Raspredelenie posevnoĭ ploshchadi po kulʻturam v % v pereselencheskikh obʻedinenii︠a︡kh Krivorogskogo raĭona

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Plan obʻedinnogo zemelʻnogo otvoda uchastkov kolonizat︠s︡ionnogo fonda "Novyĭ Putʻ" i "N", Krivorogskogo okruga Krivorogskogo raĭona, ploshchadiʻ︠u︡ 1021 desi︠a︡tina

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Vykopirovka s plana uchastka kolonizat︠s︡ionnogo fonda N 417-18-22, Khersonskogo okruga Skadovskogo raĭona pod nazvaniem "3-e Kustovoe Obʻedenenie" predtoznachennogo Narkomzemzemom pod perselenie evreev

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Vykopirovka s plana uchastka kolonizat︠s︡ionnogo fonda N 975b Khersonskogo okruga Skadovskogo raĭona, pod nazvaniem "1 Kustovoe Obʻedenenie" prenaznachennogo Narkomzemom dli︠a︡ perselenii︠a︡ evreev

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3D MHD simulations of subsurface convection in OB stars

During their main sequence evolution, massive stars can develop convective regions very close to their surface. These regions are caused by an opacity peak associated with iron ionization. Cantiello et al. (2009) found a possible connection between the presence of sub-photospheric convective motions and small scale stochastic velocities in the photosphere of early-type stars. This supports a physical mechanism where microturbulence is caused by waves that are triggered by subsurface convection zones. They further suggest that clumping in the inner parts of the winds of OB stars could be related to subsurface convection, and that the convective layers may also be responsible for stochastic excitation of non-radial pulsations. Furthermore, magnetic fields produced in the iron convection zone could appear at the surface of such massive stars. Therefore subsurface convection could be responsible for the occurrence of observable phenomena such as line profile variability and discrete absorption components. These phenomena have been observed for decades, but still evade a clear theoretical explanation. Here we present preliminary results from 3D MHD simulations of such subsurface convection.

Sobre la productio ob caesuram de sílaba abierta en el hexámetro latino

[ES] La posibilidad de contar como larga una sílaba breve acabada en consonante y ante cesura es una licencia que, aunque utilizada parcamente por todos los poetas latinos de la Antigüedad, siempre ha sido reconocida como tal. No ocurre lo mismo con los casos de alargamiento en sílaba abierta: rodeados de problemas de diverso tipo, han sido vistos con frecuencia como un fenómeno distinto del anterior. A partir de los testimonios de algunos gramáticos antiguos, se postula la existencia de una estricta prohibición de tales alargamientos de sílabas abiertas a partir de mediados del siglo I d.C.

A study of the reproductive biology of dace in the middle Ob [introduction , summary and table captions only] [Translation from: Trudy tomsk. gos. Univ. 125, pp.77-91]

The Siberian Dace (Leuciscus leuciscus baicalensis (Dyb)is an important trade fish in Siberian waters. In the Ob basin more than 30,000 centners are produced annually. Catches of dace fluctuate significantly both between different rivers and between years in the Tomsk region. Defining the stocks of dace in the waters of the Tomsk region and explaining the fluctuations over time seems to be a very important and relevant question for the workers of the fishing industry. An answer, however, requires an accurate knowledge of the biology of dace; its reproductive, feeding and migration habits and the conditions of wintering etc. In the following we examine one of the above questions i.e. the biology of the reproduction of dace. The study was carried out in the Middle Ob in May 1951. This tranlations provides the introduction, summary and table captions only of the original article.

Sobre la "productio ob caesuram" de sílaba abierta en el hexámetro latino

[ES] La posibilidad de contar como larga una sílaba breve acabada en consonante y ante cesura es una licencia que, aunque utilizada parcamente por los poetas latinos de la Antigüedad, era y es reconocida por todos los filólogos como tal licencia. No ocurre lo mismo con los casos de alargamiento en sílaba abierta: rodeados de problemas de diverso tipo, han sido vistos con frecuencia como un fenómeno distinto del anterior. El autor de este artículo propone una lectura de algunos testimonios de los gramáticos latinos antiguos que permite postular la existencia de una estricta prohibición de estos alargamientos de sílabas abiertas a partir de mediados del siglo I d. C.

高原鼠兔ob基因的组织表达特征

ob基因编码的leptin蛋白在调节生物体能量平衡中起到重要作用。本研究应用Taqman探针real time PCR技术对高原鼠兔ob基因的组织分布进行检测。通过提取不同组织总RNA，经DNase I消化后，用随机引物进行反转录合成cDNA，采用特异性Taqman探针和引物分别对ob基因及β-actin基因进行实时定量PCR扩增，对不同组织中ob基因和β-actin基因的初始拷贝数之比进行比较。结果表明ob基因在脑、心脏、肺、肝脏、脾脏、肾脏、骨骼肌、脂肪组织中均有表达，其中以白色脂肪组织中ob基因表达量最高，其次为心脏和肺，表达量最低的是肝脏和肾脏。

Effects of the novel (Pro(3))GIP antagonist and exendin(9-39)amide on GIP- and GLP-1-induced cyclic AMP generation, insulin secretion and postprandial insulin release in obese diabetic (ob/ob) mice: evidence that GIP is the major physiological incretin

AIMS/HYPOTHESIS: This study examined the biological effects of the GIP receptor antagonist, (Pro3)GIP and the GLP-1 receptor antagonist, exendin(9-39)amide.

METHODS: Cyclic AMP production was assessed in Chinese hamster lung fibroblasts transfected with human GIP or GLP-1 receptors, respectively. In vitro insulin release studies were assessed in BRIN-BD11 cells while in vivo insulinotropic and glycaemic responses were measured in obese diabetic ( ob/ ob) mice.

RESULTS: In GIP receptor-transfected fibroblasts, (Pro(3))GIP or exendin(9-39)amide inhibited GIP-stimulated cyclic AMP production with maximal inhibition of 70.0+/-3.5% and 73.5+/-3.2% at 10(-6) mol/l, respectively. In GLP-1 receptor-transfected fibroblasts, exendin(9-39)amide inhibited GLP-1-stimulated cyclic AMP production with maximal inhibition of 60+/-0.7% at 10(-6) mol/l, whereas (Pro(3))GIP had no effect. (Pro(3))GIP specifically inhibited GIP-stimulated insulin release (86%; p<0.001) from clonal BRIN-BD11 cells, but had no effect on GLP-1-stimulated insulin release. In contrast, exendin(9-39)amide inhibited both GIP and GLP-1-stimulated insulin release (57% and 44%, respectively; p<0.001). Administration of (Pro(3))GIP, exendin(9-39)amide or a combination of both peptides (25 nmol/kg body weight, i.p.) to fasted (ob/ob) mice decreased the plasma insulin responses by 42%, 54% and 49%, respectively (p<0.01 to p<0.001). The hyperinsulinaemia of non-fasted (ob/ob) mice was decreased by 19%, 27% and 18% (p<0.05 to p<0.01) by injection of (Pro3)GIP, exendin(9-39)amide or combined peptides but accompanying changes of plasma glucose were small.

CONCLUSIONS/INTERPRETATION: These data show that (Pro(3))GIP is a specific GIP receptor antagonist. Furthermore, feeding studies in one commonly used animal model of obesity and diabetes, (ob/ob) mice, suggest that GIP is the major physiological component of the enteroinsular axis, contributing approximately 80% to incretin-induced insulin release.

Chemical abundances and winds of massive stars in M31: a B-type supergiant and a WC star in OB 10

We present high quality spectroscopic data for two massive stars in the OB 10 association of M31, OB 10-64 (B0 la) and OB 10-WRI (WC6). Medium resolution spectra of both stars were obtained using the ISIS spectrograph on the William Herschel Telescope. This is supplemented with Hubble Space Telescope STIS UV spectroscopy and Keck I HIRES data for OB 10-64. A non- local thermodynamic equilibrium (LTE) model atmosphere and abundance analysis for OB 10-64 is presented, indicating that this star has similar photospheric CNO, Mg and Si abundances to solar neighbourhood massive stars. A wind analysis of this early B-type supergiant reveals a mass-loss rate of (M)over dot = 1.6 x 10(-6) M-circle dot yr(-1), and v(infinity) = 1650 km s(-1). The corresponding wind momentum is in good agreement with the wind momentum-luminosity relationship found for Galactic early-B supergiants. Observations of OB 10-WRI are analysed using a non-LTE, line-blanketed code, to reveal approximate stellar parameters of log L/L-circle dot similar to 5.7, T-* - 75 kK, v(infinity) similar to 3000 km s(-1), (M)over dot/(M-circle dot yr(-1)) similar to 10(-4.3) adopting a clumped wind with a filling factor of 10 per cent. Quantitative comparisons are made with the Galactic WC6 star HD 92809 (WR23) revealing that OB 10-WR1 is 0.4 dex more luminous, though it has a much lower C/He ratio (similar to0.1 versus 0.3 for HD 92809). Our study represents the first detailed, chemical model atmosphere analysis for either a B-type supergiant or a Wolf- Rayet (WR) star in Andromeda, and shows the potential of how such studies can provide new information on the chemical evolution of galaxies and the evolution of massive stars in the local Universe.

Chemical composition of B-type supergiants in the OB 8, OB 10, OB 48, OB 78 associations of M 31

Absolute and differential chemical abundances are presented for the largest group of massive stars in M31 studied to date. These results were derived from intermediate resolution spectra of seven B-type supergiants, lying within four OB associations covering a galactocentric distance of 5-12 kpc. The results are mainly based on an LTE analysis, and we additionally present a full non-LTE, unified model atmosphere analysis of one star (OB 78-277) to demonstrate the reliability of the differential LTE technique. A comparison of the stellar oxygen abundance with that of previous nebular results shows that there is an off set of between similar to0.15-0.4 dex between the two methods which is critically dependent on the empirical calibration adopted for the R 23 parameter with [O/H]. However within the typical errors of the stellar and nebular analyses (and given the strength of dependence of the nebular results on the calibration used) the oxygen abundances determined in each method are fairly consistent. We determine the radial oxygen abundance gradient from these stars, and do not detect any systematic gradient across this galactocentric range. We find that the inner regions of M31 are not, as previously thought, very "metal rich". Our abundances of C, N, O, Mg, Si, Al, S and Fe in the M31 supergiants are very similar to those of massive stars in the solar neighbourhood.