Changes of cloud microphysical properties during the transition from supercooled to mixed-phase conditions during CIME

A ground-based seeding experiment using carbon dioxide and propane sprayed from pressurized bottles was carried out under supercooled cloud conditions on a small spatial and short time scale. Water vapor deposition on the artificially generated dry ice and propane ice germs as the main ice formation process (nucleation and growth) is consistent with the experimental results. After nucleation, diffusional growth of the ice particles, partly at the expense of evaporating small droplets, was identified during the mixing of the seeding line with the ambient supercooled cloud. Within the seeding plume, ice water contents up to 80% of the total condensed water are observed, although the size of the formed ice particles did not exceed 25 μm. From the changes of the ice and supercooled liquid phase with time under mixed-phase conditions, liquid water content (LWC) evaporation, ice water content (IWC) formation, and ice crystal growth rates are estimated, which are not affected by the artificial nucleation process. Thus, these rates are assessed to be applicable for a growing ice phase of small ice particles in a young mixed-phase cloud, where other growth mechanisms, like riming or aggregation, are negligible.     

石家庄的云、降水和水汽特征

应用1972~2003年石家庄17个站的云、降水资料分析了各类云的发生频率及其降水特征,结果表明:全年而言,积层混合云出现频率高,且降水概率、降水率较大;夏季积状云出现频率高,降水概率、降水率大,对两者增雨机会多。应用2000~2004年常规天气图,对造成石家庄降水的天气系统、云、降水、水汽进行分析,结果显示:西来槽、冷切变、东蒙冷涡和华北低涡出现频率较高,造成的降水次数多,实施增雨的机会多;气旋类、西南涡出现频率低,但过程雨量大,降水持续时间长,是人工增雨不可忽视的天气系统;冷涡类降水时间最短,降水强度大,对其实施人工增雨,作业时机的把握很重要。石家庄上空的水汽含量呈单峰型季节变化,空中水汽资源量明显地受到大气环流和天气系统影响。对水汽通量场分析表明,对流层中高层水汽多来自于孟加拉湾和南海,低层水汽主要来自于东海、黄海,地面近地层水汽源多为黄渤海。     

利用MODIS可见光和1.38μm通道反演卷云反射率

本文介绍了一种算法,利用TERRA或AQUA卫星平台上的中分辨率成像光谱仪(MODIS)的0.66 μm和1.38 μm通道来反演卷云双向反射率.资料表明,用1.38 μm通道测量的卷云反射率会被卷云上的水汽吸收所削弱.该算法将1.38 μm通道所得的反射率与0.66 μm通道所得的反射率作比较来衡量这种削弱作用的影响,从而获得可见光谱区域较精确的卷云反射率.     

积云对二氧化硫和硫酸盐气溶胶作用的研究

利用一个冰雹云模式与云化学模式耦合而成的二维积云化学模式,研究对流云的输送、微物理转化、云内化学过程、湿清除对SO2及硫酸盐气溶胶的作用。云化学模式的结果表明,由于SO2在向上输送的过程中可溶解于云水和雨水中,从而阻止了SO2向上部的转移,因此对气相SO2来说,云的输送是一个相当无效的过程,而液相清除起主要作用。硫酸盐气溶胶的收支分析表明,降水清除了1.67 mol的SO2-4,占气溶胶总量的64%,其中液态降水清除了0.72 mol,固态降水清除了0.95 mol,说明了冰相过程在硫沉降中的重要性。     

作物气象灾害危害性的多目标灰色局势决策

计算了１９９１年７月４－９日的梅雨锋强度降水过程的热源Ｑ１和水汽汇Ｑ２，结果表明，存在着两类云系即对流云和层状云对Ｑ１和Ｑ２的结构产生影响。对流加热发生在强降水区上空，而层状云加热发生在对流区周围的弱降水区上空，在对流加热区，大量的潜热释放形成最的热源和水汽汇，热源峰值出现在上部对流层，水汽汇峰值出现在下部对流层，在层状云区，通常０℃层以上为热源和水汽汇，０℃层以下的热汇和水汽源，层状云引起的Ｑ１     

论易门铜矿区叠加钴矿化地质特征

综合研究易门铜矿区钴、铜一钴矿床的矿化围岩及蚀变、矿石与脉石矿物组合、矿体地质特征等，提出易门铜矿区的钴矿化形成于晋宁期或印支－燕山期与隐伏的中－酸性岩体有关的后生叠加岩浆期后热液作用，还指出找矿方向，注意在隆起（背斜）与断裂构造的发育区，硅化、钠化、黑云母－绿泥石化蚀变带及Ｃｕ、Ｃｏ（Ａｕ）、Ａｓ、Ｐｂ、Ｚｎ化探异常的地段，优先找矿评价，扩大钴、铜－钴矿床的远景。     

Rare earth element geochemistry of the Woxi W–Sb–Au deposit, Hunan Province, South China

The Woxi W–Sb–Au deposit in Hunan, South China, is hosted by Proterozoic metasedimentary rocks, a turbiditic sequence of slightly metamorphosed (greenschist facies), gray-green and purplish red graywacke, siltstone, sandy slate, and slate. The mineralization occurs predominantly (> 70%) as stratabound/stratiform ore layers and subordinately as stringer stockworks. The former consists of rhythmically interbedded, banded to finely laminated stibnite, scheelite, quartz, pyrite and silty clays, whereas the latter occurs immediately beneath the stratabound ore layers and is characterized by numerous quartz + pyrite + gold + scheelite stringer veins or veinlets that are typically either subparallel or subvertical to the overlying stratabound ore layers. The deposit has been the subject of continued debate in regard to its genesis. Rare earth element geochemistry is used here to support a sedimentary exhalative (sedex) origin for the Woxi deposit. The REE signatures of the metasedimentary rocks and associated ores from the Woxi W–Sb–Au deposit remained unchanged during post-depositional processes and were mainly controlled by their provenance. The original ore-forming hydrothermal fluids, as demonstrated by fluid inclusions in quartz from the banded ores, are characterized by variable total REE concentrations (3.5 to 136 ppm), marked LREE enrichment (La_N/Yb_N = 28–248, ∑LREE/∑HREE = 16 to 34) and no significant Eu-anomalies (Eu/Eu = 0.83 to 1.18). They were most probably derived from evolved seawater that circulated in the clastic sediment pile and subsequently erupted on the seafloor. The bulk banded ores are enriched in HREE (La_N/Yb_N = 4.6–11.4, ∑LREE/∑HREE = 3 to 14) and slightly depleted in Eu (Eu/Eu = 0.63 to 1.14) relative to their parent fluids. This is interpreted as indicating the influence of seawater rather than a crystallographic control on REE content of the ores. Within a single ore layer, the degree of HREE enrichment tends to increase upward while the total REE concentrations decrease, reflecting greater influence and dilution of seawater. There is a broad similarity in chondrite-normalized REE patterns and the amount of REE fractionation of the banded ores in this study and exhalites from other sedex-type polymetallic ore deposits, suggesting a similar genesis for these deposits. This conclusion is in agreement with geologic evidence supporting a syngenetic (sedex) model for the Woxi deposit.     

The Vertical Transport of Air Pollutants by Convective Clouds Part Ⅱ：Transport of Soluble Gases and Sensitivity Tests

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Study of star formation in RCW 106 using far-infrared observations

High-resolution far-infrared observations of a large area of the star-forming complex RCW 106 obtained using the TIFR 1-m balloon-borne telescope are presented. Intensity maps have been obtained simultaneously in two bands centred around 150 and 210 μm. Intensity maps have also been obtained in the four IRAS bands using HIRES-processed IRAS data. From the 150- and 210-μm maps, reliable maps of dust temperature and optical depth have been generated. The star formation in this complex has occurred in five linear sub-clumps. Using the map at 210 μm, which has a spatial resolution superior to that of IRAS at 100 μm, 23 sources have been identified. The spectral energy distribution (SED) and luminosity of these sources have been determined using the associations with the IRAS maps. The luminosity distribution of these sources has been obtained. Assuming these embedded sources to be zero-age main-sequence stars and using the mass–luminosity relation for these, the power-law slope of the initial mass function is found to be −1.73±0.5 . This index for this very young complex is about the same as that for more evolved complexes and clusters. Radiation transfer calculations in spherically symmetric geometry have been undertaken to fit the SEDs of 13 sources with fluxes in both the TIFR and the IRAS bands. From this, the r ⁻² density distribution in the envelopes is ruled out. Finally, a correlation is seen between the luminosity of embedded sources and the computed dust masses of the envelopes.