淮南煤田朱集井田岩浆侵入特征研究

在对淮南煤田朱集井田钻孔资料分析的基础上,结合侵入岩化学成分测试、X-射线衍射分析以及薄片显微镜下鉴定等结果,得出研究区侵入岩主要以岩床的形式侵入煤系地层,岩性以闪长岩、花岗岩为主,岩床层数多为单层;受NWW—NW向断裂构造带控制,侵入岩体的分布范围呈现从西向东逐渐扩大,在垂向上,从上部煤层到下部煤层,受岩浆影响的程度有明显加大的态势。由于岩浆侵入煤层,严重破坏了煤层的结构和稳定性,同时,降低了煤的工业利用价值,加大了开采难度。     

煤层冲刷带预测方法评述

介绍了沉积分析法、矿井物探法以及地质统计法三种煤层冲刷带预测方法.实例证明,根据煤矿生产的具体情况,选择一种或综合运用几种方法,能较好地预测冲刷带的位置和范围.     

沁水盆地南部潘庄区块废弃矿井煤层气地球化学特征及成因

为了研究废弃矿井中煤层气成因,以沁水盆地南部潘庄区块废弃矿井为例,抽采废弃矿井中煤层气并进行化学组分和同位素测试,并采集部分废弃矿井水样品测试水中离子浓度、pH值等进行研究。结果表明：潘庄区块废弃矿井中煤层气CH₄体积分数平均值为91.99%,CO₂为1.26%,N₂为6.73%;甲烷碳同位素（δ¹³C₁）值为-31.36‰~-33.53‰,平均-32.25‰,氢同位素（δD）值为-182.76‰~-193.20‰,平均-187.538‰。废弃矿井排采水中阴阳离子主要为Mg²⁺、K⁺、HCO₃^-、Cl^-、Na⁺、SO₄^2-和NO₃^-等,产出水型为Mg-（HCO₃）₂型,表明矿井水受到地表水的强烈影响。废弃矿井中煤层气主要以热成因气为主,少量次生生物气。与附近未开采煤储层相比,研究区废弃矿井中的环境更有利于次生生物气的生成。     

中国南京与美国德克萨斯稻田甲烷排放的比较

Field measurements of methane emission from rice paddies were made in Nanjing, China and in Texas, USA, respectively. Soil temperature at approximately 10 cm depth of the flooded soils was automatically recorded. Aboveground biomass of rice crop was measured approximately every 10 days in Nanjing and every other week in Texas. Seasonal variation of soil temperature in Nanjing was quite wide with a magnitude of 15.3℃ and that in Texas was narrow with a magnitude of 2.9℃. Analysis of methane emission fluxes against soil temperature and rice biomass production demonstrated that the seasonal course of methane emission in Nanjing was mostly attributed to soil temperature changes, while that in Texas was mainly related to rice biomass production. We concluded that under the permanent flooding condition, the seasonal trend of methane emission would be determined by the soil temperature where there was a wide variation of soil temperature, and the seasonal trend would be mainly determined by rice biomass production if there are no additional organic matter inputs and the variation of soil temperature over the rice growing season is small.     

应用纤维素示踪北京市PM2.5天然植被排放来源的研究

大气细粒子(PM_2.5)污染是全球尤其是我国许多城市的重要环境问题。利用示踪物质识别和估算大气颗粒物来源是公认的可靠技术,纤维素可以作为示踪物质表征一次颗粒物的天然植被排放来源。本文针对大气细粒子中纤维素含量低、全程序空白相对较高等难点,优化建立了纤维素酶水解、GOD-苯酚-四氨基安替比林测糖法,在我国首次应用于测定大气PM_2.5中纤维素的含量,估算天然植被排放源的贡献。方法检出限为0.26 μg/m³(纤维素),可以满足大气PM_2.5纤维素测定要求;而且有效地降低了空白,全程序空白值(36.5 μg葡萄糖)低于文献方法空白值(53.8 μg葡萄糖),使之更适合于PM_2.5的测定。使用本方法对2012年5月至6月采集的北京市大气PM_2.5样品进行分析,纤维素检出率为96%,纤维素的平均含量为(0.573±0.17) μg/m³,折合为天然植被排放量占PM_2.5质量浓度的1.37%±0.65%;天然植被排放源对有机碳的平均贡献率为4.4%,最大达到9.2%,反映出天然植被排放是北京市PM_2.5的重要来源之 一。本研究方法为我国城市大气颗粒物(包括总悬浮颗粒物、PM₁₀、PM_2.5等)来源识别提供了新的手段。     

Contrasting water–rock interaction behaviors of antimony and arsenic in contaminated rivers around an antimony mine,Hunan Province,China

Although antimony (Sb) and arsenic (As) exhibit similar geochemical behavior and toxicity in the environment, growing evidence suggests that their water–rock interaction behavior in contaminated rivers is quite different. Twenty-nine river water samples were collected between September and November 2018 from contaminated rivers around an antimony mine in Hunan Province, China. The concentrations of As and Sb were inversely proportional to the water flow distance. The rates and magnitudes of Sb decrease were more prominent than those of As. Silicate mineral dissolution from rocks such as silicified limestone increased the As and Sb concentration of in-mine-district (IMD) water. Dissolution of carbonate minerals, ion exchange, and competitive adsorption were the major water–rock interactions, resulting in rapidly decreasing As and Sb concentration in IMD direct impacted water and IMD indirect impacted water. The behaviors of As and Sb during water–rock interaction were dissimilar for areas dominated by carbonate and silicate minerals.     

Formation of the regular satellites of giant planets in an extended gaseous nebula I: subnebula model and accretion of satellites

We model the subnebulae of Jupiter and Saturn wherein satellite accretion took place. We expect each giant planet subnebula to be composed of an optically thick (given gaseous opacity) inner region inside of the planet’s centrifugal radius (where the specific angular momentum of the collapsing giant planet gaseous envelope achieves centrifugal balance, located at rCJ ∼ 15R_J for Jupiter and rCS ∼ 22R_S for Saturn) and an optically thin, extended outer disk out to a fraction of the planet’s Roche-lobe (R_H), which we choose to be ∼R_H/5 (located at ∼150 R_J near the inner irregular satellites for Jupiter, and ∼200R_S near Phoebe for Saturn). This places Titan and Ganymede in the inner disk, Callisto and Iapetus in the outer disk, and Hyperion in the transition region. The inner disk is the leftover of the gas accreted by the protoplanet. The outer disk may result from the nebula gas flowing into the protoplanet during the time of giant planet gap-opening (or cessation of gas accretion). For the sake of specificity, we use a solar composition “minimum mass” model to constrain the gas densities of the inner and outer disks of Jupiter and Saturn (and also Uranus). Our model has Ganymede at a subnebula temperature of ∼250 K and Titan at ∼100 K. The outer disks of Jupiter and Saturn have constant temperatures of 130 and 90 K, respectively.Our model has Callisto forming in a time scale ∼10⁶ years, Iapetus in 10⁶-10⁷ years, Ganymede in 10³-10⁴ years, and Titan in 10⁴-10⁵ years. Callisto takes much longer to form than Ganymede because it draws materials from the extended, low density portion of the disk; its accretion time scale is set by the inward drift times of satellitesimals with sizes 300-500 km from distances ∼100R_J. This accretion history may be consistent with a partially differentiated Callisto with a ∼300-km clean ice outer shell overlying a mixed ice and rock-metal interior as suggested by Anderson et al. (2001), which may explain the Ganymede-Callisto dichotomy without resorting to fine-tuning poorly known model parameters. It is also possible that particulate matter coupled to the high specific angular momentum gas flowing through the gap after giant planet gap-opening, capture of heliocentric planetesimals by the extended gas disk, or ablation of planetesimals passing through the disk contributes to the solid content of the disk and lengthens the time scale for Callisto’s formation. Furthermore, this model has Hyperion forming just outside Saturn’s centrifugal radius, captured into resonance by proto-Titan in the presence of a strong gas density gradient as proposed by Lee and Peale (2000). While Titan may have taken significantly longer to form than Ganymede, it still formed fast enough that we would expect it to be fully differentiated. In this sense, it is more like Ganymede than like Callisto (Saturn’s analog of Callisto, we expect, is Iapetus). An alternative starved disk model whose satellite accretion time scale for all the regular satellites is set by the feeding of planetesimals or gas from the planet’s Roche-lobe after gap-opening is likely to imply a long accretion time scale for Titan with small quantities of NH₃ present, leading to a partially differentiated (Callisto-like) Titan. The Cassini mission may resolve this issue conclusively. We briefly discuss the retention of elements more volatile than H₂O as well as other issues that may help to test our model.     

用伽玛—伽玛测井的低能组分测定煤灰分的可能

伽玛—伽玛测井中的散射伽玛射线低能部分的强度和地层的原子序数有关,因而能用来对煤层的灰分值作原位测量。对8个矿区164个煤样的计算表明,这种用煤层等效原子序数来确定灰分值的方法对煤的变质程度、水分含量变化不敏感,但对灰的元素组成变化,尤其是Fe     

再论煤中大分子基本结构单元演化的拼叠作用

芳构化作用和环缩合作用的传统煤化作用理论具有一定局限性,煤中基本结构单元拼叠作用是高煤级煤演化的特有机理。拼叠作用显著发生的起点位于镜质组最大反射率Ro,max为6．0％附近,大分子化学键的均裂提供了拼叠作用得以实现的微化学环境条件,其实质是一种“动力化学”过程,与氧接芳碳等有关的大量“均裂”是在短暂的煤化阶段中突然出现的,导致“拼叠作用”的显著发生具有“阶跃式”特征,是造成高煤级煤中期到后期阶段大分子基本结构单元急剧增大的根本原因和主要地球化学机理。     

福建省南安市废弃矿山土地利用适宜性评价

通过对福建省南安市废弃矿山及周边环境进行野外实地调查,以资源环境承载能力和国土空间开发适宜性评价(简称"双评价")成果为基础,根据矿山开发占地类型对废弃矿山土地进行分类。挖损的土地根据"木桶原理"判别出短板因子并建立评价模型,压占的土地根据周边环境以"宜农则农、宜林则林、宜园则园、宜建则建"的原则再利用,分别评价南安市废弃矿山土地农业发展和城镇建设的适宜方向。评价结果表明:南安市宜作为城镇建设的废弃矿山图斑有513处,可利用土地面积14.95 km2;宜作为农业发展的废弃矿山图斑有451处,可利用土地面积15.17 km2,后期可根据政府规划投入使用。