Observational Manifestations of the Precessional Wave in the Accretion Disk of a Cataclysmic Variable Star

Effects due to the interaction of the steam from the inner Lagrangian point with the accretion disk in a cataclysmic variable star are considered. The results of three-dimensional gas-dynamical numerical simulations confirm that the disk thickness in the vicinity of the interaction with the stream is minimum when the component-mass ratio is 0.6. As a consequence, some of the matter from the stream does not collide with the outer edge of the accretion disk, and continues its motion unperturbed toward the accretor. This part of the stream subsequent interacts (collides) with a thickening of the accretion disk due to the presence of a precessional wave in the disk, leading to the appearance of an additional zone of heating at the disk surface. This additional zone of enhanced luminosity (hot spot) is a direct observational manifestation of the precessional wave in the accretion disk.     

金试剂在光度分析中的应用

介绍了金试剂的性质,并对金试剂在Ａｕ,Ａｇ,Ｐｔ,Ｐｄ,Ｉｒ,Ｈｇ,Ｔｌ和Ｃｕ光度分析中的应用进行了综述,引用参考文献２６篇。     

吡啶偶氮类试剂在光度分析中的应用进展

吡啶偶氮类试剂是一类性能优良的络合滴定指示剂和光度显色剂,迄今已合成了200余种,在分光光度分析测定各种金属离子方面得到了广泛的应用。为了进一步改善这类试剂的灵敏度和选择性等分析性能,近年深入研究了吡啶偶氮类试剂的结构与性能的关系,进而相继开发出一系列性能优异的吡啶偶氮类试剂。文章综述了1990—2010年以来常见的吡啶偶氮类试剂及其在分光光度分析测定金属离子方面的进展。从反应体系、最大吸收波长、灵敏度、线性范围等方面归纳了吡啶偶氮类试剂在实际样品中的应用情况,为此类试剂的开发和应用提供一些理论依据。     

Parameter Determination for the Eclipsing Long-Period Dwarf Nova EX Dra from Photometric Observations during Different Activity States of the System

Astronomy Reports - The results of a long-term photometric observations of the cataclysmic variable EX Dra acquired between 2014 and 2016 at the Crimean Station of the Sternberg Astronomical...     

藏南深反射测线附近地表地质观察研究成果

本文简要介绍了ＩＮＤＥＰＴＨ项目地质组１９９４年和１９９５年间沿ＩＮＤＥＰＴＨ—Ｉ路线进行的野外填图工作的初步研究成果。它们是：①在帕里西北确定了高喜马拉雅与特提斯喜马拉雅之间拆离带的存在；③在帕里北发现了一套特提斯沉积，从而提出帕里西北的拆离带有可能穿过南北方向的亚东－谷露裂谷，而没有大规模错开；③在特提斯喜马拉雅带中确定了两条具一定规模的逆冲断裂；④发现康马穹窿存在两期构造变形，早期为上盘向北运动，晚期为横弯造穹作用。最后，结合深反射资料进一步讨论了康马穹窿与藏南拆离带之间的关系。     

山东沂沭地区白垩纪地层的新观察

１９９２年李庆年、赵风江在沂沭断裂带内建立了大盛群,其中包括同时命名的马朗沟组、田家楼组、寺前村组,时代定为早白垩世。在考察中笔者肯定了这项成果,同时根据笔者的认识进行了调整和修订,将马朗沟组易名,沿用莱阳－诸城地区的陡山组;新建小黑沟组;修订了原“田家楼组”的涵义;废除大盛群,将这３个组归入青山群;取消寺前村组,沿用莱阳－诸城地区的辛格庄组,归入王氏群。     

New Observations on the Brittle Failure Process of Simulated Crystalline Rocks

A biaxial testing program has been performed to study the process of brittle failure in crystalline rocks. Dental plaster has been selected as a model material, and mixing with different ratios of distilled water, different types of common minerals of crystalline rocks have been simulated in the form of brick-like small elements. These elements have been interlocked together according to four systematic patterns and final specimens with 180 × 180 × 76 mm dimensions have been obtained. Details of different types of cracks observed during loading process, effects of mechanical, geometrical and confining pressure on the cracking intensity, the influence of different types of heterogeneity on the macroscopic properties of a system of interlocked elements, and the sequence of events during the failure process are presented in this paper. Based on these observations, a revised mechanism for brittle failure is proposed.     

A New Model Emerged from the Three-body Problem within Frame of Variable Mass

Astronomy Reports - In this work, we have revealed a new model emerged from the restricted three-body problem within a framework of a non-isotropic variation of mass. This variation is taken when...     

Determination of Fluorine and Chlorine in Eight USGS Reference Samples Using Automated Photometric Analysis

Eight USGS reference samples have been analysed for F and Cl by automated photometric analysis following alkali fusion. The results obtained are, generally, in fairly good agreement with those quoted in the literature.     

New Data on Seismotectonics of the Laptev Sea from Observations by Ocean Bottom Seismographs

Doklady Earth Sciences - The results of new local seismic observations in the Laptev Sea obtained using ocean bottom seismographs were compared with actual data from global and regional earthquake...     

模糊可变集合方法在降雨相似性分析中的应用

基于特定流域场次降雨具有的相似性,应用考虑区间值模糊可变的模糊可变集合方法进行场次降雨相似性分析。通过计算各场次降雨隶属于各降雨级别的特征值及与目标场次降雨之间的相似距离,从而获得流域场次降雨相似性排序,有效解决了场次降雨相似分析中的模糊性和不确定性问题。找出与实时阶段场次降雨相似的历史场次降雨,预估水库实时阶段面临的洪水过程及量级,可为水库防洪调度提供信息参考。     

Observations and controls on the occurrence of inherited zircon in Concord-type granitoids,New Hampshire

U-Pb analyses of zircons separated from two Concord-type plutons near Sunapee and Dixville Notch, New Hampshire, reveal differences in the pattern and magnitude of zircon inheritance which are related to differences in melt chemistry. The Sunapee pluton contains only slightly more Zr than required to saturate the melt at the peak temperature of 700 ± 30°C. Traces of inherited zircon in this separate are inferred to be present as small, largely resorbed grains. In contrast, the Long Mountain pluton, near Dixville Notch, contains about 240% more Zr than required to saturate the melt. Thus, more than half of the Zr existed as stable, inherited zircon crystals during the partial fusion event, consistent with the observation of substantial inheritance in all grain size fractions. Ion probe intra-grain analyses of zircon from the Long Mountain pluton indicate a complex pattern of inheritance with contributions from at least two Proterozoic terrenes and caution against simple interpretations of upper and lower intercepts of chords containing an inherited component. Ion probe analyses of zircons from the Sunapee pluton reveal clear evidence of U loss which results in incorrect apparent conventional U-Pb ages. Ages of crystallization for the Long Mountain and Sunapee pluton are ~350 and 354 ± 5 Ma, respectively. A Sm/Nd measurement for the Long Mountain pluton yields a depleted mantle model age of 1.5 Ga, consistent with the observed inheritance pattern. In contrast, a Sm/Nd model age for the Sunapee pluton is improbably old due to minor monazite fractionation.     

青藏高原北麓河地区降水量观测与对比分析

根据2011年11月至2012年9月通过Thies激光雨滴谱仪、 T-200B雨雪量计和TE525翻斗式雨量筒获取的青藏高原北麓河地区降水量数据, 按3个时间段分别对3种仪器记录的降水量行了对比分析. 结果表明: 激光雨滴谱仪获取的固态降水量与经Jimmy校正公式修正后的T-200B降水量极为接近. 但在测量雨夹雪时, 激光雨滴谱仪对降水类型、 颗粒直径的误判造成了获取的降水量远高于T-200B雨量筒. 而3种仪器获取的液态降水量有很好的一致性. 但是, 当小时降雨量在2 mm以上时, 激光雨滴谱仪获取的降雨量比T-200B和TE525雨量筒小20%左右. 同时, 在风吹雪对激光雨滴谱仪的影响方面做了相关的分析研究, 初步认为风吹雪的颗粒直径主要集中在0.5 mm以下.     

Photometric parameters of the dwarf nova SS Cygni in the quiescent state

The mean 1983–1996 UBV light curves of the dwarf nova SS Cyg are used to derive the binary parameters in the quiescent state. Solutions are obtained for a classical hot-spot model and a model with an energy source lying outside the accretion disk. Photometric and spectroscopic data are combined to infer the masses and radii of the binary components. The white dwarf in SS Cyg is one and a half times as massive as the red dwarf, q=M _wd /M _rd ～1.45, M _rd ～0.46M _⊙ and M _wd ～0.66M _⊙. The orbital inclination of the system is i?51°–54°. The contribution of the accretion disk to the total flux in the quiescent state is estimated to be ～47–49% and ～54% in the VU and B filters, respectively. The hot spot contributes less than ～3% to the total optical flux. In the “non-classical” hot-spot model, the disk and bulge contributions are 27 and 2–8%, respectively, depending on the orbital phase. The shape of the mean light curves of SS Cyg suggests asymmetric heating of the red-dwarf surface in the quiescent state by high-temperature radiation generated in the hot-spot region.     

Long-Term Geophysical Observations and Analysis of the World’s Deepest Borehole

正Objective In order to reduce the interfering noise from the earth surface,scientists have carried out multi-geophysical borehole observations and the related study.This study aims at improving signal-to-noise ratio obtained from the     

The Use of Photometric Structural Analysis and Digitized Positional Observation Data to Study Small Celestial Bodies

Astronomy Reports - The problems of the study of small celestial bodies are an important component of modern space research. This applies both to the study of physicochemical and evolutionary...     

Photometric elements and apsidal motion of the eclipsing binary ES Lac

We have obtained high-accuracy photoelectric measurements of ES Lac, an eclipsing binary with an elliptical orbit (B9III + B9III; P = 4.459^d, e = 0.198) in 1985–2004 at the Sternberg Astronomical Institute’s Tien Shan High-Altitude Observatory. Our detailed analysis of the 19-year uniform series of measurements has yielded the first photometric elements for this system, as well as a self-consistent set of physical and geometrical parameters for the binary. The virtually identical components (M ₁ = M ₂ = 3.0 M _⊙; R ₁ = R ₂ = 4.12 R _⊙) are appreciably separated from the main sequence, and are located on the giant branch: their age is t = (3.5 ± 0.2) × 10⁸ yrs. An analysis of our observations together with previously published times of minima has enabled a considerable refinement of the period of the apsidal motion, U = 355 ± 20 years, and a first determination of the apsidal parameter reflecting the radial density distributions for the components stars: k ₂ ^obs = 0.00213(18). This value is in a good agreement with the value expected theoretically for current evolutionary models of such stars: k ₂ ^th = 0.00257(15).     

Photometric observations of R Coronae Borealis in the optical and infrared

The results of long-term photometric observations of R CrB in the UBV JHKLM bands are presented. The temporal and color characteristics of the emission of the star itself and of its extended dust envelope are analyzed in detail. No stable harmonic has been found in the semiregular variations of the optical brightness of R CrB. Two harmonics with periods P≈3.3 and 11.3 yrs have been detected in the brightness variations of the dust envelope; the minima of these variations coincided in 1999, resulting in a record decrease in the LM brightness of the envelope. This by chance coincided in time with a deep minimum of the visual brightness of the star, resulting in a unique decrease in the total brightness of the star and dust envelope. This enabled estimation of the bolometric flux of the hot dust clouds, which made up only a few per cent of the bolometric flux of the dust envelope. The brightness variations of the dust envelope are not accompanied by appreciable color changes and are associated with variations of its optical depth τ(V) in the range 0.2–0.4. The dust envelope forms at a large and fairly constant distance from the star $(r_{in} \approx 110R_* ,T_{gr} \approx 860 K)$ , from material in its stellar wind, whose intensity $(\dot M_{gas} \approx 2.1 \times 10^{ - 7} M_ \odot /year)$ obeys a Reimers law. No variations synchronous with those of the optical depth of the dust envelope, in particular, with the period P≈3.3 yrs, have been found in the optical emission of R CrB, suggesting that the stellar wind is not spherically symmetric. The dust envelope consists of small grains (a _gr≤0.01 µm), while the clouds screening the star from the observer are made up of large grains (a _gr≈0.1 µm). The activity of R CrB, whose nature is unclear, is reflected in variations of the stellar-wind intensity and the appearance of dust clouds in the line of sight: these variations are repeated by corresponding changes in the optical depth of the dust envelope with a delay of ～4 years (the time for a particle moving at V _env≈45 km/s to move from the star to the boundary of the dust envelope).     

Photometric study of an SX Phoenicis variable in the galactic halo

We have studied the relatively recently discovered object 2-7-0122, with a V magnitude of 17 ^m , and have confirmed that it is an SX Phe variable star. Our photometry at the 1.8 m telescope of the Boyhunsan Observatory and the 1.0 m telescope of the Mount Lemon Observatory has enabled us to refine the photometric elements and to perform a frequency analysis of the light curve. We demonstrate the presence of two close frequencies, f ₁ = 24.6539 cycles/day and f ₂ = 24.8173 cycles/day, one of them possibly non-radial, and of several combinational frequencies. The star’s metallicity is at least two orders of magnitude lower than that of the Sun, making the star the most metal-poor SX Phe object in the Galactic field. We confirm variability of another star in the field of view, and have determined its light elements and its possible variability type (RRc).