Filaments and the underlying surface from He I and H<Emphasis Type="Italic">α</Emphasis> line observations

Bright bands are observed along filaments in the He I 1083 nm line, while both bright and dark bands are observed along Hα 656.3 nm filaments. The range of brightness variations near He I filaments is 1.005–1.10 times the unperturbed brightness, with an average of 1.031 ± 0.01, while this range is 0.91–1.5 times the unperturbed brightness for Hα filaments. The physical state of the matter in these bands is investigated. Computations of the band brightness have been carried out for various chromospheric models, aimed at explaining the observed features of the bands. Two types of models are considered: with temperature or density variations in the upper chromosphere, and with temperature variations in the middle and lower chromosphere. In the first type of model, the brightness in the He I line is changed, but the Hα brightness is not. In the second type of model, only the Hα brightness is changed. Using the variations of the chromospheric parameters and both types of models, we obtained various combinations of band brightnesses in the He I line and in Hα. The brightnesses of regions were estimated by calculating the profiles of the He I and Hα lines in the corresponding models in a non-LTE approximation. A comparison of the observed and calculated quantities indicates that the enhancement in the brightness in the He I line is due to a decrease in temperature or density in the upper chromosphere (where the temperatures are about 10 000–24 000 K). The enhancement and dimming of the brightness in Hα are due to an increase or decrease of the temperature in the middle and lower chromosphere (where the temperatures are 6000–9000 K) by 800–1000 K. The dependence of the band brightness on distance from the center of the solar disk is also considered. The brightness in the He I line increases from the center to the limb by 2–4%. Computations of the center–limb brightness variaions correspond to the observed results.     

时域反射仪（TDR）测定土壤含水量标定曲线评价与方案推荐

时域反射仪（Time Domain Reflectometry）可用于室内和田间快速、 准确、 自动测定土壤含水量, 是目前应用最广泛的土壤含水量测定方法之一。适宜的土壤含水量标定曲线（即土壤表观介电常数和土壤含水量之间的关系）是TDR准确测定土壤含水量的关键。目前文献中存在大量的土壤含水量标定曲线, 但尚未有研究对这些标定曲线进行系统的验证和分析评价。因此, 它们的准确性和适用范围尚不明晰, 严重影响到与土壤含水量测定相关的研究。通过查阅大量国内外文献, 收集整理了一系列土壤含水量标定曲线的经验公式（19个）和半经验半物理模型（5个）, 并利用大量的文献实测数据对其进行综合评价。同时运用均方根差（RMSE）, 平均误差（AD）, 纳什效率系数（NSE）等三个指标对比分析和评价这些标定曲线的准确性和可靠性。研究结果表明： 经验公式中Topp、 Roth（1992）2、 Jacobosen、 Yoshikawa2、 Alharathi模型和半经验模型中Malicki1公式及其修订模型综合性能较好。研究成果可为利用TDR准确测定土壤含水量及土壤含水量标定曲线的选择提供参考和指导。     

Analysis of reflection effects in HS 2333+3927

The results of photometric and spectroscopic observations of the pre-cataclysmic variable HS 2333+3927, which is a HW Vir binary system, are analyzed. The parameters of the sdB subdwarf companion (T _eff = 37 500 ± 500 K, log g = 5.7 ± 0.05) and the chemical composition of its atmosphere are refined using a spectrum of the binary system obtained at minimum brightness. Reflection effects can fully explain the observed brightness variations of HS 2333+3927, changes in the HI and HeI line profiles, and distortions of the radial-velocity curve of the primary star. A new method for determining the component-mass ratios in HW Vir binaries, based on their radial-velocity curves and models of irradiated atmospheres, is proposed. The set of parameters obtained for the binary components corresponds to models of horizontal-branch sdB subdwarfs and main-sequence stars.     

On the mixing processes in estuaries: The fractional freshwater method revisited

A mathematically transparent model for long-term solute dynamics, based on an oscillating reference frame, is applied to the analysis of the mixing process in estuaries. Classical tidally-averaged transport models for estuaries, all derived in some way from the Fractional Freshwater Method of Ketchum (1951) are reinterpreted in this framework. We demonstrate that in these models, the dispersion coefficients obtained from salinity profiles are not always a good representation of the mixing intensity of other dissolved constituents. In contrast, the hypothesis of equal coefficients is always verified in our oscillating coordinate system, which is almost devoid of tidal harmonics. The mathematical representation of the seaward boundary condition is also investigated. In the tidally-averaged Eulerian models, a fixed Dirichlet boundary condition is usually imposed, a condition that corresponds to an immediate, infinite dilution of the dissolved constituent beyond the fixed estuarine mouth. This mathematical representation of the estuarine-coastal zone interface at a fixed location is compared with the case of an oscillating location, which protrudes back and forth into the sea with the tide. Results demonstrate that the mathematical representation of the seaward boundary condition has a significant influence on the resulting mixing curves. We also show how to apply our approach to the prediction of mixing curves in real estuaries.     

Radial-velocity curves and theoretical spectral-line profiles of the components of low-mass close X-ray binary systems

We present the results of calculations of theoretical absorption-line profiles and radial-velocity curves for optical components in X-ray binary systems. Tidal distortion of the optical star and X-ray heating by incident radiation from the relativistic object are taken into account. An emission component forms whose intensity varies with orbital phase in the absorption-line profile in the presence of significant X-ray heating. As a result, the width of the line decreases rather than increases at quadrature. The line profiles and equivalent widths and the radial-velocity curves depend substantially on the parameters of the binary systems. This provides the possibility of directly determining component masses and orbital inclinations from high-resolution spectroscopic observations of X-ray binary systems.     

原状土的剑桥模型和修正剑桥模型

常规剑桥模型和修正剑桥模型是以正常固结和弱超固结土的三轴试验现象为基础建立起来的,且试样的初始应力状态为各向等压的球应力状态,将模型应用于K0固结状态的原状土必然引起不可忽略的系统误差。基于原状土K0固结线与等倾线之间的关系,在常规剑桥模型的基础上推导并得到了基于K0线的原状土剑桥模型和修正剑桥模型。在主应力空间中,该模型以K0固结线而不是以等倾线为轴线,因而能反映原状土的结构性和各向异性。既有试验数据的验证表明,与常规剑桥模型和修正剑桥模型相比,该模型能更合理的描述原状土的屈服和强度特性。     

Interpretation of light curves of the cataclysmic variable OY Car in a model with shockless interaction between a gaseous stream and the disk

To determine the parameters of the accretion disk and shock-wave region responsible for the formation of the orbital peak in the light curve of the binary system OY Car (an SU UMa-type variable), we have analyzed its U BV R and JK light curves using two gas-dynamical models with different regions of shock interaction: one with a hot line along the stream from the Lagrange point L1 and one with a hot spot on the accretion disk. The hot-line model can better describe the quiescent state of the system: the maximum X² for the optical light curves does not exceed 207, whereas the minimum residual for the hot-spot model is X²>290. The shape of the eclipse is almost identical in both models; the main differences are in interpreting out-of-eclipse portions of the light curves, whose shape can varyin the transition from one orbital cycle to another. The hot-spot model is not able to describe variations of the system’s brightness at orbital phases ?～0.1–0.6. The rather complex behavior of the observed flux in this phase interval can be explained in the hot-line model as being due to variations of the temperature and size of the system. Based on the analysis of a sequence of 20 B curves of OY Car, we conclude that the flux variations in the primary minimum are due to variations of the luminosity of the accretion disk, whereas the flux variability in the vicinity of the orbital peak is due to the combined effect of the radiation of the disk and hot line. The JK light curves of OY Car in the quiescent state and during a small flare also indicate preference for the hot-line model, since the primaryminimum and the flux near quadratures calculated using the hot-spot model are not consistent with the observations.     

Interpretation of orbital light curves of U Geminorum

We interpret optical and IR orbital light curves of the dwarf nova U Gem in its quiescent state in the framework of “hot line” and “hot spot” models. The hot-line model provides an adequate fit to the light curves, while the hot-spot model is not fully consistent with the observations. The minimum χ² residuals for the hot-spot and hot-line models are 2203 and 168, respectively.     

Density profiles in molecular cloud cores associated with high-mass star-forming regions

Radial density profiles for the sample of dense cores associated with high-mass star-forming regions from southern hemisphere have been derived using the data of observations in continuum at 250 GHz. Radial density profiles for the inner regions of 16 cores (at distances ≲0.2−0.8 pc from the center) are close on average to the ρ ∝ r ^−α dependence, where α = 1.6 ± 0.3. In the outer regions density drops steeper. An analysis with various hydrostatic models showed that the modified Bonnor-Ebertmodel, which describes turbulent sphere confined by external pressure, is preferable compared with the logotrope and polytrope models practically in all cases. With a help of the Bonnor-Ebert model, estimates of central density in a core, non-thermal velocity dispersion and core size are obtained. The comparison of central densities with the densities derived earlier from the CS modeling reveals differences in several cases. The reasons of such differences are probably connected with the presence of density inhomogenities on the scales smaller than the telescope beam. In most cases non-thermal velocity dispersions are in agreement with the values obtained from molecular line observations.     

基于Monte Carlo-BP神经网络TBM掘进速度预测

预测隧道工程中TBM掘进速度,主要有完全经验的、半理论半经验的模型和人工智能等方法,所用参数均为确定性的,未考虑参数存在的随机性,故导致预测结果的不准确性。基于此,提出了Monte Carlo-BP神经网络TBM掘进速度预测模型,着重考虑了一些重要输入参数的随机性, 其中输入参数重要性的大小通过粗糙集进行计算排序。采用Monte Carlo产生随机数时,由于参量的样本数据的有限,分布函数均采用阶梯形经验分布函数。如果采用的数据是来自不同类型的 TBM,则应当考虑机器性能参数,并重新对参数重要性进行排序。实例计算表明,Monte Carlo-BP神经网络模型预测结果和实测值总体趋势和均值比较一致。     

热力学方法在土体动力Ramberg—Osgood模型中的应用研究

从Ramberg—Osgood模型的骨架曲线和滞回曲线出发,假定塑性中心的移动为直线,构造土体动力耗散函数,从热力学基本定律出发研究了土体动力耗散特性及动力变形机理．提出了反映筑坝堆石料动力特性的第1阌值应变和第2阈值应变,两个阈值应变主要受最大动剪切模量系数、指数及无黏性土的内摩擦角的影响．第1和第2阈值应变间屈服面...     

Non-LTE analysis of the formation of KI lines in the spectra of A-K stars

The non-LTE formation of KI lines in the spectra of A-K stars is analyzed. The computations are based on a 36-level model of the neutral potassium atom for blanketed LTE Kurucz model atmospheres with T _eff=4000–10000 K, logg=0.0–4.5, and [M/H]=(0.0)–(?2.0). The KI atoms in the atmospheres of these stars are in states of moderate and strong “over-recombination.” A number of atomic parameters are refined using the profiles and equivalent widths of five lines in the solar spectrum. The classical van der Waals damping constants must be increased by factors of 2–60 to fit the observed profiles. The non-LTE solar potassium abundance—logε (K)=5.14—corresponds to the meteoritic abundance. Non-LTE corrections to the potassium abundance are important and equal to ?0.4...?0.7 dex for the λ7699 Å line and ?0.15...?0.3 dex for the λλ12522, 12432, and 11769 Å lines.     

The formation of polarized lines: Allowance for the Hanle effect

The paper formulates the standard theory for the transport of polarized radiation in the presence of resonance scattering in an atmosphere with a weak magnetic field, so that the Zeeman splitting is small compared to the Doppler line width. For an atmosphere with conservative scattering, this reduces to the Milne problem, which consists of computing a polarized radiation field in a medium with sources lying in infinitely deep layers. In the approximation of complete frequency redistribution, the problem reduces to solving a Wiener-Hopf integral equation for a (6×6)-matrix source function. Asymptotic and numerical solutions for the standard problem are obtained, including solutions for the Milne problem, for the case of a Doppler absorption profile. The line polarization profiles for the emergent flux at various angular distances from the disk center are derived, and the dependence of the limiting degree of polarization (at the line center at the disk edge) on the direction of the magnetic field is computed. For nearly conservative scattering with photon destruction probability ε?1, the limiting degree of polarization varies with ε in accordance with a simple empirical law similar to that found earlier for a medium with zero magnetic field.     

Surface settlement predictions for Istanbul Metro tunnels excavated by EPB-TBM

In this study, short-term surface settlements are predicted for twin tunnels, which are to be excavated in the chainage of 0 + 850 to 0 + 900 m between the Esenler and Kirazlı stations of the Istanbul Metro line, which is 4 km in length. The total length of the excavation line is 21.2 km between Esenler and Basaksehir. Tunnels are excavated by employing two earth pressure balance (EPB) tunnel boring machines (TBMs) that have twin tubes of 6.5 m diameter and with 14 m distance from center to center. The TBM in the right tube follows about 100 m behind the other tube. Segmental lining of 1.4 m length is currently employed as the final support. Settlement predictions are performed with finite element method by using Plaxis finite element program. Excavation, ground support and face support steps in FEM analyses are simulated as applied in the field. Predictions are performed for a typical geological zone, which is considered as critical in terms of surface settlement. Geology in the study area is composed of fill, very stiff clay, dense sand, very dense sand and hard clay, respectively, starting from the surface. In addition to finite element modeling, the surface settlements are also predicted by using semi-theoretical (semi-empirical) and analytical methods. The results indicate that the FE model predicts well the short-term surface settlements for a given volume loss value. The results of semi-theoretical and analytical methods are found to be in good agreement with the FE model. The results of predictions are compared and verified by field measurements. It is suggested that grouting of the excavation void should be performed as fast as possible after excavation of a section as a precaution against surface settlements during excavation. Face pressure of the TBMs should be closely monitored and adjusted for different zones.     

SP anomaly over doable line of poles-interpretation through log curves

In the analysis and interpretation ofsp anomalies, two-dimensional finite sheet models are equated to the double line of poles. The profiles over such a model being asymmetric with a minor positive peak and a major negative peak, a double logarithmic curve matching technique simpler than that of Meiser is suggested in the paper for easy and unique solution for all values of depth, dip and length. This technique along with a few others have been tested on two profiles across the sulphide deposit from the Rakha Mines, Singhbhum copper belt, India.     

基于附加层法的非规则剖面的瑞利波频散特性研究

对于某些非规则水平层状地质剖面,采用传递矩阵法获得的瑞利波频散曲线可能会出现截止或截断现象,但采用附加层的方法可避免这些现象的发生。通过采用附加层法前后相速度与激发强度大小的对比,来论证附加层法的正确性。对3个典型的非规则剖面进行模拟计算,利用传递矩阵法算得添加附加层前后瑞利波频散曲线,以及某些特征点处位移分量随深度的变化情况。通过对计算结果的对比分析可知,附加层法不仅可计算出地质剖面的实数导波,还可算出其泄漏模式波;在固定的频率点上,附加层的埋深越大,则添加附加层后算得的激发强度大小与原模型的误差越小;当附加层的埋深固定时,添加附加层后计算出的位移曲线与原位移曲线之间的误差随着对比点频率的增大而减小。可见,今后根据实际工作的精度要求,可用附加层法计算某些非规则剖面的瑞利波频散曲线。     

On the dynamics of open clusters

The kinematics of stars in open-cluster models are investigated. The central regions of these model clusters are fairly “cool, ” leading to gravitational instability in the cluster cores. A temporary virilization is observed in the model clusters, during which an appreciable fraction of the fluctuation energy of the cluster is temporarily transformed into the kinetic energy of the peculiar motions of stars. The duration of this stage can reach ∼10⁸ yr. The origins of this temporary virialization of the model clusters are discussed. The instability of the intrinsic fluctuations of the phase density in the centers of six clusters and model clusters is investigated. Several new regions of unstable phase-density fluctuations are found, in addition to those already known. The observed and model clusters can move toward a stable equilibrium state when the density of the cluster core both decreases and increases. The structure of regions of instability of the phase-density fluctuations in the centers of the six clusters is studied. Resonance curves for the amplitudes of steady-state phase-density fluctuations in the center of NGC 6705 are constructed. Analysis of the structure of the regions of instability indicates an appreciable rate of fluctuation-energy loss due to relaxation effects. The instability increments and widths of regions of instability fall off with increasing distance of the cluster from the Galactic center. An important role in the formation of regions of instability may be played by resonances between the frequency of the orbital motion of the cluster in the Galaxy and the frequencies of intrinsic phase-density fluctuations in the centers of the clusters considered.     

Modeling of Spectroscopic and Interferometric Observations of the Herbig Star VV Ser with Hybrid Models

Modeling of hydrogen emission lines is a powerful tool to study physical processes in the nearest vicinity of young stars because spectral lines carry information on the kinematics and physical conditions of the gas. One of the lines that probe emitting regions closest to the star is the Br$$\gamma $$ line. We consider different types of hybrid models to reproduce both interferometric VLTI-AMBER observations and LBT-LUCIFER spectroscopic observations of the single-peak profile of the Br$$\gamma $$ line of the Herbig AeBe star (HAEBE) VV Ser, a member of the UX Ori type subclass. We computed models of a magneto-centrifugal disk wind, a magnetospheric accretion region (magnetosphere), Cranmer’s polar wind, and scattered light from circumstellar polar dust. Furthermore, we calculated hybrid two-component models consisting of a disk wind and one of the aforementioned models. We computed visibilities and line profiles for all types of models and compared them with the available interferometric observations to constrain model parameters. We conclude that for the inclinations reported for this star (60°–70°), the disk wind alone cannot explain the Br$$\gamma $$ line profile although it may be a dominant contributor to the hydrogen line radiation. However, magneto-centrifugal disk wind in combination with aforementioned emitting regions (magnetosphere, polar wind, or scattered light from polar dust) may be able to reproduce the observations.     

Analysis of optical spectra of V1357 Cyg≡Cyg X-1

Optical spectra and light curves of the massive X-ray binary V1357 Cyg are analyzed. The calculations were based on models of irradiated plane-parallel stellar atmospheres, taking into account reflection of the X-ray radiation, asphericity of the stellar surface, and deviations from LTE for several ions. Comparison of observed spectra obtained in 2004?C2005 at the Bohyunsan Observatory (South Korea) revealed variations of the depths of HI lines by up to 18% and of HeI and heavy elements lines by up to 10%. These variations are not related to the orbital motion of the star, and are probably due to variations of the stellar wind intensity. Perturbations of the thermal structure of the atmosphere due to irradiation in various states of Cyg X-1 (including outburst) do not lead to the formation of a hot photosphere with an electron temperature exceeding the effective temperature. As a result, variations of the profiles of optical lines of HI, HeI, and heavy elements due to the orbital motion of the star and variations of the irradiating X-ray flux do not exceed 1% of the residual intensities. Allowing for deviations from LTE enhances the HI and HeI lines by factors of two to three and the MgII lines by a factor of nine, and is therefore required for a fully adequate analysis of the observational data. Analysis of the HI, HeI, and HeII lines profiles yielded the following set of parameters for theOstar at the observing epoch: T _eff = 30 500±500 K, log g = 3.31±0.05, [He/H] = 0.42 ± 0.05. The observed HeI line profiles have emission components that are formed in the stellar wind and increase with the line intensity. The abundances of 11 elements in the atmospheres of V1357 Cyg and ?? Cam, which has a similar spectral type and luminosity class, are derived. The chemical composition of V1357 Cyg is characterized by a strong excess of helium, nitrogen, neon, and silicon, which is related to the binarity of the system.