不同地区雷暴电荷结构的模式计算

利用二维时变轴对称模式和实际探空资料 ,模式计算了南昌、兰州和昌都 3个地区雷暴云的电荷结构 ,并对形成机制进行了讨论。结果表明 :兰州地区雷暴的上升气流速度最大 ,雷暴发展最快 ;南昌地区雷暴次之 ;昌都地区雷暴最弱。南昌地区雷暴的持续时间最长。在雷暴的初始阶段 3个地区都存在雷暴下部次正电荷区 ,在雷暴的成熟阶段兰州地区在感应和非感应起电机制的共同作用下雷暴呈明显的 3极性电荷结构 ,南昌地区的雷暴主要在感应起电机制作用下形成偶极性电荷结构 ,而昌都地区的雷暴在非感应起电机制作用下形成偶极性电荷结构。 3个地区的雷暴负电荷区中心基本处于 - 1 0～ - 2 0℃的同一温度区内。中国北方地区的温度层结有利于形成 3极性电荷结构 ,且通过非感应起电机制来完成。     

雷暴非感应起电机制的模拟研究：Ⅰ.云内因子影响

利用一个二维时变积云动力－电数值模式模拟了非感应起电过程，讨论了流场。降水以及冰晶谱分布对起电的影响。结果指出：只有在强上升气流穿过－２０℃高度层时才会产生强起电，且发生达到最大上升速度后出现降落的时段。     

Charging state of atmospheric nanoparticles during the nucleation burst events

In this work, the charging state of atmospheric nanoparticles was estimated through simultaneous measurements of aerosol size distribution and air ions mobility distribution with the aim to elucidate the formation mechanisms of atmospheric aerosols. The measurements were performed as a part of the QUEST 2 campaign at a boreal forest station in Finland. The overlapping part of the measurement ranges of the particle size spectrometers and air ion mobility spectrometers in the mass diameter interval of 2.6–40 nm was used to assess the percentage of charged particles (charging probability). This parameter was obtained as the slope of the linear regression line on the scatterplot of the measured concentrations of total (neutral + charged) and charged particles for the same diameter interval. Charging probabilities as a function of particle diameter were calculated for different days and were compared with the steady state charging probabilities of the particles in the bipolar ion atmosphere. For the smallest particles detectable by the particle size spectrometers (2.6–5 nm), the high percentages of negatively charged particles were found during the nanometer particle concentration bursts. These values considerably exceeded the values for the steady charging state and it was concluded that negative cluster ions preferably act as condensation nuclei. This effect was found to be the highest in the case of comparatively weak nucleation bursts of nanoparticles, when the rate of the homogeneous nucleation and the concentration of freshly nucleated particles were low. The nucleation burst days were classified according to the concentration of the generated smallest detectable new particles (weak and strong bursts). Approximately the same classification was obtained based on the charge asymmetry on particles with respect to the charge sign (polarity). The probabilities of negative and positive charge on the particles with the diameter of 5–20 nm were found to be nearly equal and they approximately agree with the values corresponding to the steady state charge distribution for negative particles known from lab experiments. It means that the steady charging state was reached during the growing time of particles up to 5 nm. The natural charging state of particles with a diameter between 2.5 and 4.5 nm was estimated by means of a special DMPS setup. Results were found to be in good correlation with the data by the particle size spectrometers and air ion mobility spectrometers.     

Charging of oil fields surrounding the Shaleitian uplift from multiple source rock intervals and generative kitchens,Bohai Bay basin,China

This paper discusses origin and charging directions of oil fields on the Shaleitian Uplift, Bohai Bay basin. The Shaleitian Uplift is a footwall uplift surrounded by three sags containing mature source rocks. The origins of the four oil fields on the Shaleitian Uplift, both in terms of source rock intervals and in terms of generative kitchens, were studied using biomarker distributions for 61 source rock samples and 27 oil samples. Hierarchical cluster analysis using 12 parameters known to be effective indicators of organic matter input and/or depositional conditions allowed the identification of six oil types or classes. These six oil classes could then be linked to three distinct source rock intervals ranging in age from 43.0 Ma to 30.3 Ma. The third member (43.0–38.0 Ma in age) and first member (35.8–32.8 Ma) of the Eocene Shahejie Formation, and the third member of the Oligocene Dongying Formation (32.8–30.3 Ma) each sourced one class of oil. The other three classes represent mixtures of oil generated from multiple source rock intervals. Traps on the Shaleitian Uplift were charged in the east by oil generated from the Eocene Shahejie Formation in the Bozhong Sag, in the southeast by oil generated from the Eocene Shahejie and then Oligocene Dongying formations in the southwestern part of the Bozhong Sag and/or in the eastern part of the Shanan Sag, and in the southwest by oil generated from the Eocene Shahejie Formation in the western part of the Shanan Sag. The estimated migration distances range from less than 5 km to about 20 km. The compositional heterogeneity within fields and multiple-parameter comparisons between oils from nearby wells in different fields have proven to be a powerful tool to determine the in-filling histories of oil fields in cases where multiple source rock intervals and multiple generative kitchens exist.     

冰晶核化对雷暴云闪电行为影响的数值模拟研究

为了探讨冰晶核化对雷暴云闪电行为的影响,通过已有的三维对流云起、放电模式探讨对比了3种冰晶核化方案,分别为原模式中的经验公式YS方案及与气溶胶相关的DE方案和LP方案。研究表明冰晶核化方案对雷暴云内冰晶微物理发展特征、起电及放电过程均有一定影响。模拟结果显示:(1)考虑了气溶胶的两种新参数化方案中冰晶粒子在高温区(高于-13.8℃)出现,在雷暴云发展过程中DE方案和LP方案冰晶的垂直分布均大于YS方案。(2)DE方案和LP方案中高温区出现的冰晶所带电荷极性有明显的反转现象,导致雷暴云电荷结构产生差异;雷暴云发展旺盛时刻DE方案和LP方案出现三级性电荷结构,而YS方案在整个雷暴云过程都是偶极性,并且DE方案和LP方案中电荷空间分布区域更加广泛。(3)不同核化方案下雷暴云放电特征存在差异,YS方案在偶极性电荷结构背景下没有负地闪产生,而DE方案和LP方案中次正电荷区的存在促进了负地闪的发生,并且负先导出现在较低的高度范围内;DE方案和LP方案中电荷量级较大,因此云闪发生频次以及正、负先导传播次数增加明显。     

High-altitude charged aerosols in the atmosphere of Titan

Observations by several instruments onboard the Cassini spacecraft revealed the existence of heavy hydrocarbon and nitrile species with masses of several thousand atomic mass units in the ionosphere of Titan. These very large molecules are in fact aerosols. The goal of this paper is to compute the concentrations of the charged aerosols in the upper atmosphere (950-1200 km) of Titan. The charging of these aerosols has been studied using the charge balance equations, where positive ions, negative ions, electrons, neutral and charged aerosols are included. Number concentrations of charged aerosols are compared with those observed by the Cassini instruments. The present work estimates the aerosol mass density as 1-10 kg/m³, which is within the predicted range. The results show that the aerosols must be smaller than 10 nm in order to have reasonable agreement with observations by the Cassini Plasma Spectrometer.