THEMIS-VIS observations of clouds in the martian mesosphere: Altitudes, wind speeds, and decameter-scale morphology

We present measurements of the altitude and eastward velocity component of mesospheric clouds in 35 imaging sequences acquired by the Mars Odyssey (ODY) spacecraft’s Thermal Emission Imaging System visible imaging subsystem (THEMIS-VIS). We measure altitude by using the parallax drift of high-altitude features, and the velocity by exploiting the time delay in the THEMIS-VIS imaging sequence.We observe two distinct classes of mesospheric clouds: equatorial mesospheric clouds observed between 0° and 180° L_s; and northern mid-latitude clouds observed only in twilight in the 200–300° L_s period. The equatorial mesospheric clouds are quite rare in the THEMIS-VIS data set. We have detected them in only five imaging sequences, out of a total of 2048 multi-band equatorial imaging sequences. All five fall between 20° south and 0° latitude, and between 260° and 295° east longitude. The mid-latitude mesospheric clouds are apparently much more common; for these we find 30 examples out of 210 northern winter mid-latitude twilight imaging sequences. The observed mid-latitude clouds are found, with only one exception, in the Acidalia region, but this is quite likely an artifact of the pattern of THEMIS-VIS image targeting. Comparing our THEMIS-VIS images with daily global maps generated from Mars Orbiter Camera Wide Angle (MOC-WA) images, we find some evidence that some mid-latitude mesospheric cloud features correspond to cloud features commonly observed by MOC-WA. Comparing the velocity of our mesospheric clouds with a GCM, we find good agreement for the northern mid-latitude class, but also find that the GCM fails to match the strong easterly winds measured for the equatorial clouds.Applying a simple radiative transfer model to some of the equatorial mesospheric clouds, we find good model fits in two different imaging sequences. By using the observed radiance contrast between cloud and cloud-free regions at multiple visible-band wavelengths, these fits simultaneously constrain the optical depths and particles sizes of the clouds. The particle sizes are constrained primarily by the relative contrasts at the available wavelengths, and are found to be quite different in the two imaging sequences: r_eff = 0.1 μm and r_eff = 1.5 μm. The optical depths (constrained by the absolute contrasts) are substantial: 0.22 and 0.5, respectively. These optical depths imply a mass density that greatly exceeds the saturated mass density of water vapor at mesospheric temperatures, and so the aerosol particles are probably composed mainly of CO₂ ice. Our simple radiative transfer model is not applicable to twilight, when the mid-latitude mesospheric clouds were observed, and so we leave the properties of these clouds as a question for further work.     

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.     

基于构造分析的辽宁汤岗子地热系统概念模型研究

通过分析辽东地区深部和浅部构造特点,研究汤岗子地热田的成因,查明地热系统的储、盖、通、源,建立热水系统的概念模型：深部构造是地热发育的重要背景条件,在其影响下的浅部构造体系构成了基岩地区地下裂隙水的运移通道和赋存空间,深循环水在运移途中接受来自深部的热流加热形成热水,并在一定条件下出露地表形成温泉,同一个区域地下水流动系统可以发育多个热储,各个热储之间存在间接的能量和物质联系。     

云南孟连芒信金矿成因探讨

芒信金矿脉状、透镜状、串球状金矿体,赋存于石炭系碳酸盐岩破碎带中。以裂隙金、晶隙金、固溶金、吸附金状存在。经历沉积—变质—岩浆活动等阶段。     

云南昌宁文沧铜矿矿床特征及找矿思路

矿体产于平掌组变质绿片岩中,NW向F3断裂破碎带控矿。边缘向中央品位增高。研究构造延伸和矿源可扩大远景。     

云南武定荒箐铁铜多金属矿矿床成因

矿床产于断层破碎带中,受断层和地层层位控制,与迤纳厂矿床具有一定的相似性。铁矿为中低温热液裂隙充填型脉状矿床,而铜矿床应为沉积——变质型。     

云南巧家仓房沟铅锌矿矿床成矿模式

铅锌矿赋存于灯影组硅质条带白云岩中,局部产于筇竹寺组,脉状、透镜状,与峨眉山玄武岩喷发关系密切,属岩浆晚期热液成因。     

用于盐湖提锂的聚酰胺复合纳滤膜制备及其性能研究

纳滤膜技术以其环境友好、装置集成度高和智能化控制等优势,在卤水锂资源绿色开发领域具有良好的应用前景。实验通过添加聚乙烯醇对纳滤膜功能层进行改性,考察了聚乙烯醇相对含量对纳滤膜性能的影响。结果表明,聚乙烯醇参与界面聚合反应,纳滤膜功能层O/N比增加,聚乙烯醇分子链间氢键作用降低纳滤膜表面粗糙度。羟基官能团的引入有效改善纳滤膜材料亲水效果,膜面羧基密度随聚乙烯醇相对添加量的增加逐渐增加。聚乙烯醇改性纳滤膜截留效果优异,纳滤膜对镁离子的截留率高于95%,锂离子截留率低于-44%,不可逆通量衰减指数低于15%。聚乙烯醇改性纳滤膜材料具有较好的镁锂分离选择效果及抗污染能力,为用于盐湖卤水镁锂分离国产化纳滤膜材料的开发提供新思路。     

从硫酸锂粗矿中分离富集锂的实验研究

针对从西藏查波措盐湖卤水中获得的硫酸锂粗矿,开展从该矿物中分离提取锂的研究。根据该矿物的组成,设计了去除与锂离子共存的镁、硫酸根等主要离子的工艺路线,通过除镁、硫酸根、钙等过程和蒸发浓缩、结晶分离等步骤,得到了杂质离子含量较低的富锂溶液。实验对除镁步骤的加水量、加料方式、反应时间、Ca O加入量等反应关键控制因素进行了考察,确定了较优的分离条件。     

德钦佛山托罗铅锌矿地质特征及成因分析

在对该区野外地质调查的基础上,本文对该铅锌矿化带的成矿构造背景、矿化体特征进行了初步分析与总结,认为该矿受区域构造断裂控制,矿床类型为中低温热液脉状铅锌多金属矿床.该区成矿地质条件优越,矿化体较多,矿体在走向和倾向延伸方向仍可有新突破,并有找到新矿体的可能.