The evolutionary status of UX CVn

We have analyzed available spectroscopic and photometric observations of the close binary UX CVn using model atmospheres. Theoretical spectra and light curves were derived from models of a precataclysmic variable and a close binary consisting of degenerate stars. We have used the 6-m telescope of the Special Astrophysical Observatory to obtain ten moderate-resolution spectra at three orbital phases. Our analysis of the radial-velocity curve shows that the orbital period of the system has been stable over 40 yrs, and the variations of the intensities of lines of various elements at different phases and radial velocities indicates an absence of the reflection effect. As a result, we have classified UX CVn as a detached close binary consisting of a hot, low-luminosity sub-dwarf primary and a white-dwarf secondary.     

Lithium lines in the spectra of M dwarfs: UX Tau C

The results of numerical modeling of lithium lines in the spectra of M dwarfs are discussed. The behavior of the lithium lines relative to the local pseudocontinuum formed by molecular bands is analyzed as a function of model atmosphere parameters: effective temperature T _eff, gravity logg, and metallicity μ The molecular opacity was computed using the just overlapping line approximation (JOLA) and “line-by-line” methods. The pseudo-equivalent widths of lithium lines depend appreciably on metallicity μ and weakly on T{nteff}. The lithium abundance in the atmosphere of UX Tau C is redetermined. Previous studies underestimated the lithium abundance in this star as a result of the use of insufficiently accurate molecular-line lists. The new lithium abundance log N (Li)=3.2±0.3was derived by comparing the observed profiles of the 670.8 nm resonance doublet lines with profiles calculated using the new TiO line list of Plez.¹ The new abundance agrees with the atmospheric lithium abundances of the other two components in the stellar system, providing further evidence that the three stars in the UX Tau system have the same age. A comparison of the observed spectra of UX Tau C near the lithium resonance doublet (665–680 nm) with spectra computed using JOLA and line-by-line methods suggests that the list of Plez is the best currently available.     

Unusual Eclipse of the UX Ori Type Star V719 Per

Astronomy Reports - The results of new photometric ( $$VRI$$ ) observations of the young star V719 Per from the IC 348 cluster are presented. Up until 2014, this star demonstrated brightness...     

Photometric activity of UX orionis stars and related objects in the near infrared and optical: CO Ori,RR Tau,UX Ori,and VV Ser

This paper continues a study of the photometric activity of UX Ori stars in the optical and near-infrared (JHKLM bands) initiated in 2000. For comparison, the list of program stars contains two Herbig Ae stars that are photometrically quiet in the optical: MWC480 andHD179218. Fadings ofUXOri stars in the optical (V band) due to sporadic increases of the circumstellar extinction are also observed in the infrared (IR), but with decreasing amplitude. Two stars, RR Tau and UX Ori, displayed photometric events when V -band fadings were accompanied by an increase in IR fluxes. Among the two Herbig Ae stars that are photometrically quiet in the optical, MWC 480 proved to be fairly active in the IR. Unlike the UX Ori stars, the variation amplitude of MWC 480 increases from the J band to the M band. In the course of the observations, no deep fadings in the IR bands were detected. This indicates that eclipses of the program stars have a local nature, and are due to extinction variations in the innermost regions of the circumstellar disks. The results presented testify to an important role of the alignment of the circumstellar disks relative to the direction towards the observer in determining the observed IR variability of young stars.     

Diagnostics for accretion disks around UX Ori stars based on Balmer, Paschen, and Brackett Lines

We have modeled the H_α, H_β, and H_γ (Balmer series), P₁₄ (Paschen series), and Br_γ (Brackett series) hydrogen lines formed in the inner regions of the accretion disk around the Herbig Ae star UX Ori. Our calculations are based on spectra obtained with the Nordic Optical Telescope (NOT) and the IRTF. We computed a grid of non-LTE models for a radiating area in the accretion disk and determined the basic parameters of the lines using the method of Sobolev. Analyzing the theoretical and observed line profiles, equivalent widths, and luminosities, we have estimated the accretion rate and electron-temperature distribution in the inner parts of the accretion disk. The accretion rate of UX Ori is about $\dot M_a = (3 - 10) \times 10^{ - 9} M_ \odot /yr$ , and the temperature distribution is consistent with the power law T(r)=T(r _*)(r/r _*)^?1/n , where the electron temperature near the stellar surface T(r _*) is 15000–20000 K and the power-law index n≈2–3 is about two to three. The resulting value for $\dot M_a $ eliminates problems connected with the application of magnetospheric accretion models to Herbig Ae/Be stars. Another important conclusion is that, at the estimated accretion rate, the energy release is substantially (about two orders of magnitude) lower than the stellar luminosity. Therefore, the optical radiation of UX Ori accretion disks cannot appreciably contribute to the observed variability of these stars, which must be determined mainly by variability in the circumstellar extinction.     

Structure of the accretion disk in the cataclysmic variable UX UMa in the transition to its quiescent state

Our analysis of BV RI light curves for the cataclysmic variable UX UMa obtained in intermediate activity states, in the transition between the active and quiescent states of the system on March 12, 1997 and May 3, 2000, shows that the shapes of these light curves cannot be adequately described using the standard hot-spot model. A model with a “hot line” near the edge of the disk and a two-armed spiral structure on the disk surface reproduces much better out-of-eclipse variations in the light curves. The presence of an extended hot line can explain the anomalous shape of the I light curve on March 12, 1997. The decrease in the observed luminosity of the system between March 12, 1997 and May 3, 2000 could be due to a decrease in the disk luminosity by a factor of 2–2.5; the higher disk luminosity on the earlier date is associated with appreciable deviations of the radial temperature distribution of the disk material from that for the standard model. The phases and depths of dips in the out-of-eclipse sections of the UX UMa light curves are due primarily to the parameters of the complex shape of the accretion disk, which has a spiral structure located mainly near its outer edge. The contribution of the spiral arms in the V filter reaches 20–50% of the total disk radiation. The crest of the first spiral wave in our model maintains its approximate position in azimuth; this structure could represent a bulge in a halo at the outer edge of the disk near orbital phases φ ～ 0.7, in the direction of the continuation of the extended shock in the disk itself. The position of the crest of the second spiral arm changes with time. This structure may represent a one-armed spiral wave near the apastron of the weakly elliptical disk. Finally, the observations testify to the presence of another spiral arm that is les clearly manifest in terms of both its luminosity and its height above the unperturbed disk surface. Thus, in an intermediate activity state of UX UMa, the surface of the accretion disk is distorted by the action of a two-armed spiral structure in the outer regions of the disk, which is asymmetric in both its luminosity and dimensions, and a bulge at the disk edge in the region of its interaction with the inflow to the disk.     

Modeling of Hydrogen Emission Lines in the Spectrum of UX Ori in Its Bright State and during Eclipses

Astronomy Reports - The hydrogen spectrum of the UX Ori-type star is modeled in a bright state and during an eclipse by an opaque dusty fragment of its own protoplanetary disk. The disk wind is...     

Atmospheric lithium abundances of the carbon giants AQ And,HK Lyr,UX Dra,and WZ Cas

The LTE lithium abundances, logN (Li), have been determined for the atmospheres of the four carbon giants AQ And, HK Lyr, UX Dra, and WZ Cas, applying the synthetic-spectrum technique to the LiI λ670.8 nm resonance doublet. We used estimates of the effective temperatures T _eff, metallicities, elemental abundances, and carbon-isotope ratios for these stars from the literature [12C/13C]. The resulting lithium abundances depend significantly on the adopted T _eff, so that we can find each star’s range of possible logN(Li) values for a given range of effective temperatures (ΔT _eff = 200−300 K). The uncertainty in the derived logN(Li) values is 1.3 for AQ And and UX Dra, 0.5 for HK Lyr, and 0.8 for WZ Cas. Our most probable logN(Li) values (or ranges) are −1.25 for AQ And, −1.2 for HK Lyr, −1.0 ≤ logN(Li) ≤ +0.3 for UX Dra, and 4.3 ≤ logN(Li) ≤ 4.8 for WZ Cas. The derived C/O ratios for the stellar atmospheres also depend on T _eff. Possible uncertainties in other atmospheric parameters do not change logN(Li) by more than 0.2.     

流域地貌参数影响因子分析

在流域地貌特征提取中采用AGREE算法的关键技术,将水系形态特征融入数字高程模型形成水文数字高程模型。通过分析不同集水阈值(0.2km2、1km2、2km2、3km2、4km2、5km2)、不同比例尺(万分之一、5万分之一、25万分之一)、不同流域面积标准(0.2km2、1km2、2km2、3km2、4km2、5km2)下流域地貌参数,得出地貌参数的稳定性与河流分级有关,当河流级别达到5级时,参数不随比例尺、集水阈值、面积标准变化而变化。在缺资料地区洪水预报中,只要具备一定精度的地形数据及相应水系,即可满足流域地貌参数的获取。地貌瞬时单位线法相对较稳定,适用于无资料地区中小流域洪水预报。     

Hybrid Estimation of Semivariogram Parameters

Two widely used methods of semivariogram estimation are weighted least squares estimation and maximum likelihood estimation. The former have certain computational advantages, whereas the latter are more statistically efficient. We introduce and study a “hybrid” semivariogram estimation procedure that combines weighted least squares estimation of the range parameter with maximum likelihood estimation of the sill (and nugget) assuming known range, in such a way that the sill-to-range ratio in an exponential semivariogram is estimated consistently under an infill asymptotic regime. We show empirically that such a procedure is nearly as efficient computationally, and more efficient statistically for some parameters, than weighted least squares estimation of all of the semivariogram’s parameters. Furthermore, we demonstrate that standard plug-in (or empirical) spatial predictors and prediction error variances, obtained by replacing the unknown semivariogram parameters with estimates in expressions for the ordinary kriging predictor and kriging variance, respectively, perform better when hybrid estimates are plugged in than when weighted least squares estimates are plugged in. In view of these results and the simplicity of computing the hybrid estimates from weighted least squares estimates, we suggest that software that currently estimates the semivariogram by weighted least squares methods be amended to include hybrid estimation as an option.     

土壤水分对土壤参数的敏感性及其参数优化方法研究

利用2008年1月1日至2009年9月31日黑河流域阿柔冻融观测站的气象和土壤水分数据,采用基于方差的多参数敏感性分析方法研究通用陆面模型（Common Land Model,CoLM）模拟的土壤水分对土壤质地（砂土和黏土）的敏感性,进而采用SCE-UA参数优化算法分别优化土壤质地和土壤水力参数,分析不同优化策略对土壤水分模拟结果的影响。研究结果表明,浅层土壤水分对土壤质地较为敏感,敏感性系数达到了0.45以上,并且砂土含量对土壤水分的影响更为显著;利用SCE-UA算法优化土壤质地或土壤水力参数都可以有效地提高土壤水分的模拟精度,优化土壤水力参数易产生＂异参同效＂现象,而优化土壤质地能够使土壤水力参数的取值范围更加合理。     

Bayesian Inference of Spatial Covariance Parameters

This paper shows the application of the Bayesian inference approach in estimating spatial covariance parameters. This methodology is particularly valuable where the number of experimental data is small, as occurs frequently in modeling reservoirs in petroleum engineering or when dealing with hydrodynamic variables in groundwater hydrology. There are two main advantages of Bayesian estimation: firstly that the complete distribution of the parameters is estimated and, from this distribution, it is a straightforward procedure to obtain point estimates, confidence regions, and interval estimates; secondly, all the prior information about the parameters (information available before the data are collected) is included in the inference procedure through their prior distribution. The results obtained from simulation studies are discussed.     

Analysis of Varation of Clay Consolidation Parameters

Based on the fundamental conception soil mechanics, by experimental research, the relation of the coefficient of permeability K to the void ratio e and that of the coefficient of compression aγ to the effective consolidation pressureσ’ are first expressed for normally consolidation clays. Hences the expression of relation of the consolidation coefficient cν to the void ratio e or the effective consolidation pressures is given. There are three typical cases of variation of the consolidation coefficient for different soils types, i.e. the value Cν decreases with the void ratio’s decrease; the value Cν increases with the void ratio’s decrease and the value Cν is essentially independent of the void ratio. Specific variation of the value Cν for specifically soil type is pointed out. The physical foundation for the variation of consolidation index m is explained. The relationships between the value m, the effective consolidation pressure σ’ and the soil layer thickness H are discussed. Finally, correlation between the value Cν and m’s variation as well as the noteworthy problems in practice are represented.     

粘土固结参数变化的分析

本文依据土力学中已建立的基本概念,通过试验研究,首先找出正常固结粘土的渗透系数K与孔隙比e的关系,压缩系数a_V与孔隙比e或有效固结压力σ′的关系,从而推导出固结系数C_V与孔隙比或有效固结压力的关系表达式。分析不同土类固结系数的变化,归纳出三种典型的情况,即:C_V随e的减小而减小;C_V随e的减小而增大和C_V基本上与e无关。并指出特殊土类的C_V有特殊的变化规律。其次,分析了固结指数m变化的物理依据,讨论了m值与有效固结压力和上层厚度H的关系,最后,说明C_V和m变化的相互关系以及实用计算中应注意的问题。     

水文地质参数计算方法探讨

阐述了水文地质参数的重要性,及其发展和尚需完善的方面。推出可以解决基岩裂隙、溶隙含水层坐标距离与水力距离不一致问题的导水系数计算方法。该方法的特点是简捷,能较直观地判别含水层主要水文地质参数的大小,具有很高的可靠性。     

Energy Parameters of Ore-Forming Deep Fluid Systems

The energy parameters of ore-forming deep fluid systems (enthalpy and Gibbs free energy) for compounds of S, Cl, and B have been estimated by thermodynamic methods at a lithosphere depth of 1000–20 km. At a depth of 1000 km, ore-forming fluids are dominated by BF₃. With a decrease in a depth to 100–20 km, the range of fluid ore-forming systems becomes wider due to the B, F, Cl, and S compounds providing a real basis for development of the voluminous ore-forming fluid systems at the top of the lithosphere.     

Maximum Likelihood Estimation of Spatial Covariance Parameters

In this paper, the maximum likelihood method for inferring the parameters of spatial covariances is examined. The advantages of the maximum likelihood estimation are discussed and it is shown that this method, derived assuming a multivariate Gaussian distribution for the data, gives a sound criterion of fitting covariance models irrespective of the multivariate distribution of the data. However, this distribution is impossible to verify in practice when only one realization of the random function is available. Then, the maximum entropy method is the only sound criterion of assigning probabilities in absence of information. Because the multivariate Gaussian distribution has the maximum entropy property for a fixed vector of means and covariance matrix, the multinormal distribution is the most logical choice as a default distribution for the experimental data. Nevertheless, it should be clear that the assumption of a multivariate Gaussian distribution is maintained only for the inference of spatial covariance parameters and not necessarily for other operations such as spatial interpolation, simulation or estimation of spatial distributions. Various results from simulations are presented to support the claim that the simultaneous use of maximum likelihood method and the classical nonparametric method of moments can considerably improve results in the estimation of geostatistical parameters.     

含盐土水理参数的试验研究

By the indoor experiment research the hydraulic parameters of the saline soil (soil-water potential and coefficient of permeability), find the some characters of the soil- water potential of saline soil: for the same saline soil at the same dry bulk density, whenever salt solution in soil, at the same liquor content the absolute value of the soil-water potential is always bigger than the saltless soil. And at the same liquor content the absolute value of the soil-water potential increases with increasing the concentration of the salt liquor. And at the same concentration of the salt liquor and at the same liquor content, the absolute value of the soil-water potential of sulphate salt liquor soil is bigger than chloride salt liquor soil. Moreover, the absolute value of the soil-water potential of calcium chloride liquor is bigger than sodium chloride liquor. The disciplinarian of the coefficient of permeability to the saline soil is that whenever saline soil the coefficient of permeability decreases with increasing the salt content and the fine soil change more obviously than coarse-grained soil and the sulphate salt soil change more obviously than sodium chloride salt soil.     

利用抽水试验资料确定水文地质参数

本文根据抽水试验取得的数据,分别采用稳定流公式法、降深-距离配线法、漏斗疏干法和直线解析法四种方法,计算了黄河侧渗补给浅层地下水的各项水文地质参数,最后对试验成果的合理性进行了分析评价并确定了各项水文地质参数.     

城市暴雨径流模拟的参数不确定性研究

基于暴雨管理模型(SWMM),构建了澳门半岛雅廉访实验小区降雨径流模拟系统,采用generalized likelihood uncertainty estimation(GLUE)方法对复杂降雨径流模型参数的不确定性进行了分析,采用均匀分布为参数的先验分布(prior distribution),选取拉丁超立方法作为采样方法,Nash-Sutcliffe效率系数作为似然评判准则。结果表明该方法可以有效的分析降雨径流模型参数的不确定性,对降雨径流模型参数识别提供了深入分析与理解模型系统的有效途径。