Infrared photometry of Sakurai’s object (V4334 Sgr) in 1996–1999

The infrared photometric observations of V4334 Sgr in 1996–1999 are presented. Together with optical data, they have allowed us to accurately estimate the bolometric flux from this star and to investigate the structure of its dust envelope over the above period. The star is shown to have passed through four well-defined stages in these four years as it moved backward along the post-AGB track, and it now appears to have started moving forward after a halt. At the first stage (1996), there was no dust in the star’s envelope. Its visual brightness slightly increased, and it reddened in the entire observed spectral range. The bolometric flux also gradually rose. At the second stage (1997), an optically thick dust envelope condensed around the star, which, however, essentially did not manifest itself at optical wavelengths. The bolometric flux continued to rise through an increase in the star’s infrared brightness alone; the rate of its rise also increased. At the third stage (1998–March 1999), V4334 Sgr entered the R CrB phase. First two shallow minima and then two deep minima were observed at optical wavelengths. The star appreciably reddened during the deep minima. The bolometric flux ceased to rise and began to gradually fall in the second half of 1998. At the fourth stage (since March 1999 up until now), V4334 Sgr has been at a protracted deep minimum, which is atypical of the R CrB stars. The bolometric flux between March and October underwent no significant variations. We describe the structure of the dust envelope around V4334 Sgr since its formation. From June 1997 until July 1998, the optical depth of the dust shell, its inner and outer radii, and its mass increased by factors of ～2.2, ～2.0, 2.3, and ～10, respectively. In July 1998, τ(V)≈2.3, R _{d, in}≈7.4×10¹⁴ cm, R _{d, in}/R _{d, out}≈0.7(R _{d, in}/R _*≈47), and M _dust≈1.6×10^?7 M _⊙.     

Analysis of HST ultraviolet spectra for T Tauri stars: RU Lup

The ultraviolet spectra of the star RU Lup obtained with the Hubble Space Telescope are analyzed. Emission lines are identified. The presence of absorption components with a nearly zero residual intensity in the Mg II resonance doublet lines is indicative of mass outflow with a velocity V _∞?300 km s^?1. These lines also exhibit a broad (?1400 km s^?1 at the base) component originating in the star itself. The profiles of the (optically thin) Si II] and Si III]1892 Å lines for the first time unequivocally prove that these lines originate in an accretion shock wave rather than in the chromosphere, with the gas infall velocity being V ₀?400 km s^?1. The intensity ratio of the C IV 1550 Å and Si IV 1400 Å resonance doublet components was found to be close to unity, suggesting a high accreted-gas density, logN ₀>12.5. Molecular H₂ Lyman lines formed in the stellar wind were detected. The H I Lα luminosity of RU Lup was found from their intensities to exceed 10% of L _bol. Radiation pressure in the Lα line on atomic hydrogen may play a significant role in the initial acceleration of stellar-wind matter, but the effect of Lα emission on the dynamics of molecular gas is negligible.     

用滑块模型对冲击地压的研究（I）

根据冲击地压发生的力学条件和地质条件, 引入 (Ruina,1983年)单状态变量本构模型(Single state variable model, SSVM)对冲击地压的动力学行为和演化行为进行了描述。研究表明：模型中参数K, 对冲击地压系统动力学行为和状态变量演化行为贡献较大,而系统动力学行为和演化行为对 ,f初值的敏感性相对较低。模型模拟了冲击地压系统的粘滑特性和冲击地压系统的动力失稳过程,较好地解释了冲击地压的发生机理,为冲击地压失稳破坏的预测预报提供了理论依据。     

The influence of dependence in characterizing multi-variable uncertainty for climate change impact assessments

Few approaches exist that explicitly use the uncertainty associated with the spread of climate model simulations in assessing climate change impacts. An approach that does so is second-order approximation (SOA). This incorporates quantification of uncertainty to ascertain its impact on the derived response using a Taylor series expansion of the model. This study uses SOA in a statistical downscaling model of monthly streamflow, with a focus on the influence of dependence in the uncertainty of multiple atmospheric variables. Uncertainty is quantified using the square root error variance concept with a new extension that allows the inter-dependence terms among the atmospheric variable uncertainty to be specified. Applying the model to selected point locations in Australia, it is noted that the downscaling results differ considerably from downscaling that ignores uncertainty. However, when the effects of dependence in uncertainty are incorporated, the results differ according to the regional variations in dependence structure.     

Size scale of the R Coronae Borealis variables

The radius of R CrB is estimated to 90–100 radii of the Sun. The dust layer, which is the cause of the deep minimum in the visible light of R Coronae Borealis-type stars, has a radius of about 6 radii of the star. This follows from the delay of the infrared light increase after the visual minimum and also from the analogy with the dust formation in novae. The emission lines appearing in the minimum have an origin analogous to the metal emissions in the comets of 1882 II and 1965 VIII in which they were observed at a distance of 20–30 R⊙. The permanent dust shell has a radius about of 26 stellar radii.     

Photometric observations of the central star of the planetary nebula NGC 2346 in 1991/1992

Photoelectric UBV observations of the central star of the planetary nebula NGC 2346 obtained during 60 nights between October 1991 and February 1992 are presented (Tables 1 and 2). Four minima have been stated and can be interpreted in terms of occulting dust clouds, probably representing dense condensations of the planetary nebula. We derived R = A_V/E_B—V = 4.0.     

变密度声波全波形反演中密度影响因素及反演策略

密度信息可预测储层流体饱和度,因此获取可靠的密度参数已成为全波形反演中首要考虑的问题。为了获得更稳定的反演密度,本文从频率、初始速度模型、初始密度模型和密度速度同时反演四个方面对密度的影响进行了研究。根据研究测试结果制定了稳定的反演策略：首先将密度固定,反演速度,此时波动方程中不再含有密度项,因而可以得到准确的速度模型;将其作为初始速度模型进行速度、密度同时反演,可以较好地减小速度对密度的影响。理论模型测试结果充分说明了策略的有效性。     

古滑坡滑带土的力学特性与库水位变化对其稳定性影响及加固措施

与普通滑坡体相比,库岸古滑坡体不仅影响稳定的因素多,且受库水位变化影响明显,极易诱发地质灾害,对人类生命财产安全造成危害。以某水库古滑坡体工程为例,利用现场直剪试验、室内直剪试验及标准贯入试验手段,研究滑带土的力学特性,并对利用得到的参数计算分析水位变化对古滑坡体稳定性影响的规律,得到鹅公带古滑坡体的安全系数随库水位升高成U形的变化规律。采用文献[12]提出的利用应力场判断滑坡体的类型,在高应力水平位置采取加固措施降低应力水平后边坡安全系数就提高的方法,由计算出的应力场判断鹅公带古滑坡具有上部推移下部牵引的特征,属于混合破坏型滑坡,针对其上部和下部坡体进行加固处理。对比分析不同加固方案对滑坡体应力场的改变和比较抗滑桩在不同位置时安全系数与位移场和应力场之间的关系,表明对高应力水平区和位移大的区域进行加固的效果最好,该滑坡体下部也是高应力水平区,由于现场施工条件,考虑经济性,最后采用在滑坡体下部设置反压体加固,加固后3年的实践表明利用边坡应力场的应力水平确定加固位置合理可行。文中的研究方法和思路可为类似工程处理提供一个很好地分析问题和解决问题的思路和同类工程借鉴。     

Axisymmetric dynamic response of the multi-layered transversely isotropic medium

By virtue of the precise integration method (PIM) and the technique of mixed variable formulations, solutions for the dynamic response of the multi-layered transversely isotropic medium subjected to the axisymmetric time-harmonic forces are presented. The planes of cross anisotropy are assumed to be parallel to the horizontal surface of the stratified media. Four kinds of vertically acting axisymmetric loads are prescribed either at the external surface or in the interior of the soil system. Thicknesses and number of the medium strata are not limited. Employing the Hankel integral transform in cylindrical coordinate, the axisymmetric governing equations in terms of displacements of the multi-layered media are uncoupled. Applying mixed variable formulations, more concise first-order ordinary differential matrix equations from the uncoupled motion equations can be obtained. Solutions of the ordinary differential matrix equations in the transformed domain are acquired by utilizing the approach of PIM. Since PIM is highly accurate to solve the sets of first-order ordinary differential equations, any desired accuracy of the solutions can be achieved. All calculations are based on the corresponding algebraic operations and computational efforts can be reduced to a great extent. Comparisons with the existing numerical solutions are made to confirm the accuracy of the present solutions proposed by this procedure. Several examples are illustrated to explore the influences of the type and degree of material anisotropy, the frequency of excitation and loading positions on the dynamic response of the stratified medium.     

Changes in water table level influence solute transport in uniform porous media

Changes in the water table level result in variable water saturation and variable hydrological fluxes at the interface between the unsaturated and saturated zone. This may influence the transport and fate of contaminants in the subsurface. The objective of this study was to examine the impact of a decreasing and an increasing water table on solute transport. We conducted tracer experiments at downward flow conditions in laboratory columns filled with two different uniform porous media under static and transient flow conditions either increasing or decreasing the water table. Tracer breakthrough curves were simulated using a mobile–immobile transport model. The resulting transport parameters were compared to identify dominant transport processes. Changes in the water table level affected dispersivities and mobile water fractions depending on the direction of water table movement and the grain size of the porous media. In fine glass beads, the water flow velocity was similar to the decline rate of the water table, and the mobile water fraction was decreased compared with steady‐state saturated conditions. However, immobile water was negligible. In coarse glass beads, water flow was faster because of fingered flow in the unsaturated part, and the mobile water fraction was smaller than in the fine material. Here, a rising water table led to an even smaller mobile water fraction and increased solute spreading because of diffusive interaction with immobile water. We conclude that changes of the water table need to be considered to correctly simulate transport in the subsurface at the transition of the unsaturated–saturated zone. Copyright © 2014 John Wiley & Sons, Ltd.