1984—2019年念青唐古拉山中段冰川ELA变化估算及特征分析

平衡线高度（equilibrium line altitude,ELA）是冰川响应气候变化的直接反映,分析其变化特征对于了解现在和过去的气候具有重要意义。念青唐古拉山中段作为西南季风通道以及怒江与雅鲁藏布江的分水岭,ELA变化及特征研究可为不同流域冰川变化与气候相互关系提供参考。基于遥感影像及气候数据,结合模型计算的冰川ELA数据作为输入参数,建立多元线性回归方程,重建并分析了1984—2019年间念青唐古拉山中段冰川ELA变化。结果表明：研究时段内平均ELA为5 360 m a.s.l.,总体呈上升趋势,上升速率为1.57 m?a^-1。ELA年变化量显示出波动变化特征,波动范围为5 360~5 420 m a.s.l.,上升幅度为60 m。受印度季风、流域位置及冰川朝向等因素影响,各流域ELA变化具有差异性,霞曲流域、易贡藏布流域和麦曲流域多年平均ELA高程分别为5 335 m a.s.l.、4 987 m a.s.l.和5 317 m a.s.l.,平均上升幅度分别为265 m、314 m和335 m,上升速率分别7.57 m?a^-1、8.97 m?a^-1和9.57 m?a^-1。对冰川区多年ELA变化的气候响应分析显示,ELA变化主要受气温控制,随气温变化1 ℃,冰川ELA总体波动幅度为126.02 m。     

基于MapGIS与Oracle的地质数据库建立

与普通的数据相比,地质数据有着多源、多量、多类、多元、多维、多主题等特点。由于地质数据自身的特点,如何有效地存储管理海量地质成果资料和相关信息要素,已经成为当前的热门研究课题。以矿产资源潜力评价数据为例,在Oracle 10G、MapGIS K9平台基础上完成全国矿产资源潜力评价数据的数据库建设工作。在原有软件的基础上,对海量地质数据进行统一管理,为地质数据的应用提供基础保障,从而提高地质数据的信息化服务能力。     

FY-2G卫星冬夏云量产品偏差分析

开展卫星反演云量的精度评估是业务应用的基础,也是充分发挥卫星观测效益的前提。利用同类卫星产品EOS Aqua/MODIS云产品,选取2015年6月和12月共80个个例,包括43个白天个例,37个夜间个例。采用交叉比对方法对FY-2G云量产品进行相对偏差分析。结果表明:FY-2G与Aqua/MODIS计算云量总体趋势相当,无论从时间分布（白天和夜间）还是季节分布（6月和12月）上看,FY-2G与Aqua云量相对偏差较为稳定,FY-2G反演云量小于Aqua/MODIS反演云量。匹配个例中FY-2G平均云量为72.81%,Aqua/MODIS平均云量是76.19%,两者相关系数为0.74。两者绝对偏差小于5%的像元比例为72.34%;云量偏差绝对值小于15%的像元比例为79.51%。FY-2G与Aqua/MODIS云量偏差主要来自各自卫星的观测能力与所采用的云检测算法。与具有36个探测通道、星下点最低空间分辨率为0.01°×0.01°的Aqua/MODIS观测数据相比,FY-2G所具有的5通道、星下点最高空间分辨率为0.05°×0.05°的观测数据会出现对云,尤其是破碎云和薄卷云的漏检。两种具有不同时空属性的数据在匹配处理时采用的不同算法也会在比对分析中引入偏差。     

光照和温度对细基江蓠繁枝变型的生长及生化组成影响

实验研究光照、温度对细基江蓠的生长率及生化组成等指标的影响。结果表明 ,光照、温度及其相互作用均显著影响以上指标。在该实验条件下 ( 15～ 30℃ ,12 0 0～ 12 0 0 0 lx) ,细基江蓠繁枝变型 ( Gracilaria tenuistipitata var.liui)在光照为 10 0 0 0 lx,温度为 2 5℃时生长率最大 ,光照对生长的影响大于温度 ,而且在适宜的温度范围内 ,随着温度的升高 ,细基江蓠繁枝变型生长的光饱和点也增高。光强是影响藻红素、叶绿素 a及碳水化合物 /蛋白质比率的主要环境因子 ,它与藻红素、叶绿素 a含量负相关 ,与碳水化合物 /蛋白质比率正相关。温度则是调节蛋白质及藻红素 /叶绿素 a比率的主要因素 ,它与蛋白质的含量负相关 ,与藻红素 /叶绿素 a比值正相关。温度和光照对碳水化合物的含量影响不明显     

金橙G螯合形成树脂分离富集地质样品中微量贵金属研究Ⅱ——铑的分离富集测定

主要报道了用金橙Ｇ螯合负载形成树脂分离富集地质样品中贵金属Ｒｈ的方法。在最佳试验条件下Ｒｈ的回收率可达９５％～１０５％之间；其相对标准偏差为４．４９％；百分相对误差较小，为－２．４％；方法无系统误差；用硫脲洗脱，该负载形成树脂不被破坏，重复使用５次，树脂均未见异常，均能定量回收，回收率在９８．５％～１０４％之间，符合要求。说明，这种负载形成树脂也较稳定，也可用于实际地质样品中微量贵金属的分离富集     

Could the conventionally known Abu Roash “G” reservoir (upper Cenomanian) be a promising active hydrocarbon source in the extreme northwestern part of Egypt? Palynofacies,palaeoenvironmental, and organic geochemical answers

In different areas of the Western Desert of Egypt, the Abu Roash “G” Member exhibits either a reservoir or source affinity. Thus, thirteen cutting samples covering the Abu Roash “G” Member were selected from the Nest-1A well at Matruh Basin to investigate its hydrocarbon source potential. Palynological age dating of the section that is calibrated with foraminifera and ostracodes enabled a proper identification of the “G” Member. Detailed analysis of the vertical distribution of particulate organic matter of this member shows two palynofacies types. PF-1 reflects an outer middle shelf depositional environment of prevailed reducing (suboxic-anoxic) conditions for the organic-rich shales of the lower “G” Member (samples 1–8). While, PF-2 reflects a minor regression that resulted in deposition of another organic-rich shales of the upper “G” Member (samples 9–13) in an inner middle shelf setting under the same prevailing reducing (suboxic-anoxic) conditions.Organic geochemical analysis reveals good to very good potential of the “G” Member as a hydrocarbon source rock (1.8–2.41, avg. 2.15 total organic content wt %). It also shows good to very good petroleum potential (PP: 4.8–11 , avg. 8 mg HC/g rock). Pyrolsis and palynofacies analyses show kerogen type II for the lower “G” Member (samples 1–8), which is characterized by high Hydrogen index (HI: 396 and 329 mg HC/g TOC at depths 1500 and 1560 m) and very high dominance of oil-prone material (amorphous organic matter “AOM”, marine palynomorphs, and sporomorphs) and very rare occurrence of gas-prone material (brown phytoclasts). The upper “G” Member (samples 9–13) shows kerogen type II-III, which is characterized by a lower HI value of 213 mg HC/g TOC at depth 1340 m and it contains fewer amounts of gas-prone material and relatively lower AOM and marine palynomorphs in comparison to the upper “G” Member. Maturation parameters T_max (430–433 °C), production index (PI: 0.1 mg HC/g rock), and thermal alteration index (TAI: 2+) indicate the lower “G” Member has already entered the early oil-window kitchen, and it is expected to produce oil. The upper “G” Member is expected to produce only oil with no gas shows, because it is marginally mature (T_max 426 °C, PI 0.2, TAI 2). The source potential index (SPI: 5.3 t HC/m²) of the “G” Member shows it as currently generating moderate quantities of oil in the area of Nest-1A well.Consequently, the organic-rich shales of the “G” Member are suggested here as a promising, active oil source rock in that extreme northwestern part of the Western Desert of Egypt. However, for commercial oil recovery from the Abu Roash “G” Member, it is highly recommended to explore the depocentre of Matruh Basin at about 150 km east the Nest-1A well.     

弱碱性阴离子树脂分离富集-发射光谱法测定痕量钯

在盐酸介质中，钯与氯离子发生反应生成配合物[PdCl6]^2-，该配合物能被大孔弱碱性苯乙烯系阴离子交换树脂吸附。吸附物灰化后，灰分与缓冲剂混合均匀，全部装入杯形电极，发射光谱法测定钯。方法检出限为0．12ng／g（10．0g样品）。方法经国家一级标准物质验证，测定值与标准值相符，精密度（RSD，n=12）为8．9％～13．9％，回收率为89％～118％。方法已用于测定水系沉积物中的痕量钯。     

新型锥体连接复合钎头暨G308,YJ2.1R凿岩合金

对传统刃片状和球齿钎头实现了扬长避短的“飞龙”φ42-4P1C锥体连接复合钎头，配合使用强度和耐磨性均佳的新型G308，YJ2．1R凿岩硬质合金，其使用寿命为我国目前广泛流行的锒YG11C合金片的φ40，φ42一字形钎头的3倍以上，是具有显著高效，低耗特点的换代产品。     

Gas infall in the massive star formation core G192.16–3.84

Previous observations have revealed an accretion disk and outflow motion in the high-mass starforming region G192.16–3.84, but collapse has not been reported before. Here we present molecular line and continuum observations toward the massive core G192.16–3.84 with the Submillimeter Array. C18 O(2–1) and HCO+(3–2) lines show pronounced blue profiles, indicating gas infalling in this region. This is the first time that infall motion has been reported in the G192.16–3.84 core. Two-layer model fitting gives infall velocities of 2.0±0.2 and 2.8±0.1 km s-1. Assuming that the cloud core follows a power-law density profile(ρ∝ r1.5), the corresponding mass infall rates are(4.7±1.7)×10-3 and(6.6±2.1)×10-3 M⊙yr-1 for C18 O(2–1) and HCO+(3–2), respectively. The derived infall rates are in agreement with the turbulent core model and those in other high-mass star-forming regions, suggesting that high accretion rate is a general requirement for forming a massive star.