plant height indicating that yield of bell pepper declined with increasing CWSI values (P < 0.01). Bell pepper should be irrigated at mean CWSI value of 0.20 without any yield reduction. CWSI in the RDI and I75 treatments were slightly greater than 0.20. Irrigation treatments had significant effect on yield and quality traits. The highest total soluble solutes were found in PRD50 and I50. The DI I100 treatment generated the highest net income followed by the SDI I100 and RDI. In conclusion, RDI and I75 appear to be good alternatives to I100 for sustainable bell pepper production in the Mediterranean region. [ABSTRACT FROM AUTHOR]

For solar-like oscillators, the asteroseismic relations connect the stellar mean density and surface gravity to observable properties of the oscillations. Since the space missions CoRoT and Kepler, the asteroseismic relations have been massively employed out of their theoretical domain of validity, that is the main-sequence solar-type stars, in particular for red giant stars. However, despite a surprisingly good performance of the asteroseismic relation with red giant stars, they are biased and attempts to parametrize the departure of the relations for evolved stars have been the subject of many recent efforts. In this study, we propose a new parametrization of the asteroseismic relations for red giants of radii up to |${\sim } 50\, \mathrm{R}_\odot$|⁠ , based on a calibration performed with Gaia parallax data. We find that the asteroseismic scaling relations depend on metallicity and effective temperature. For this solution, we obtain a parallax offset of about −0.026 ± 0.001 mas, and radius ranges from 3.8 to 53.2 R⊙. Most stars have masses that range from 0.9 to 1.7 M⊙, with the star count peaking around 1.2 M⊙. We also use data of the eclipsing binaries with solar-like oscillating components for calibration and discuss the diagnostic potential of the mass–metallicity diagram for our understanding of the evolution of red giants and the chemodynamics of the Galactic disc. Using this diagram, we identify stars that lost and gained mass and estimate the minimum change in mass. [ABSTRACT FROM AUTHOR]

This study aimed to investigate the prevalence of fear of childbirth (FOC) and associated factors including vaginismus in pregnant women with high/severe FOC. In the study, 407 women who were at 24–40 weeks of gestation were included. The Wijma Delivery Expectancy/Experience Questionnaire Version A (WDEQA), Beck Depression Inventory (BDI), Beck Anxiety Inventory (BAI), and vaginismus sub-scale of the Golombok Rust inventory of sexual satisfaction (GRISS) were used. 186 (46%) participants had high/severe FOC. Pregnant women with high/severe FOC had a significantly higher fear of pain during sexual intercourse, higher scores in the WDEQA, BDI, BAI, and vaginismus sub-scale of GRISS. Depression and anxiety level, educational level, access to information on delivery during pregnancy, presence of medical disease, and expression of FOC were predictors of high/severe FOC. Assessment of FOC and associated risk factors, including vaginismus, during pregnancy, will enable the identification of risk groups and the creation of support programmes. What is already known on this subject? The range of fear of childbirth (FOC) changes from mild anxiety to severe fear. The prevalence and severity of FOC and related risk factors vary in the studies due to cultural factors, differences in the definition of FOC and measurement tools. The relationship between FOC and vaginismus has not been sufficiently investigated. What do the results of this study add? This study aimed to investigate the prevalence of fear of childbirth (FOC) and associated factors including vaginismus in pregnant women with high/severe FOC. What are the implications of these findings for clinical practice and/or further research? This is the first study that evaluates vaginismus as a risk factor for FOC. Assessment of FOC and associated risk factors, including vaginismus, in pregnant women, will enable the identification of risk groups and the creation of support programs for risk reduction. [ABSTRACT FROM AUTHOR]

Copyright of Journal of Ankara University Faculty of Medicine / Ankara Üniversitesi Tip Fakültesi Mecmuasi is the property of Galenos Yayinevi Tic. LTD. STI and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Data from the space missions Gaia, Kepler, CoRoT and TESS , make it possible to compare parallax and asteroseismic distances. From the ratio of two densities ρsca/ρπ, we obtain an empirical relation f Δν between the asteroseismic large frequency separation and mean density, which is important for more accurate stellar mass and radius. This expression for main-sequence (MS) and subgiant stars with K -band magnitude is very close to the one obtained from interior MS models by Yıldız, Çelik & Kayhan. We also discuss the effects of effective temperature and parallax offset as the source of the difference between asteroseismic and non-asteroseismic stellar parameters. We have obtained our best results for about 3500 red giants (RGs) by using 2MASS data and model values for f Δν from Sharma et al. Another unknown scaling parameter |$f_{\nu _{\rm max}}$| comes from the relationship between the frequency of maximum amplitude and gravity. Using different combinations of |$f_{\nu _{\rm max}}$| and the parallax offset, we find that the parallax offset is generally a function of distance. The situation where this slope disappears is accepted as the most reasonable solution. By a very careful comparison of asteroseismic and non-asteroseismic parameters, we obtain very precise values for the parallax offset and |$f_{\nu _{\rm max}}$| for RGs of –0.0463 ± 0.0007 mas and 1.003 ± 0.001, respectively. Our results for mass and radius are in perfect agreement with those of APOKASC-2: the mass and radius of ∼3500 RGs are in the range of about 0.8–1.8 M⊙ (96 per cent) and 3.8–38 R⊙, respectively. [ABSTRACT FROM AUTHOR]

Asteroseismology using space-based telescopes is vital to our understanding of stellar structure and evolution. CoRoT, Kepler , and TESS space telescopes have detected large numbers of solar-like oscillating evolved stars. Solar-like oscillation frequencies have an important role in the determination of fundamental stellar parameters; in the literature, the relations between the two is established by the so-called scaling relations. In this study, we analyse data obtained from the observation of 15 evolved solar-like oscillating stars using the Kepler and ground-based telescopes. The main purpose of the study is to determine very precisely the fundamental parameters of evolved stars by constructing interior models using asteroseismic parameters. We also fit the reference frequencies of models to the observational reference frequencies caused by the He  ii ionization zone. The 15 evolved stars are found to have masses and radii within ranges of 0.79–1.47 M⊙ and 1.60–3.15 R ⊙, respectively. Their model ages range from 2.19 to 12.75 Gyr. It is revealed that fitting reference frequencies typically increase the accuracy of asteroseismic radius, mass, and age. The typical uncertainties of mass and radius are ∼3–6 and ∼1–2 per cent, respectively. Accordingly, the differences between the model and literature ages are generally only a few Gyr. [ABSTRACT FROM AUTHOR]

In the present study, a Schiff base (E)-2-[(3,5-bis(trifluoromethyl)phenylimino)methyl]-4,6-dichlorophenol has been synthesized. Its spectroscopic and X-ray single-crystal data have been compared with the results of theoretical calculations based on the DFT method, as well as molecular electrostatic potential (MEP), HOMO and LUMO, and nonlinear optical (NLO) effects. Antimicrobial activity of the compound has been tested against some bacteria and fungi. According to UV-Vis and agarose gel electrophoresis methods, the compound interacts with DNA electrostatically and breaks it oxidatively. Antioxidant activity of the compound measured by the DPPH method, is lower than that of BHT. [ABSTRACT FROM AUTHOR]

Background/Aim: Burnout is a syndrome of physical exhaustion, prolonged fatigue, and helplessness reflected by negative attitudes on work, life, and other people around. The aim of this study is to investigate the relationship between burnout and working conditions in the banking sector, which has intense emotional demands. Methods: The research group consisted of 1183 individuals working in 138 different branches. A data form questioning the working conditions and sociodemographic characteristics of the participants that may be related to the burnout level was filled with face-to-face interviews. Burnout level was determined using the Maslach Burnout Inventory. This was planned as a cross-sectional research. Results: Higher levels of burnout was determined in those who thought that their family income was insufficient, who had to work more than 8.5 hours per day, who were exposed to physical or mental violence, those with chronic diseases and finally, workers who thought they dealt with too many customers in a day. Conclusion: It appears that the burnout levels of the employees can be reduced by arrangements at corporate and individual levels in addition to the regulations that can be realized within the legislation. [ABSTRACT FROM AUTHOR]

Mechanical performance of marine sandwich panels comprising E-glass/vinyl ester face sheets and perforated poly-vinyl chloride foam core was evaluated and compared with conventional foam core sandwich panels. Circular holes through the foam core thickness were drilled with 12 different arrangements in square patterns and the holes were filled with the resin during the infusion process which created the through-the-thickness solid resin pins. The effect of each pattern on the flatwise compression and core shear properties of the sandwich panels were experimentally investigated. The three-point bending maximum failure load of perforated foam core sandwich panels was increased over 133.8% by increasing the diameter of the resin pins at the expense of increased panel weight up to 67%. The flatwise compression stress to induce core crushing was significantly increased by reinforcing the resin pins. [ABSTRACT FROM AUTHOR]

Context. The Transiting Exoplanet Survey Satellite (TESS) is observing bright known planet-host stars across almost the entire sky. These stars have been subject to extensive ground-based observations, providing a large number of radial velocity measurements. Aims. The objective of this work is to use the new TESS photometric observations to characterize the star λ2 Fornacis, and following this to update the parameters of the orbiting planet λ2 For b. Methods. We measured the frequencies of the p-mode oscillations in λ2 For, and in combination with non-seismic parameters estimated the stellar fundamental properties using stellar models. Using the revised stellar properties and a time series of archival radial velocities from the UCLES, HIRES and HARPS instruments spanning almost 20 years, we refit the orbit of λ2 For b and searched the residual radial velocities for remaining variability. Results. We find that λ2 For has a mass of 1.16 ± 0.03 M⊙ and a radius of 1.63 ± 0.04 R⊙, with an age of 6.3 ± 0.9 Gyr. This and the updated radial velocity measurements suggest a mass of λ2 For b of 16.8−1.3+1.2M⊕ 16. 8 − 1.3 + 1.2 M ⊕ $ 16.8^{+1.2}_{-1.3}\,{{M}_\oplus} $ , which is ∼5M⊕ less than literature estimates. We also detect an additional periodicity at 33 days in the radial velocity measurements, which is likely due to the rotation of the host star. Conclusions. While previous literature estimates of the properties of λ2 For are ambiguous, the asteroseismic measurements place the star firmly at the early stage of its subgiant evolutionary phase. Typically only short time series of photometric data are available from TESS, but by using asteroseismology it is still possible to provide tight constraints on the properties of bright stars that until now have only been observed from the ground. This prompts a reexamination of archival radial velocity data that have been accumulated in the past few decades in order to update the characteristics of the planet hosting systems observed by TESS for which asteroseismology is possible. [ABSTRACT FROM AUTHOR]

Context. Observations of neutral hydrogen (H I) and molecular gas show that 50% of all nearby early-type galaxies contain some cold gas. Molecular gas is always found in small gas discs in the central region of the galaxy, while neutral hydrogen is often distributed in a low-column density disc or ring typically extending well beyond the stellar body. Dust is frequently found in early-type galaxies as well. Aims. The goal of our study is to understand the link between dust and cold gas in nearby early-type galaxies as a function of H I content. Methods. We analyse deep optical g − r images obtained with the MegaCam camera at the Canada-France-Hawaii Telescope for a sample of 21 H I-rich and 41 H I-poor early-type galaxies. Results. We find that all H I-rich galaxies contain dust seen as absorption. Moreover, in 57% of these H I-rich galaxies, the dust is distributed in a large-scale spiral pattern. Although the dust detection rate is relatively high in the H I-poor galaxies (∼59%), most of these systems exhibit simpler dust morphologies without any evidence of spiral structures. We find that the H I-rich galaxies possess more complex dust morphology extending to almost two times larger radii than H I-poor objects. We measured the dust content of the galaxies from the optical colour excess and find that H I-rich galaxies contain six times more dust (in mass) than H I-poor ones. In order to maintain the dust structures in the galaxies, continuous gas accretion is needed, and the substantial H I gas reservoirs in the outer regions of early-type galaxies can satisfy this need for a long time. We find that there is a good correspondence between the observed masses of the gas and dust, and it is also clear that dust is present in regions further than 3 Reff. Conclusions. Our findings indicate an essential relation between the presence of cold gas and dust in early-type galaxies and offer a way to study the interstellar medium in more detail than what is possible with H I observations. [ABSTRACT FROM AUTHOR]

Planets and planet candidates are subjected to great investigation in recent years. In this study, we analyse 20 planet and planet-candidate host stars at different evolutionary phases. We construct stellar interior models of the host stars with the mesa e.volution code and obtain their fundamental parameters under influence of observational asteroseismic and non-asteroseismic constraints. Model mass range of the host stars is 0.74–1.55    |$\rm M_{\odot }$|⁠. The mean value of the so-called large separation between oscillation frequencies and its variation about the minima shows the diagnostic potential of asteroseismic properties. Comparison of variations of model and observed large separations versus the oscillation frequencies leads to inference of fundamental parameters of the host stars. Using these parameters, we revise orbital and fundamental parameters of 34 planets and four planet candidates. According to our findings, radius range of the planets is 0.35–16.50  |$\rm R_{{\oplus }}$|⁠. The maximum difference between the transit and revised radii occurs for Kepler-444b-f is about 25 per cent. [ABSTRACT FROM AUTHOR]

Recently, by analysing the oscillation frequencies of 90 stars, Yıldız, Çelik Orhan & Kayhan have shown that the reference frequencies (νmin0, νmin1, and νmin2) derived from glitches due to He  ii ionization zone have very strong diagnostic potential for the determination of their effective temperatures. In this study, we continue to analyse the same stars and compute their mass, radius, and age from different scaling relations including relations based on νmin0, νmin1, and νmin2. For most of the stars, the masses computed using νmin0 and νmin1 are very close to each other. For 38 stars, the difference between these masses is less than 0.024 M |$\odot$| . The radii of these stars from νmin0 and νmin1 are even closer, with differences of less than 0.007 R |$\odot$| . These stars may be the most well known solar-like oscillating stars and deserve to be studied in detail. The asteroseismic expressions we derive for mass and radius show slight dependence on metallicity. We therefore develop a new method for computing initial metallicity from this surface metallicity by taking into account the effect of microscopic diffusion. The time dependence of initial metallicity shows some very interesting features that may be important for our understanding of chemical enrichment of Galactic Disc. According to our findings, every epoch of the disc has its own lowest and highest values for metallicity. It seems that rotational velocity is inversely proportional to 1/2 power of age as given by the Skumanich relation. [ABSTRACT FROM AUTHOR]

(E)-2-((4-tert-butylbenzylimino)methyl)-4-methoxyphenol is synthesized by the reaction of 4-tert-buthylbenzylamine with 5-methoxysalicylaldehyde. The structure of the Schiff base is investigated by FT-IR, UV-visible, and 1H NMR, 13C NMR, and X-ray data. Moreover, the molecular structure, molecular electrostatic potential surfaces (MEP), frontier molecular orbitals, and nonlinear optical properties (NLO) are also investigated by density functional theory (DFT) calculations. The experimental and calculated results show that the phenol-imine form of the compound is more favoured than the keto-amine form. The most energy favourable docked structures are obtained from the rigid molecular docking of the compound with DNA. The compound binds at the active site of DNA proteins by weak non-covalent interactions. UV-Vis spectroscopy studies of the interactions between the compounds and calf thymus DNA (CT-DNA) show that the compounds interact with CT-DNA via the electrostatic and intercalative binding. The compound inhibits the frameshift and base pair mutations in the absence of S9 mix with a high inhibition rate. Also, the molecular docking is made to identify the interaction between the ligand and DNA. [ABSTRACT FROM AUTHOR]

Abstract: Cyclization of 2-chloro-3-((4-(hexyloxy)phenyl)amino)naphthalene-1,4-dione obtained from the reaction of 2,3-dichloro-1,4-naphthoquinone with 4-(hexyloxy)aniline by sodium azide in N,N-dimethylformamide (DMF) at 90-95°C gives 2-(hexyloxy)benzo[b]phenazine-6,11-dione. This is a remarkable example of a general procedure to prepare functionalized benzo[b]phenazine-6,11-dione derivatives. The structure of the title compound was confirmed by single crystal X-ray diffraction analysis. The compound, C22H20N2O3, crystallizes in the sp. gr. P, Z = 2. Both O atoms and one of N atoms are involved in hydrogen bonds forming a network. Besides, there is offset stacking interaction between the planes of polycyclic systems with interplanar distance of 3.383 Å. [ABSTRACT FROM AUTHOR]

Purpose: To share the lower recurrence rate achieved during long-term follow-up by repairing incisional hernias (IHs) with full-thickness fixation of onlay mesh.Methods: We retrospectively analyzed 196 IH cases operated on by the same surgeon between 2002 and 2013. After exclusions (unrelated death, lack of follow-up), 154 cases were included. Abdominal examination findings, recurrence dates (if accessible), and imaging results were obtained from computer records and evaluated. Intraoperatively, all hernial sac adhesions were separated to reveal the anterior abdominal wall, and full-thickness suspension sutures were placed 6-8 cm lateral to the fascial edge at 2-cm intervals, excluding the peritoneum. The primary fasciae were closed, suspension sutures were passed through the mesh holes, and the mesh was fixed as an onlay, leaving no space between the fasciae.Results: In total, 154 subjects with IHs were analyzed: 107 (69.5%) females and 47 (30.5%) males. The mean patient age was 52.60 years [standard deviation (SD) 11.24 years], and the mean fascial defect diameter was 77 cm(2). The average operation time was 128 min (SD 42.5 min), and the average patient follow-up time was 54 months (SD 22.8 months). Eight (5.2%) patients developed recurrences after full-thickness mesh fixation, and ten subjects (6.5%) had persistent pain in the operative area for longer than 3 months.Conclusions: Full-thickness mesh fixation mechanically supports the fascia, especially in the early postoperative period, and enables homogeneous fibrous healing in a wide area, preventing mesh migration; we believe that these attributes are crucial in reducing the IH recurrence rate. [ABSTRACT FROM AUTHOR]

Asteroseismology provides fundamental properties (mass, radius and effective temperature) of solar-like oscillating stars using so-called scaling relations. These properties allow the computation of the asteroseismic distance of stars. We compare the asteroseismic distances with the recently released Gaia distances for 74 stars studied in Yıldız et al. There is a very good agreement between these two distances; for 64 of these stars, the difference is less than 10 per cent. However, a systematic difference is seen if we use the effective temperature obtained by spectroscopic methods; the Gaia distances are about 5 per cent greater than the asteroseismic distances. [ABSTRACT FROM AUTHOR]

So-called scaling relations based on oscillation frequencies have the potential to reveal the mass and radius of solar-like oscillating stars. In the derivation of these relations, it is assumed that the first adiabatic exponent at the surface (Γ1s) of such stars is constant. However, by constructing interior models for the mass range 0.8-1.6 M⊙, we show that 1s is not constant at stellar surfaces for the effective temperature range with which we deal. Furthermore, the well-known relation between large separation and mean density also depends on Γ1s. Such knowledge is the basis for our aim of modifying the scaling relations. There are significant differences between masses and radii found from modified and conventional scaling relations. However, a comparison of predictions of these relations with the non-asteroseismic observations of Procyon A reveals that new scaling relations are effective in determining the mass and radius of stars. In the present study, solar-like oscillation frequencies of 89 target stars (mostly Kepler and CoRoT) were analysed. As well as two new reference frequencies (νmin1 and νmin2) found in the spacing of solar-like oscillation frequencies of stellar interior models, we also take into account νmin0. In addition to the frequency of maximum amplitude, these frequencies have a very strong diagnostic potential in the determination of fundamental properties. The present study applies the derived relations from the models to the solar-like oscillating stars, and computes their effective temperatures using purely asteroseismic methods. There are in general very close agreements between effective temperatures from asteroseismic and nonasteroseismic (spectral and photometric) methods. For the Sun and Procyon A, for example, the agreement is almost total. [ABSTRACT FROM AUTHOR]

Purpose: Diagnosis of cortical vein thrombosis (CVT) on the basis of clot hyperintensity on diffusion-weighted imaging (DWI) has been reported as limited. Our aim was to evaluate different DWI findings of CVT either in isolated form or in combination with sinus thrombosis. Methods: In this review-board-approved study, patients with the diagnosis of CVT on magnetic resonance venography (MRV) between 2004 and 2011 were evaluated, and 13 patients with 26 CVT (3 isolated and 23 combined CVT) sites were recruited. The evaluated DWI findings were as follows: (1) the hyperintense clot signal (CS) itself, and (2) clot susceptibility signal (CSS) that appears next to the CVT. Two blinded radiologists evaluated the data. Kappa (κ) statistics was applied for interobserver agreement. Results: Both readers reported CS within the vascular clot itself in 6 of 26 (23 %) CVT sites on DWI. CSS was reported in 16 of 26 (61.5 %) CVT sites by reader 1, and in 14 of 26 (54 %) of the CVT sites by reader 2. At four CVT sites with thrombosed veins on MRV, both readers reported no DWI findings. When both CS and CSS were evaluated together, reader 1 reported a positive DWI finding in 22 of 26 (84 %) of the CVT sites, and reader 2 reported in 20 of 26 (79 %) of the sites. κ Statistics showed a very good agreement (κ: 0.87). Conclusions: Besides the hyperintense CS, with additional evaluation of the presence of CSS, DWI can provide an additional clue in CVT patients and may suggest its diagnosis, which is important in clinically unsuspected patients. [ABSTRACT FROM AUTHOR]

Schiff base podands have been synthesized by reaction of triethylene glycol bis(4-aminophenyl) ether with salicylaldehyde, 5-substituted salicylaldehydes, and 2-hydroxy-1-naphthaldehyde. Manganese(II), iron(II), cobalt(II), nickel(II), and copper(II) complexes have been prepared from the salicylaldehyde-based podand via reaction with MCl · nHO. The structures of the ligands and complexes have been studied by elemental analysis, FT-IR and UV-visible spectroscopy, H and C NMR, and thermogravimetric analysis. The UV-visible spectral and TG data suggest tetrahedral geometry of the metal complexes. The antimicrobial activities of the ligands and metal complexes have been evaluated as minimum inhibitory concentrations with respect to bacteria and yeast cultures. The interaction of the Schiff base podands with calf thymus DNA has been investigated by UV-visible spectroscopy, and intercalative binding to DNA has been found. The anion recognition ability of all Schiff base podands has been examined by UV-visible spectroscopy. A visually detectable color change has been observed upon addition of fluoride, cyanide, hydroxide, and acetate ions due to formation of 1: 1 H-complexes and/or deprotonation of the receptor. No significant color change has been observed upon addition of other anions such as dihydrogen phosphate, bromide, iodide, thiocyanate, perchlorate, and hydrogen sulfate. [ABSTRACT FROM AUTHOR]

The purpose of this study is to examine some of the variables in the level of students' boldness who study at Physical education and sports colleges and to compare the findings with the other studies in the literature. The Research Group contains 92 male and 64 female (/age = 21,612 + 1,921), in total 156 students from Selcuk University physical education and sports college. In order to reach the purpose of the study "Rathus Assertiveness Schedule" has been used as the methodology which is developed by Rathus [12,13], and adopted to Turkish by Voltan [18]. For the interpretation of the data, the Kolmogorov-Smirnov test, one way anova test have been applied and to determine the difference between the groups Turkey test has been applied too. The significance was P <0.05. According to the level of sports; the difference between the average levels of scores of the assertiveness is meaningful [t value = 4,327 P = 0,000 < 0.05]. Looking at average values; average levels of the assertiveness of students doing some sports is (X =86,5614), average levels of the assertiveness of students doing some sports is (X =80,7857). As a result of this study; According to the level of sports observations, the difference between the average levels of scores of the assertiveness is meaningful [t value = 4,327 P = 0,000 < 0.05]. Looking at average values we see that students, who engaged in sports, has been obtained more level of average score of assertiveness than students engaged in no sports. From the point of assertiveness, participation in sport from the perspective of individuals there is a difference in favor of those engaged in sports. [ABSTRACT FROM AUTHOR]

Purpose: There is clinical need to predict risk of febrile neutropenia before a specific cycle of chemotherapy in cancer patients. Methods: Data on 3882 chemotherapy cycles in 1089 consecutive patients with lung, breast, and colon cancer from four teaching hospitals were used to construct a predictive model for febrile neutropenia. A final nomogram derived from the multivariate predictive model was prospectively confirmed in a second cohort of 960 consecutive cases and 1444 cycles. Results: The following factors were used to construct the nomogram: previous history of febrile neutropenia, pre-cycle lymphocyte count, type of cancer, cycle of current chemotherapy, and patient age. The predictive model had a concordance index of 0.95 (95 % confidence interval (CI) = 0.91-0.99) in the derivation cohort and 0.85 (95 % CI = 0.80-0.91) in the external validation cohort. A threshold of 15 % for the risk of febrile neutropenia in the derivation cohort was associated with a sensitivity of 0.76 and specificity of 0.98. These figures were 1.00 and 0.49 in the validation cohort if a risk threshold of 50 % was chosen. Conclusions: This nomogram is helpful in the prediction of febrile neutropenia after chemotherapy in patients with lung, breast, and colon cancer. Usage of this nomogram may help decrease the morbidity and mortality associated with febrile neutropenia and deserves further validation. [ABSTRACT FROM AUTHOR]

Copyright of Herz is the property of Springer Nature and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

The large separations between the oscillation frequencies of solar-like stars are measures of stellar mean density. The separations have been thought to be mostly constant in the observed range of frequencies. However, detailed investigation shows that they are not constant, and their variations are not random but have very strong diagnostic potential for our understanding of stellar structure and evolution. In this regard, frequencies of the minimum large separation are very useful tools. From these frequencies, in addition to the large separation and frequency of maximum amplitude, Yıldız et al. recently have developed new methods to find almost all the fundamental stellar properties. In the present study, we aim to find metallicity and helium abundances from the frequencies, and generalize the relations given by Yıldız et al. for a wider stellar mass range and arbitrary metallicity (Z) and helium abundance (Y). We show that the effect of metallicity is significant for most of the fundamental parameters. For stellar mass, for example, the expression must be multiplied by (Z/Z⊙)0.12. For arbitrary helium abundance, M ∝ (Y/Y⊙)0.25. Methods for determination of Z and Y from pure asteroseismic quantities are based on amplitudes (differences between maximum and minimum values of Δν) in the oscillatory component in the spacing of oscillation frequencies. Additionally, we demonstrate that the difference between the first maximum and the second minimum is very sensitive to Z. It also depends on νmin1/νmax and small separation between the frequencies. Such a dependence leads us to develop a method to find Z (and Y) from oscillation frequencies. The maximum difference between the estimated and model Z values is about 14 per cent. It is 10 per cent for Y. [ABSTRACT FROM AUTHOR]

The article presents a study on the management of coronary artery perforation (CAP) in patients with acute coronary syndrome (ACS). Topics include the use of the Ellis classification to determine the grade of perforation, the performance of a prolonged balloon inflation, and the requirement of emergent coronary artery bypass grafting (CABG) on some patients. It also discusses the use of anti-platelet agents for CAP management.

It is already stated in the previous studies that the radius of the giant planets is affected by stellar irradiation. The confirmed relation between radius and incident flux depends on planetary mass intervals. In this study, we show that there is a single relation between radius and irradiated energy per gram per second (l−), for all mass intervals. There is an extra increase in radius of planets if l− is higher than 1100 times energy received by the Earth (l⊕). This is likely due to dissociation of molecules. The tidal interaction as a heating mechanism is also considered and found that its maximum effect on the inflation of planets is about 15 per cent. We also compute age and heavy element abundances from the properties of host stars, given in the TEPCat catalogue (Southworth 2011). The metallicity given in the literature is as [Fe/H]. However, the most abundant element is oxygen, and there is a reverse relation between the observed abundances [Fe/H] and [O/Fe]. Therefore, we first compute [O/H] from [Fe/H] by using observed abundances, and then find heavy element abundance from [O/H]. We also develop a new method for age determination. Using the ages we find, we analyse variation of both radius and mass of the planets with respect to time, and estimate the initial mass of the planets from the relation we derive for the first time. According to our results, the highly irradiated gas giants lose 5 per cent of their mass in every 1 Gyr. [ABSTRACT FROM AUTHOR]

Copyright of Education & Science / Egitim ve Bilim is the property of Turkish Education Association and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Copyright of Medical Bulletin of Haseki / Haseki Tip Bulteni is the property of Galenos Yayinevi Tic. LTD. STI and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Low amplitude is the defining characteristic of solar-like oscillations. The space projects Kepler and CoRoT give us a great opportunity to successfully detect such oscillations in numerous targets. Achievements of asteroseismology depend on new discoveries of connections between the oscillation frequencies and stellar properties. In the previous studies, the frequency of the maximum amplitude and the large separation between frequencies were used for this purpose. In the present study, we confirm that the large separation between the frequencies has two minima at two different frequency values. These are the signatures of the He ii ionization zone, and as such have very strong diagnostic potential. We relate these minima to fundamental stellar properties such as mass, radius, luminosity, age and mass of convective zone. For mass, the relation is simply based on the ratio of the frequency of minimum Δν to the frequency of maximum amplitude. These frequency comparisons can be very precisely computed, and thus the mass and radius of a solar-like oscillating star can be determined to high precision. We also develop a new asteroseismic diagram which predicts structural and evolutionary properties of stars with such data. We derive expressions for mass, radius, effective temperature, luminosity and age in terms of purely asteroseismic quantities. For solar-like oscillating stars, we now will have five very important asteroseismic tools (two frequencies of minimum Δν, the frequency of maximum amplitude, and the large and small separations between the oscillation frequencies) to decipher properties of stellar interior astrophysics. [ABSTRACT FROM AUTHOR]

Copyright of Journal of Surgical Arts / Cerrahi Sanatlar Dergisi is the property of Journal of Surgical Arts / Cerrahi Sanatlar Dergisi and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Abstract: In this study, the effect of freezing and thawing on the strength and permeability of two clayey soils (high and low plasticity), which had been stabilized with lime, were investigated. Before and after stabilization, the permeability and strength of the specimens were determined with various freeze-thaw cycles. Results of this study indicated that for both clays, 6% lime addition increased the hydraulic conductivity of the specimens 1000 times. However, the hydraulic conductivity of clay with 6% lime increased 10–20 times after only 3 freeze-thaw cycles. The results of strength tests exhibited different trends. The strength of stabilized high plasticity clay increased approximately 15 times at the end of 28 day curing, whereas the strength of stabilized low plasticity clay increased about 3 times only. The strength of both stabilized clays decreased 10–15% at the end of the freeze-thaw cycles. [Copyright &y& Elsevier]

The Sun and α Cen A and B are the nearest stars to us. Despite the general agreement between their models and seismic and non-seismic constraints, there are serious problems pertaining to their interiors. The good agreement between the sound speed and base radius of the convective zone of the Sun and the solar models is broken apart by a recent revision in solar chemical composition. For α Cen A and B, however, it is not possible to fit models with the same age and chemical composition to all seismic and non-seismic observational constraints. At the age deduced from seismic constraints, the luminosity ratio () of the models is significantly lower than the ratio taken from the observed luminosities. Enhancement of opacity as a function of temperature is one way to restore the agreement between solar models and the Sun, but such an enhancement does not alter the situation for α Cen A and B. The reason is that models of both components are influenced in a similar manner and consequently the luminosity ratio does not change much. In the present study, problems pertaining to the interiors of these three stars with a single expression for opacity enhancement are modelled. The opacity enhancement is expressed as a function of density, ionization degree of heavy elements (oxygen) and temperature. According to this expression, for improvement of the models the required opacity enhancement for α Cen A and B at , for example, is about 7 and 22 per cent, respectively. The enhancement takes place in the region in which pressure ionization is effective, and is higher for low-mass stars than for high-mass stars. This result seems to be a possible explanation for the serious differences between models and observational results for cool stars. [ABSTRACT FROM AUTHOR]

This study was to determine the quality of curing of second generation light emitting diode (LED-II) compared to a first generation LED (LED-I) and conventional halogen (quartz tungsten halogen) light curing unity by measuring depth of cure, degree of polymerisation and surface hardness. Filtek Z-250 hybrid composite resin (3M-ESPE, Germany), with shade A2, was used in this study. One quartz tungsten halogen/light curing unit (LCU) (Hilux, Benlioglu Dental, Turkey), one LED-I-LCU unit (Elipar Freelight 3M-ESPE, Germany) and one LED-II-LCU (Elipar Freelight, 3M-ESPE, Germany) were used for polymerisation of the composite resin. The depth of cure was obtained with scrape test, degree of cure was measured with Fourier transform infrared spectrometer (Spectrum-One, Perkin-Elmer, USA) and surface hardness was calculated with surface hardness tester (Micromet-2001, Buehler, Dusseldorf, Germany). The data were analysed by Kruskal Wallis and Mann Whitney-U. The polymerisation depth of LED-I-LCU was significantly lower than that of the other LCUs (p<0·05). However, no significant differences were obtained among all tested systems in point of degree of cure and surface hardness at 2 mm depth. Within the limitations of this study, although LED-I showed lower depth of cure, all tested systems appear suitable for routine clinical practice for polymerisation of the composite resin. [ABSTRACT FROM AUTHOR]

The α Centauri (α Cen) binary system is a well-known stellar system with very accurate observational constraints on the structure of its component stars. In addition to the classical non-seismic constraints, there are also seismic constraints for the interior models of α Cen A and B. These two types of constraint give very different values for the age of the system. While we obtain 8.9 Gyr for the age of the system from the non-seismic constraints, the seismic constraints imply that the age is about 5.6–5.9 Gyr. There may be observational or theoretical reasons for this discrepancy, which can be found by careful consideration of similar stars. The α Cen binary system, with its solar-type components, is also suitable for testing the stellar mass dependence of the mixing-length parameter for convection derived from the binaries of Hyades. The values of the mixing-length parameter for α Cen A and B are 2.10 and 1.90 for the non-seismic constraints. If we prioritize the seismic constraints, we obtain 1.64 and 1.91 for α Cen A and B, respectively. By taking into account these two contrasting cases for stellar mass dependence of the mixing-length parameter, we derive two expressions for its time dependence, which are also compatible with the mass dependence of the mixing-length parameter derived from the Hyades stars. For assessment, these expressions should be tested in other stellar systems and clusters. [ABSTRACT FROM AUTHOR]

We present our findings based on a detailed analysis of the binaries of the Hyades, in which the masses of the components are well known. We fit the models of the components of a binary system to observations so as to give the observed total V and B− V of that system and the observed slope of the main sequence in the corresponding parts. According to our findings, there is a very definite relationship between the mixing-length parameter and the stellar mass. The fitting formula for this relationship can be given as , which is valid for stellar masses greater than . While no strict information is gathered for the chemical composition of the cluster, as a result of degeneracy in the colour–magnitude diagram, by adopting and using models for the components of 70 Tau and θ2 Tau we find the hydrogen abundance to be and the age to be 670 Myr. If we assume that , then and the age is 720 Myr. Our findings concerning the mixing-length parameter are valid for both sets of the solution. For both components of the active binary system V818 Tau, the differences between radii of the models with and the observed radii are only about 4 per cent. More generally, the effective temperatures of the models of low-mass stars in the binary systems studied are in good agreement with those determined by spectroscopic methods. [ABSTRACT FROM AUTHOR]

In this study, we show that only models with differential rotation, as opposed to non-rotation or solid-body rotation for the components of PV Cas, are in satisfactory agreement with the observations (including constraints on the apsidal advance rate and the synchronous rotation of the components in addition to their luminosities and radii). Internal rotation profiles found for solar and metal-rich chemical compositions are similar to each other in that only a small part of the outermost regions is rotating very slowly and the rest is rotating very rapidly. Confirmation of Ap-like variations in the light curve of the system leads us to search for a connection between this type (and similar types) of internal rotation and chemically peculiar stars. The temperature difference between the blue sides of the main sequence for the normal and for the magnetic Ap stars may arise from such a connection, since we find a similar difference between the models with this kind of rotation and the non-rotating models of somewhat lower mass. [ABSTRACT FROM AUTHOR]

The aim of this study was to investigate the effects of long-term inhaled corticosteroids on bone mineral density (BMD) of the mandible in relation with the tooth loss. Cross sectional analytic study. Patients ( n = 30) with chronic obstructive pulmonary disease under inhaled corticosteroid therapy for at least 1 year were compared with sex- and age-matched healthy controls ( n = 30). BMD of the mandible was measured by dual-energy X-ray absorptiometry. The clinical examination included recording the number of teeth present together with periodontal condition. Levels of serum osteocalcin, alkaline phosphatase, calcium, phosphorus and cortisol were also assessed. BMD of the mandible in patients on corticosteroid treatment was significantly lower than that in the control group ( P = 0.001). Patients under treatment had more missing teeth than the control group but the difference did not reach statistical significance. The two groups exhibited similar clinical parameters of periodontal condition. Significantly lower levels of osteocalcin ( P < 0.0001), calcium ( P = 0.004) and cortisol ( P = 0.03) were observed in the patients on corticosteroid treatment. Long-term use of inhaled corticosteroids may impair bone metabolism and lead to a marked decrease in the mandibular BMD. [ABSTRACT FROM AUTHOR]

N-(3-pyridil)-2-oxo-1-naphthylidenemethylamine (C16H12N2O) was studied by elemental analysis, IR, 1H NMR, and UV–visible techniques and X-ray diffraction methods. The UV–visible spectrum of the compound was investigated in solutions effect polarity. The polarity of the some solvents was modifierly the additional (CF3COOH) and [(C2H5)3N]. The compound is in tautomeric equilibrium ( phenol-imine O–H···N and keto-amine O···H–N forms) in polar and nonpolar solvents. The keto-amine form is observed in basic solutions of DMSO, ethanol, chloroform, benzene, cyclohexane, and in acidic solutions of chloroform and benzene, but not in acidic solutions of DMSO and ethanol. The compound crystallizes in the monoclinic, space group P21/a with a = 7.010(5) Å, b = 13.669(4) Å, c = 12.764(4) Å, β = 101.23(4)°, V = 1199.6(10) Å3, Z = 4, Dc = 1.375 g/cm3, μ(Mo Kα) = 0.088 mm−1, R = 0.045 for 1658 reflections [ I > 2σ( I)]. The title compound is not planar two Schiff base moieties A [C1–C11, O1] and B [N1, C12, C13, N2, C14, C15, C16] are inclined at an angle of 27.4(1)° reflecting mainly the twist about C12–N1 [C11–C12–N1–C13, 29.7(2)°]. There is a strong intramolecular hydrogen bond (O–H···N) of 2.529(2) Å. [ABSTRACT FROM AUTHOR]

Objective: We present our data comparing retrospectively the efficacy of abiraterone and cabazitaxel in patients who progress after docetaxel treatment.Patients and Methods: The study included 56 patients diagnosed with hormone-refractory metastatic prostate cancer who were previously treated with abiraterone therapy at four oncology centers in Turkey.Results: With abiraterone, the patients had a median progression-free survival (PFS) of 5.9 months (95% confidence interval (CI) for hazard ratio (HR) (4.4-7.4)) and an overall survival of 13.4 months (95% CI for HR (5.5-21.3)). When we compared the disease-free survival (DFS) of reference patients treated with cabazitaxel as a second-line treatment with those receiving second-line abiraterone therapy, there was no significant difference. (PFS = 5.9 months with cabazitaxel vs. 6.7 months with abiraterone, P = 0.213).Conclusion: This study has shown that in our experience abiraterone acetate is an effective agent in metastatic castration-resistant prostate cancer (mCRPC) regardless of the line of treatment. [ABSTRACT FROM AUTHOR]

The article presents a case study a 33-year-old female who has been admitted to hospital for the treatment of primary amenorrhea and swelling in inguinal regions. In the study, double-stranded DNA sequencing was performed for screening presence of androgen receptor (AR) exons in which novel mutations were also diagnosed. [ABSTRACT FROM AUTHOR]