A Hapke model implementation for compositional analysis of VNIR spectra of Mercury

An implementation of Hapke’s radiative transfer-based photometric model for light scattering in semi-transparent porous media is presented with special emphasis on the analysis of reflectance spectra of Mercury. The model allows intimate mixing of an arbitrary number of regolith components with varying modal abundances, modal chemistries and grain sizes, matured by microphase iron. Reflectance spectra of suites of silicates of varying grain sizes and chemistries are used to calculate the imaginary coefficient of the complex index of refraction as a function of chemistry, thus limiting the modeling effects of chemically atypical laboratory samples, and allowing controlled modeling of minerals with varying chemical compositions. The performance of the model in the visual to near-infrared wavelength range is evaluated for a range of chemically characterized silicate mixtures of terrestrial powders, meteorite powders, matured lunar return samples, and remotely sensed lunar spectra.     

Multi-wavelength simulations of atmospheric radiation from Io with a 3-D spherical-shell backward Monte Carlo radiative transfer model

Conflicting observations regarding the dominance of either sublimation or volcanism as the source of the atmosphere on Io and disparate reports on the extent of its spatial distribution and the absolute column abundance invite the development of detailed computational models capable of improving our understanding of Io’s unique atmospheric structure and origin. Improving upon previous models, Walker et al. (Walker, A.C., Gratiy, S.L., Levin, D.A., Goldstein, D.B., Varghese, P.L., Trafton, L.M., Moore, C.H., Stewart, B. [2009]. Icarus) developed a fully 3-D global rarefied gas dynamics model of Io’s atmosphere including both sublimation and volcanic sources of SO₂ gas. The fidelity of the model is tested by simulating remote observations at selected wavelength bands and comparing them to the corresponding astronomical observations of Io’s atmosphere. The simulations are performed with a new 3-D spherical-shell radiative transfer code utilizing a backward Monte Carlo method. We present: (1) simulations of the mid-infrared disk-integrated spectra of Io’s sunlit hemisphere at 19 μm, obtained with TEXES during 2001-2004; (2) simulations of disk-resolved images at Lyman-α obtained with the Hubble Space Telescope (HST), Space Telescope Imaging Spectrograph (STIS) during 1997-2001; and (3) disk-integrated simulations of emission line profiles in the millimeter wavelength range obtained with the IRAM-30 m telescope in October-November 1999. We found that the atmospheric model generally reproduces the longitudinal variation in band depth from the mid-infrared data; however, the best match is obtained when our simulation results are shifted ∼30° toward lower orbital longitudes. The simulations of Lyman-α images do not reproduce the mid-to-high latitude bright patches seen in the observations, suggesting that the model atmosphere sustains columns that are too high at those latitudes. The simulations of emission line profiles in the millimeter spectral region support the hypothesis that the atmospheric dynamics favorably explains the observed line widths, which are too wide to be formed by thermal Doppler broadening alone.     

HST observations of azimuthal asymmetry in Saturn's rings

From 378 Hubble Space Telescope WFPC2 images obtained between 1996-2004, we have measured the detailed nature of azimuthal brightness variations in Saturn's rings. The extensive geometric coverage, high spatial resolution (), and photometric precision of the UBVRI images have enabled us to determine the dependence of the asymmetry amplitude and longitude of minimum brightness on orbital radius, ring elevation, wavelength, solar phase angle, and solar longitude. We explore a suite of dynamical models of self-gravity wakes for two particle size distributions: a single size and a power law distribution spanning a decade in particle radius. From these N-body simulations, we calculate the resultant wake-driven brightness asymmetry for any given illumination and viewing geometry. The models reproduce many of the observed properties of the asymmetry, including the shape and location of the brightness minimum and the trends with ring elevation and solar longitude. They also account for the “tilt effect” in the A and B rings: the change in mean ring brightness with effective ring opening angle, |Beff|. The predicted asymmetry depends sensitively on dynamical ring particle properties such as the coefficient of restitution and internal mass density, and relatively weakly on photometric parameters such as albedo and scattering phase function. The asymmetry is strongest in the A ring, reaching a maximum amplitude A∼25% near a=128,000 km. Here, the observations are well-matched by an internal particle density near 450 kg m⁻³ and a narrow particle size distribution. The B ring shows significant asymmetry (∼5%) in regions of relatively low optical depth (τ∼0.7). In the middle and outer B ring, where τ?1, the asymmetry is much weaker (∼1%), and in the C ring, A<0.5%. The asymmetry diminishes near opposition and at shorter wavelengths, where the albedo of the ring particles is lower and multiple-scattering effects are diminished. The asymmetry amplitude varies strongly with ring elevation angle, reaching a peak near |Beff|=10° in the A ring and at |Beff|=15-20° in the B ring. These trends provide an estimate of the thickness of the self-gravity wakes responsible for the asymmetry. Local radial variations in the amplitude of the asymmetry within both the A and B rings are probably caused by regional differences in the particle size distribution.     

The stellar mass spectrum of the open cluster NGC 3293

We have obtained and analyzed UBVRI CCD frames of the young, 4–10 Myr, open cluster NGC 3293 and the surrounding field in order to study its stellar content and determine the cluster’s IMF. We found significantly fewer lower mass stars, M≤2.5M _⊙, than expected. This is particularly so if a single age for the cluster of 4.6 Myr is adopted as derived from fitting evolutionary models to the upper main sequence. Some intermediate-mass stars near the main sequence in the HR diagram imply an age for the cluster of about 10 Myr. When compared with the Scalo (The stellar initial mass function. ASP conference series, vol. 24, p. 201, 1998) IMF scaled to the cluster IMF in the intermediate mass range, 2.5≤M/M _⊙≤8.0 where there is good agreement, the high mass stars have a distinctly flatter IMF, indicating an over abundance of these stars, and there is a sharp turnover in the distribution at lower masses. The radial density distribution of cluster stars in the massive and intermediate mass regimes indicate that these stars are more concentrated to the cluster core whereas the lower-mass stars show little concentration. We suggest that this is evidence supporting the formation of massive stars through accretion and/or coagulation processes in denser cluster cores at the expense of the lower mass proto-stars. R.W. Slawson and E.P. Horch are guest investigators at the University of Toronto Southern Observatory, Las Campanas, Chile.     

输变电设施电磁辐射环境影响评价方法探讨

结合输变电设施周围电磁环境特点,对其电磁辐射环境影响评价方法进行探讨,提出相应的电磁辐射污染防治措施与建议,消除公众疑虑。在此基础上,总结当前电磁辐射环评工作中存在的问题,以期为后续同类问题深入研究提供思路。     

黄河黑山峡大柳树坝坝址岩体渗漏量及灌浆量数值模拟研究

大坝坝址岩体的渗漏研究对于大坝的安全运营至关重要。在进行渗漏治理的措施中,灌浆是常见的一种,但目前确定灌浆的各项参数,如配合比,孔距等,需通过灌浆试验花费大量的人财物力及时间才能确定。为快速查清每一种灌浆方案所灌浆量,本文针对模拟坝址水库渗漏灌浆效果的三维数值模拟开展了计算研究。在对大柳树坝坝址岩体地质情况及渗漏情况分析的基础上,将蓄水前的地下水运移规律模拟出,与实际通过钻孔平硐资料及分析得出的实际地下水运移规律做比较,验证对地下水运移规律的假设;然后将蓄水后的地下水运移规律模拟出,确定地下水的运移规律,了解地下水运移的方向,验证与根据实际情况初步判断的地下水运移方向是否吻合;最后通过数值模拟确定在一定灌浆浆液配合比的情况下所需灌浆量与实际的灌浆试验结果做比较。得出结果与实际灌浆试验结果吻合,证明通过数值模拟,建立浆液配合比与灌浆效果之间的关系,在类似情况快速地选取配合比是可行的。     

Numerical analysis on post-grouted drilled shafts: A case study at the Brazo River Bridge,TX

This paper investigates the effects of post-grouting on the behavior of drilled shafts using a case study carried out at the Brazo River, Texas. Commercial finite element software, PLAXIS, was used to quantify the improvement of the tip resistance and side shear resistance of post-grouted drilled shafts (PGDS). The input material parameters of PLAXIS were initially estimated using CPT sounding results, and then the parameters were updated by calibrating the numerical results against full-scale STATNAMIC load test results. Based on the numerical analysis, the authors concluded that (1) the increase in total resistance of PGDS resulted from soil improvement at the shaft tip, (2) the apparent increase in side shear resistance resulted from side shear reversal that occurred during post-grouting, and (3) the apparent increase in the tip resistance of PGDS may be caused by stress relief of the grout. In addition, two approaches to estimate the resistance of PGDS were compared against numerical results. In this case study, the Axial Capacity Multiplier (ACM) approach over-predicted the total resistance whereas the Tip Capacity Multiplier (TCM) approach reasonably predicted the increase in total resistance.     

冈底斯东段泽当大型钨铜钼矿新发现及走滑型陆缘成矿新认识

冈底斯成矿带以斑岩型铜矿(伴生钼矿)为主体,通常作为"挤压型"陆缘岩浆弧—"碰撞裂谷带"斑岩成矿的典型代表而被广泛关注,但层矽卡岩型钨铜钼矿和斑岩型独立钼矿的勘查和研究却未能引起足够的重视,尤其是层矽卡岩型白钨矿的发现,填补了区带矿种的空白;在雅鲁藏布江缝合带边部发现的隐伏斑岩型钼矿,突破了"挤压型"陆缘成矿认识的传统误区。中国冶金地质总局新近发现的冈底斯东段则当钨铜钼矿,既是一处大型钨铜钼矿详查开发基地,又是一组统一于陆缘走滑断裂构造成矿体制作用的钨、铜、钼矿床组合,称为"泽当矿田"。在NWW向雅鲁藏布江缝合带陆缘走滑断裂作用下,早期(68～40.3Ma)拉分型转换构造——NEE向剥离断层,控制了层矽卡岩型钨铜钼矿的形成;在NEE向冲木达陆缘走滑断裂作用下,晚期(30.26～23.62Ma)推闭型转换构造——NWW向逆冲断层,控制了隐伏斑岩型钼矿的形成。层矽卡岩型矿床形成和改造于68～66Ma和57～40.3Ma,叠加富集于斑岩型矿床的形成阶段——30.26～23.62Ma。     

大体积混凝土的施工控制要点

以邢台市七里河大桥为例,基于施工中采取的施工工艺,针对大体积混凝土出现温度裂缝的病害,提出了相应的施工控制要点。