位涡塔结构及演变对飓风Wilma(2005)强度变化的影响

本文利用高分辨率模式输出资料,对飓风Wilma(2005)不同发展阶段内位涡塔(Potential Vorticity Tower:PVT)的结构和演变进行诊断分析,并讨论位涡塔分布特征对飓风快速增强(Rapid Intensification:RI)过程的影响.研究结果表明,内核区域位涡的强度和结构变化主要取决于高层的暖心下传、中层的凝结潜热释放和低层的动力稳定性,而低层切向平均位涡的结构及其稳定性变化,对飓风快速增强的不同发展阶段具有很好的指示意义.飓风Wilma增强过程中,在高层增温、潜热释放和对流垂直混合作用下,PVT的结构出现单极位涡塔(Monopole PVT:MPVT)和中空位涡塔(Hollow PVT:HPVT)的相互转化,也造成了涡旋系统动力稳定性的变化.在实际个例中,重新定义位涡环的结构参数,即相对厚度和中空度,这两个参数能够表征系统的稳定性,将其在RI过程中的变化与飓风Wilma强度变化作相关性分析,表明结构参数能够表征PVT结构的不稳定性,且与飓风系统强度变化参数具有很好的相关性,结构参数与海平面气压变化率的相关性能够通过显著性检验.     

树干水分分布及运移的高密度电阻率成像法时空监测

在砍伐树干周围四个特定高度环形布置一定数量的金属电极,测定了对应横截面上各点视电阻率,再利用有限元反演计算,获得了树干各截面上电阻率的空间分布图像.由于树干内的水分含量和对应部分的导电特性密切相关,可以从得到的电阻率平面分布图上反映出树木内水分含量的空间分布和动态变化特征.结果表明,树干横截面上电阻率的空间分布呈现一系列的同心圆结构,且从核心部到外边缘的韧皮部电阻率有一个减小的趋势,说明截面内树木水分的含量沿径向向外有逐渐递增的趋势.时间变化过程中,各监测截面上的电阻率的分布和变化基本反映了截面水分的流逝过程,表明高密度电阻率成像法动态监测树干水分分布及变化是可行的.     

基态位涡径向分布对浅水涡旋系统演变的影响分析Part Ⅱ:扰动发展和结构变化

本文在基态位涡（Potential Vorticity,PV）径向分布和基态涡旋强度对热带气旋（Tropical Cyclone,TC）类涡旋系统稳定性特征影响的研究基础上,结合理想试验和数值模拟诊断分析基态PV径向分布对扰动增长和系统结构变化的影响.基于线性正压浅水模型,设计三种典型基态PV中空结构下基态涡旋强度对系统稳定性影响的敏感性试验.结果表明：基态涡旋的强度主要影响稳定性的强弱,强度越强,不稳定增长率越大,而基态PV径向分布对系统最不稳定波动性质起着决定作用.分析不同波数下扰动的发展及不同波数间扰动的相互作用可知,对于宽且实的PV环,系统稳定性主要取决于低波数不稳定,且最不稳定波数扰动的发展具有明显的优势地位;对于窄且空的PV环,系统稳定性主要取决于高波数不稳定,且多个高波数下增长最快模态的不稳定增长率值十分接近.利用模态线性叠加法讨论扰动增长对系统结构变化的影响表明：最不稳定波数的扰动发展对系统结构变化有关键影响,而多个波数的扰动不稳定增长相当时,不同波数的扰动发生相互作用从而影响系统结构变化.最后,利用实际个例模拟资料分析基态PV径向分布及其变化对TC结构和强度的影响表明：TC内核区出现的多边形眼墙结构与当前时刻基态PV径向分布所决定的最不稳定波数有很好的对应关系,同时基态PV径向分布变化所反映出的系统动力稳定性强弱与TC强度发展阶段具有很好的相关性.     

地球内核及其边界的结构特征和动力学过程

现代地震学展现出了一个复杂的地球内核内部和表面结构.地球内核内部结构的主要特征表现为其地震波速度和衰减呈现各向异性,且各种结构（速度、衰减和各向异性）均呈现东西半球差异,而内核表面的新发现则包括其局部区域存在起伏的地形和固液并存的糊状层.地球内核压缩波速度和衰减均呈现以地球旋转轴为轴的柱对称各向异性,沿地球旋转轴方向传播的压缩波比沿赤道方向传播的压缩波传播更快且衰减更强烈.同时,内核各向异性结构随深度而变化：内核顶部约100~400 km接近各向同性,而在内核最深处300~600 km内则可能存在一个具有不同各向异性特征的内内核.地球内核的东西半球差异表现在多方面：在内核顶部~100 km厚度内,东半球的各向同性速度比西半球快约0.8%,东半球具有较强的衰减（Q=250）,而西半球则具有较弱的衰减（Q=600）;西半球的顶部各向同性层厚度约为100 km,而东半球顶部各向同性层厚度则约为400 km;在各向同性层底下,西半球具有较强的各向异性（~4%）,而东半球则具有较弱的各向异性（~0.7%）.地球内核边界在菲律宾海、黄海、西太平洋以及中美洲下方存在1~14 km高的地形起伏,在鄂霍次克海西南部下方存在4~8 km厚的糊状层.地球内核的这些新发现引发了对许多可能的新物理机制的探讨,也促使我们重新评估我们对外核成分、外核热化学对流、内核凝固过程和地球磁场驱动力的认识.这些结果表明内核凝固过程和地球磁场的热和化学驱动力远比传统观念认为的横向均匀分布复杂得多.内核西半球可能不断凝固并释放潜热和轻元素,而东半球则可能不断熔化并吸收潜热和轻元素,外核对流的驱动力在东西半球可能截然不同,甚至呈现相反方向.这些凝固与熔化交替过程也发生在局部地形起伏区域.在糊状层区域,地球内核凝固释放潜热和化学能,而在大部分无糊状地区,内核凝固只释放潜热.     

GPS揭示的郯庐断裂带中南段闭锁及滑动亏损

利用华北地区2009—2014年GPS水平运动速度场数据,采用块体负位错模型反演了郯庐断裂带中南段断层深部滑动速率、断层闭锁程度分布、断层滑动亏损速率分布及地震矩积累率,结合地表应变率分布,对郯庐断裂带中南段深、浅部形变、应变特征以及华北地区的地壳形变模式进行了分析.结果表明:郯庐断裂中南段的北端主要为右旋走滑特性,南端则表现为右旋走滑兼拉张性运动,断层滑动速率在0.9mm·a~(-1)至1.2mm·a~(-1),且沿断层走向由北至南逐次增大.断层闭锁程度分布沿走向分布不均一,断层闭锁深度由最北端的27km增加到中段的32km,至最南端变为5km,断层闭锁最深处与1668年郯城MS8.5震中位置相对应.断层滑动亏损速率沿走向由0.9mm·a~(-1)增加到1.2mm·a~(-1),沿倾向由地表至深部逐渐减小为0mm·a~(-1).地震矩积累率在郯庐断裂带中南段郯城附近较大,而地表对应区域为第二应不变分量的低值区.华北地区地壳变形以块体运动为主,块体内部应变及断层闭锁产生的负位错效应次之;郯庐断裂带中南段断层形变沿走向呈条带状分布,形变宽度单侧小于50km,形变量不超过1mm·a~(-1),且上盘形变略大于下盘.     

基于毫米波雷达、无线电掩星和探空仪资料的云边界高度对比研究

为准确评估基于相对湿度廓线法反演云边界高度的有效性,以CloudSat和CALIPSO联合探测结果为基准,对2008年1月至2009年1月COSMIC无线电掩星和探空仪的云底高与云顶高反演结果进行定量对比验证,结果表明:CloudSat、掩星和探空仪检测到高云的比例差异较大,掩星和探空仪云检测效率相近,但云检测质量掩星优于探空仪,云层沿高度的发生概率同样掩星与CloudSat具有更好的一致性;陆地与海洋地区掩星和探空仪云底高反演精度大于云顶高,且反演精度与云层高度有关,二者对不同类型云的边界高度具有不同的反演优势,云底高发生概率掩星和探空仪与CloudSat都有很好的一致性,但云顶高概率掩星与CloudSat的吻合程度更好;CloudSat云边界高度随纬度升高而减小,其与掩星和探空仪的反演偏差同样是低纬大于中高纬,且具有不同的季节分布特点.此外,三者检测的底层云中低云所占比例从冬季到夏季逐渐减小,顶层云中云顶高于10 km的比例从冬季到夏季却逐渐增加.     

黄河源区冻融地质作用及其生态环境地质特征

0引言 黄河源区位于青藏高原腹地的青海省青南高原内部,地处青海省玛多县黄河沿水文站以西,各式各雅山以东,东昆仑山东延中列布青山南麓和南列巴颜喀拉山中段之北地区,面积约20 930km2,海拔均在4 200m以上,属无冰川分布的多年冻土区.     

沙尘暴电效应的实验观测研究

利用国内大型风沙物理风洞实验模拟沙尘暴电现象,研究风沙起电机理,结果表 明,不同风速下不同沙粒会产生不同极性的电场强度和电位效应,风沙电随风速增大而增强 ,且随沙粒度增大而减小. 在沙漠区的16m,8m,4m和1m高度上观测到27次不同沙尘暴天气 过程的电场和风速随时间变化. 结果表明, 在晴天4个高度上的电场均为小正电场值,电场 随高度降低而减小,最大电场强度在5kV/m以下,日风速变化对各层电场起伏没有较大影响 . 有沙尘天气,各高度上的电场强度随风速变化而变化. 16m高度上电场均为负值,平均值 为 -20kV/m;中层8m 电场一般为较高正电场值,达到10～40kV/m,与16m高度上电场呈反相 关;下层1m 电场值变化一般很小,在1kV/m以下. 在强沙尘暴天气4个高度上的电场均为负 电值,电场值随高度降低而减小,16m高度上最大平均电场强度达到-200kV/m以上,瞬时值 超过 -2500kV/m,与晴天电场矢量相反.     

大西洋和西太平洋海域热带气旋海表面入流角和拖曳系数特征对比分析

本文利用大量全球定位下投式探空仪(dropsonde)资料,对15个大西洋飓风和11个西太平洋台风海域的入流角频数分布差异进行对比,探究在热带气旋不同强度和不同边界层平均风速下入流角的分布特征,分析了两个海域拖曳系数随入流角变化的趋势.结果表明,两海域在热带气旋背景下的入流角分布具有共同点:在强度更大的热带气旋里入流角的平均值更大,分布更集中,入流角在不同风速范围内均呈正态分布且差异较小;同时两海域的入流角特征也存在差异,大西洋飓风的平均入流角大于西太平洋台风,并且大西洋飓风的拖曳系数随着入流角增加而增大,而西太平洋台风的拖曳系数随入流角的增加先减小后增大.研究结果为探究热带气旋背景下入流角的作用和影响拖曳系数变化的因子提供了新的参考.     

反应HO2+O→OH+O2对OH夜气辉辐射的贡献

本文探讨了OH Meinel夜气辉辐射的光化学模式,给出OH(ν≤9)分子数密度分布的计算通式,重点研究了化学反应HO2 O→OH(ν≤6) O2对ν≤6各振动能级上OH分子数密度分布以及(ν′—ν″)(ν′≤6)振动带气辉辐射的影响.结果表明,该反应对数密度的贡献随振动能级的减小而增大,对(ν′—ν″)振动带辐射的贡献随着较高振动能级ν′的减小而增大,以春分时为例,它可使第1振动能级上的OH分子最大数密度和(1—0)带的最大辐射率增加约33%,第6振动能级上的最大数密度和(6—ν″)带的最大辐射率增加约7%,(1—0)带的辐射强度增加约30%,(6—ν″)带的强度增加约11%.该反应使各振动能级上分子数密度的高度分布剖面以及各振动带体辐射率的高度分布剖面变宽,最大数密度、最大发射率所处的高度下降1km左右.此外,该反应的影响程度随着原子氧密度的降低而增大,随着温度的升高而增大,并且在夏至时最大,在冬至时最小.     

基于CloudSat资料的北上江淮气旋暴雪云系结构特征

2007年3月3-5日和2013年11月24-25日,受江淮气旋北上影响,我国北方大部地区遭遇罕见暴风雪天气,2次暴雪过程有很多相似之处.利用常规观测、CloudSat卫星云廓线雷达的探测资料和NECP/NCAR再分析资料,分析了这2次暴雪过程江淮气旋云系结构和微物理特征.结果表明：（1）北上江淮气旋的冷锋云系较窄,以深厚对流云为主,回波核心在2~7 km,其结构在气旋发展的不同阶段变化不大;（2）逗点头云系范围宽广,在气旋的不同发展阶段,结构和强度有显著差异.气旋初始锋面波动和锋面断裂阶段,逗点头云系有两个降水区：北部为由多个单体组成的大范围层状云区,强回波从地表向上伸展,上空有高空对流泡,建立了播撒云-供水云机制,有利于下部冰晶粒子长大;南部有对流云柱发展.逗点头西部的冷输送带云系主要集中在6 km以下,强度弱,冰粒子含量少;（3）气旋暖锋后弯阶段,干侵入加强,冷锋后部的无云区或少云区范围扩大,逗点头云系南北范围收缩、变窄,云系的高度、强度和含水量减弱,冷锋云系也减弱;（4）气旋冷锋云系和逗点头南部的对流云柱以降雨为主,位于高纬度陆地上的逗点头云系以降雪为主,当逗点头云系处于海上有对流不稳定发展,以降雨为主.冷锋云系北部和逗点头云系南部均有由层积云或高积云组成的低云,以毛毛雨为主.冷锋云系和逗点头云系北部100-200 km的范围为随高度和距离逐渐变薄的高层云,无降水对应.     

Experimental investigation of the velocity of a sand cloud blowing over a sandy surface

The velocity of a wind‐blown sand cloud is important for studying its kinetic energy, related erosion, and control measures. PDA (particle dynamics analyser) measurement technology is used in a wind tunnel to study the probability distribution of particle velocity, variations with height of the mean velocity and particle turbulence in a sand cloud blowing over a sandy surface. The results suggest that the probability distribution of the particle velocity in a blowing sand cloud is stochastic. The probability distribution of the downwind velocity complies with a Gaussian function, while that of the vertical velocity is greatly complicated by grain impact with the bed and particle–particle collisions in the air. The probability distribution of the vertical velocity of ?ne particles (0·1–0·3 mm sands) can be expressed as a Lorentzian function while that of coarse particles (0·3–0·6 mm sands) cannot be expressed by a simple distribution function. The mean downwind velocity is generally one or two orders greater than the mean vertical velocity, but the particle turbulence in the vertical direction is at least two orders greater than that in the downwind direction. In general, the mean downwind velocity increases with height and free‐stream wind velocity, but decreases with grain size. The variation with height of the mean downwind velocity can be expressed by a power function. The particle turbulence of a blowing sand cloud in the downwind direction decreases with height. The variations with height of the mean velocity and particle turbulence in the vertical direction are very complex. It can be concluded that the velocity of a sand cloud blowing over a sandy surface is mainly in?uenced by wind velocity, grain impact with the bed and particle–particle collisions in the air. Wind velocity is the primary factor in?uencing the downwind velocity of a blowing sand cloud, while the grain impact with the bed and particle–particle collisions in the air are the primary factors responsible for the vertical velocity. Copyright © 2004 John Wiley & Sons, Ltd.     

Statistics on the vertical structure of rainshowers

A large sample of summertime data from the McGill Radar Weather Observatory was analyzed to determine the variation with altitude of the horizontal extent of individual rainshowers. For echoes defined by a reflectivity factor of 39 dBz (equivalent to a rainfall rate of about 10 mm/h) it was found that the mean area of the total population of echoes decreases linearly with altitude from approximately 20 km² at 2 km to 11 km² at 8 km. Subsets of the total population were investigated, consisting of only the echoes penetrating the altitudes of 6, 7, and 8 km. On the average these relatively tall echoes are much greater in horizontal extent than the total population. Whereas the sizes of the total population of echoes at any altitude are distributed approximately exponentially in terms of the square root of area, the sizes of the “survivors” that extend to high altitudes may be described by the gamma distribution with a mean value decreasing approximately linearly with height above 3 km and a dispersion of 0.55. Some characteristics are also reported for echoes defined by reflectivities of 31 dBz and 47 dBz. Estimates are given of the fraction of the total area in a horizontal plane that contains echoes in each of these categories.     

雷暴云准静电场对夜间电离层D区的影响

模型，计算了雷暴云电荷突然对地放电后QE场大小 在0～90km高度上的分布. 对200C的正电荷对地放电后的计算表明，在放电1ms后，在65～78km的区域内，QE场大于大气的雪崩电场，而0.5s后，该电场迅速衰减到很低的水平. 在电 离层高度上，由于电子的热化时标和电离时标极短，在QE场的作用下，夜间局部低电离层会 有比较大的响应. 对Boltzmann方程数值求解的结果表明，在某些高度上，电子分布函数有 明显的高能尾巴；在63～83km的高度上，电子平均能量为3eV＜ε＜6eV；计算的电子数 密度 的峰值扰动表明，在65～78km的高度上，电子的数密度增加，最大的电离峰值约在74km处， 大约增加了3个数量级，比电磁脉冲（EMP）的电离效果大得多.     

Simulating the dispersal of tephra from the 1991 Pinatubo eruption: Implications for the formation of widespread ash layers

PUFF and HAZMAP, two tephra dispersal models developed for volcanic hazard mitigation, are used to simulate the climatic 1991 eruption of Mt. Pinatubo. PUFF simulations indicate that the majority of ash was advected away from the source at the level of the tropopause (~ 17 km). Several eruptive pulses injected ash and SO₂ gas to higher altitudes (~ 25 km), but these pulses represent only a small fraction (~ 1%) of the total erupted material released during the simulation. Comparison with TOMS images of the SO₂ cloud after 71 and 93 h indicate that the SO₂ gas originated at an altitude of ~ 25 km near the source and descended to an altitude of ~ 22 km as the cloud moved across the Indian Ocean. HAZMAP simulations indicate that the Pinatubo tephra fall deposit in the South China Sea was formed by an eruption cloud with the majority of the ash concentrated at a height of 16–18 km. Results of this study demonstrate that the largest concentration of distal ash was transported at a level significantly below the maximum eruption column height (~ 40 km) and at a level below the calculated height of neutral buoyancy (~ 25 km). Simulations showed that distal ash transport was dominated by atmospheric circulation patterns near the regional tropopause. In contrast, the movement of the SO₂ cloud occurred at higher levels, along slightly different trajectories, and may have resulted from gas/particle segregations that took place during intrusion of the Pinatubo umbrella cloud as it moved away from source.     

The initial giant umbrella cloud of the May 18th, 1980, explosive eruption of Mount St. Helens

The initial eruption column of May 18th, 1980 reached nearly 30 km altitude and released 10¹⁷ joules of thermal energy into the atmosphere in only a few minutes. Ascent of the cloud resulted in forced intrusion of a giant umbrella-shaped cloud between altitudes of 10 and 20 km at radial horizontal velocities initially in excess of 50 m/s. The mushroom cloud expanded 15 km upwind, forming a stagnation point where the radial expansion velocity and wind velocity were equal. The cloud was initiated when the pyroclastic blast flow became buoyant. The flow reduced its density as it moved away from the volcano by decompression, by sedimentation, and by mixing with and heating the surrounding air. Observations indicate that much of the flow, covering an area of 600 km², became buoyant within 1.5 minutes and abruptly ascended to form the giant cloud. Calculations are presented for the amount of air that must have been entrained into the flow to make it buoyant. Assuming an initial temperature of 450°C and a magmatic origin for the explosion, these calculations indicate that the flow became buoyant when its temperature was approximately 150°C and the flow consisted of a mixture of 3.25 × 10¹¹ kg of pyroclasts and 5.0 × 10¹¹ kg of air. If sedimentation is considered, these figures reduce to 1.1 × 10¹¹ kg of pyroclasts and 1.0 × 10¹¹ kg of air.     

SOFIE PMC observations during the northern summer of 2007

This work examines the first season of polar mesospheric cloud (PMC) observations from the Solar Occultation for Ice Experiment (SOFIE). SOFIE observations of temperature, water vapor, and PMC frequency, mass density, particle shape, and size distribution are used to characterize the seasonal evolution and altitude dependence of mesospheric ice and the surrounding environment. SOFIE indicates that ice is nearly always present during summer, and that the ice layer is continuous from about 81 km altitude to the mesopause and above. Ice particles are observed to be more aspherical above and below the extinction peak altitude, suggesting a relationship between particle shape and mass density. The smallest particles are observed near the top of the ice layer while the largest particles exist at low concentrations near cloud base. A strong correlation was found between water vapor and particle size with small particles existing when H₂O is low. This relationship holds when examining variability in altitude, and variability over time at one altitude.     

The quasi-biennial oscillation in the equatorial stratosphere: Seasonal regularity in zonal wind changes,discrete QBO-cycle period and prediction of QBO-cycle duration

The changes of vertical wind structure in equatorial stratosphere in course of Quasi-Biennial Oscillation (QBO) demonstrates the evident seasonal dependence. The easterly wind regime descending from the middle to lower stratosphere always includes the stationary period—the stagnation stage. At stagnation stage the bottom boundary of the easterly wind is located in different QBO-cycles at different altitude in the range from ∼22 to ∼26 km, but in each QBO-cycle this altitude is actually constant during the whole stagnation period. Stagnation always begins in solstice (in June–July or December–January). Descent of the easterly wind after stagnation is always resumed near equinox—in March–April or September–October. Consequently, the duration of stagnation stage varies discretely and can be equal to one, three, or five seasons (three, nine, or fifteen months, respectively) in different QBO-cycles. The QBO-cycle period determined as an interval between the beginnings of two successive stagnation stages turns out to be of discrete duration also, and can be equal to 24, 30, or 36 months. The dependence of many atmosphere phenomena determining the Earth’s climate on QBO-phase suggests the need to forecast the QBO-cycle evolution. The established seasonal regularity and discrete QBO-cycle period make it possible the forecasting the QBO-cycle evolution, its duration, and the dates of the QBO-phase changing.     

青海地区一次雷暴的地闪活动及云内的电场探空观测

2016年夏季在青海大通地区获得一次局地雷暴云内的电场探空资料,结合雷达、地闪定位资料,详细分析了该雷暴的地闪活动特征及云内的电荷结构.结果显示,该雷暴过程的负地闪在时间上呈间歇性发生,在空间分布上表现为不连续,且所有的正地闪都发生于雷暴的成熟阶段.在雷暴成熟阶段与消散阶段过渡期获得云内的垂直电场廓线表明,雷暴内的电荷结构在探空阶段呈四极性,最下部为处于暖云区内负电荷区,往上依次改变极性.最上部的正电荷区由于数据丢失无法判断其上边界外,其余3个电荷区的海拔高度分别为:5.5～5.7km(3.4～2.3℃)、5.7～6.2km(2.3～-0.4℃)和6.2～6.6km(-0.9～-1.7℃),对应的电荷密度为-1.81nC·m^-3、2.47nC·m^-3和-1.76nC·m^-3.其中,下部正电荷区的强度最大,其次为上部的负电荷区.通过分析电荷区分布与正地闪活动的关系,认为暖云区内负电荷区的形成有利于诱发下部正电荷区的对地放电.     

Inner-core conductivity in numerical dynamo simulations

Speculation about its possible super-rotation has drawn the attention of many geophysical researchers to the Earth’s inner core. An issue of special interest for geodynamo modelling is the influence of the inner-core conductivity. It has been suggested that the finite magnetic diffusivity of the inner core prevents more frequent reversals of the Earth’s magnetic field. We explore the possible influence of the inner-core conductivity by comparing convection-driven 3D dynamo simulations with insulating or conducting inner cores (CIC) at various parameters. The influence on the field structure in the outer core is only marginal. The time behaviour of dipole-dominated non-reversing dynamos is also little affected. Concerning reversing dynamos, the inner-core conductivity reduces the number of short dipole-polarity intervals with a typical length of a few thousand years. Reversals are always correlated with low dipole strength and these short intervals are found in periods where the dipole moment stays low. Polarity intervals longer than about 10,000 years, where the dipole moment has time recover in strength, are equally likely in insulating and CIC models. Since these latter intervals are of more geophysical relevance, we conclude that the influence of the inner-core conductivity on Earth-like reversal sequences is insignificant for the dynamo model employed here.