减弱对流云降水的AgI催化原理的数值模拟研究

在对流云模式中增加了AgI两个预报量,耦合了考虑受水汽过饱度和温度影响的4种核化机制的AgI催化模块,使其具备了对AgI类催化剂的模拟能力,能够研究AgI类催化剂对对流云系统的影响。利用该模式对一次华南对流云降水过程进行了AgI催化数值模拟试验,对人工减缓对流云降水的可能性及原理进行了研究。模拟结果表明,在适当的时机对适当的部位进行大剂量的催化,可以减少总降水量,也可以减少最大降水中心的雨强。当催化浓度达到2×10~8 kg~(-1)时,可以减少32%的降水量,具备有效减缓对流云降水的可能性。大剂量催化后,大量的AgI粒子在冷区核化后,消耗了大量的过冷水。催化后霰粒子的落速和雨水的落速减小。催化阶段由于霰融化成雨水减少而使降水减弱。催化结束后在霰融化成雨水增多的情况下,雨水的蒸发大幅增加,从而导致了降水量的持续减少。AgI在模拟的强对流云中主要以受过饱和度影响的凝结冻结和催化剂长时间作用的浸没冻结这两种方式成核。研究所用催化方法在外场作业中具有技术可行性。     

BUILDING DENSITY AND INTERIOR BUILDING TEMPERATURES: A PHYSICAL MODELING EXPERIMENT

The effect of building density on the interior temperatures of buildings is explored using scaled physical models. The urban canopy layer is modeled as a single-cube structure surrounded by a wall that represents neighboring structures. Each physical model was constructed of plywood and consisted of a cube 200 mm in height, enclosed by a wall 200 mm in height. Four models were constructed corresponding to height/width ratios (H/W) of 4, 2, 1, and 0.5 and placed at an exposed site located at 34°N. The interior air temperature of each cube, direct and diffuse solar radiation on a horizontal surface, and ambient air temperature and wind velocity were measured over a period from late November 1996 to early June 1997. To extract the influence of building density, air temperatures were compared against those measured in the model representing a H/W of 1. The results show that nighttime cooling is primarily a function of building density, but that daytime heating depends on the interaction of density with changing model-sun relationships. [Key words: urban canopy layer, building air temperature, building density, physical model.]     

Dynamics of convective dissolution from a migrating current of carbon dioxide

During geologic storage of carbon dioxide (CO₂), trapping of the buoyant CO₂ after injection is essential in order to minimize the risk of leakage into shallower formations through a fracture or abandoned well. Models for the subsurface behavior of the CO₂ are useful for the design, implementation, and long-term monitoring of injection sites, but traditional reservoir-simulation tools are currently unable to resolve the impact of small-scale trapping processes on fluid flow at the scale of a geologic basin. Here, we study the impact of solubility trapping from convective dissolution on the up-dip migration of a buoyant gravity current in a sloping aquifer. To do so, we conduct high-resolution numerical simulations of the gravity current that forms from a pair of miscible analogue fluids. Our simulations fully resolve the dense, sinking fingers that drive the convective dissolution process. We analyze the dynamics of the dissolution flux along the moving CO₂–brine interface, including its decay as dissolved buoyant fluid accumulates beneath the buoyant current. We show that the dynamics of the dissolution flux and the macroscopic features of the migrating current can be captured with an upscaled sharp-interface model.     

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Beach erosion and recovery during consecutive storms at a steep‐sloping,meso‐tidal beach

This study analyses beach morphological change during six consecutive storms acting on the meso‐tidal Faro Beach (south Portugal) between 15 December 2009 and 7 January 2010. Morphological change of the sub‐aerial beach profile was monitored through frequent topographic surveys across 11 transects. Measurements of the surf/swash zone dimensions, nearshore bar dynamics, and wave run‐up were extracted from time averaged and timestack coastal images, and wave and tidal data were obtained from offshore stations. All the information combined suggests that during consecutive storm events, the antecedent morphological state can initially be the dominant controlling factor of beach response; while the hydrodynamic forcing, and especially the tide and surge levels, become more important during the later stages of a storm period. The dataset also reveals the dynamic nature of steep‐sloping beaches, since sub‐aerial beach volume reductions up to 30 m³/m were followed by intertidal area recovery (–2 < z < 3 m) with rates reaching ~10 m³/m. However, the observed cumulative dune erosion and profile pivoting imply that storms, even of regular intensity, can have a dramatic impact when they occur in groups. Nearshore bars seemed to respond to temporal scales more related to storm sequences than to individual events. The formation of a prominent crescentic offshore bar at ~200 m from the shoreline appeared to reverse the previous offshore migration trend of the inner bar, which was gradually shifted close to the seaward swash zone boundary. The partially understood nearshore bar processes appeared to be critical for storm wave attenuation in the surf zone; and were considered mainly responsible for the poor interpretation of the observed beach behaviour on the grounds of standard, non‐dimensional, morphological parameters. Copyright © 2011 John Wiley & Sons, Ltd.     

强磁暴的时间分布特性

对比分析1957--2008年间Dst≤-100nT的强磁暴数与太阳黑子数的变化趋势,发现太阳黑子数和Dst≤-100nT的强磁暴数的变化趋势有很好的一致性。进一步统计强磁暴在太阳周不同阶段的分布后发现,同一太阳周内60％以上的强磁暴出现在下降年,但从太阳周各个阶段的平均磁暴年发生率来看,强磁暴平均年发生率最高的年份仍然是太阳活动极大年。     

Effect of charging of aerosols in the lower atmosphere of Mars during the dust storm of 2001

Aerosols are very important in the Martian climate system. Aerosols get charged by the attachment of ions in the atmosphere. Charging of aerosols reduces the conductivity of the atmosphere as the very mobile ions are lost during the ion-aerosol attachment. During a dust storm the dust opacity increases and more ion-aerosol attachment process occurs and consequently conductivity reduces further. It was found that with the background aerosols (dust opacity ∼0.2), the conductivity close to the surface of Mars was reduced by a factor of 5, but during the dust storm (opacity ∼5) of 2001 the conductivity decreased by about 2 orders of magnitude.     

Statistical relationship between solar wind conditions and geomagnetic storms in 1998-2008

Applying ACE data and pressure-corrected Dst index (Dst*), annual distributions of solar wind structures detected at L1 point (the first Lagrangian point between solar-terrestrial interval) and correlations between solar wind structures and geomagnetic storms in 1998-2008 have been studied. It was found that, within the Earth's upstream solar wind, the dominant feature was interplanetary coronal mass ejections (ICMEs), primarily magnetic clouds, during solar maximum period but corotating interaction regions (CIRs) at solar minimum. During rising and declining phases, solar wind features became unstable for the complicated solar corona transition processes between the maximum and minimum phases, and there was a high CIR occurrence rate in 2003, the early period of the declining phase, for the Earth's upstream solar wind was dominated by high-speed southern coronal-hole outflows at that time. The occurrence rate of sector boundary crossing (SBC) events was evidently higher at the late half of declining phase and minimum period. ICMEs mainly centered on the maximum period but CIRs on all the declining phase. The occurrence rate of ICMEs was 1.3 times of that of CIRs, and more than half of ICMEs were magnetic clouds (MCs). Half of magnetic clouds could drive interplanetary shock and played a crucial role for geomagnetic storms generation, especially intense storms (Dst*≤100 nT), in which 45% were jointly induced by sheath region and driving MC structure. Sixty percent of intense storms were totally induced by shock-driving MCs; moreover, 74% of intense storms were driven by magnetic clouds, 81% of them driven by ICMEs. Shock-driving MC was the most geoeffective interplanetary source for four fifths of it able to lead to storms and more than one-third to intense storms. The rest of intense storms (19%) were induced just by 3% of all detected CIRs, and most of CIRs (53%) were corresponding to nearly 40% moderate and small storms (−100 nT<Dst*≤−30 nT). The true sector boundary crossing (SBC) events actually had no obvious geoeffectiveness, just 6% of them corresponding to small storms.     

Non-radial solar wind flows and IMF Bz during 1973-2003

The characteristics of latitudinal angles of solar wind flow (θ_v) observed near earth have been studied during the period 1973-2003. The average magnitude of θ_v shows distinct enhancements during the declining and maximum phases of the sunspot cycles. A close association of B_z component of IMF in the GSE system and the orientation of meridional flows in the solar wind is found which depends on the IMF sector polarity. This effect has been studied in typical geomagnetic storm periods. The occurrence of non-radial flows is also found to exhibit heliolatitudinal dependence during the years 1975 and 1985 as a characteristic feature of non-radial solar wind expansion from polar coronal holes.     

干侵入对济南“7. 18”暴雨的作用

利用NCEP/NCAR再分析资料对2007年7月18日发生在济南地区的短时大暴雨过程进行了详细的分析, 发现这次强降水过程是在高空槽和低空风切变的有利形势下产生的。济南附近最大干空气侵入出现在暴雨发生前1～2天, 干空气侵入有利于深厚干层的形成和维持, 而深厚干层的存在则有利于对流有效位能在中高层的产生、 积聚和释放, 从而导致强的对流上升运动, 为暴雨的产生提供了条件。济南以北地区干空气侵入现象在暴雨过程中一直存在, 主要有两种表现形式: 对流层顶附近向下的干空气侵入和对流层低层由北向南的干空气侵入。济南外的干侵入一方面有利于低层产生辐合、 高层产生辐散, 导致上升运动的发展, 另外一方面还对锋区的形成和移动具有重要作用。上述两方面表明干侵入在这次暴雨过程中起到了至关重要的作用。