北美地区一次冬季中尺度对流系统上空红色精灵现象的空间观测及其母体雷暴分析

红色精灵是发生在雷暴云上空的一种大尺度瞬态放电发光现象,它们通常出现在地面上空40～90 km之间,是由地闪回击和随后可能存在的连续电流产生的。目前,由于综合同步观测资料较少,与夏季红色精灵相比,全世界对冬季红色精灵的研究屈指可数。2008年12月27～28日,受高空槽及低层暖湿气流的影响,北美阿肯色州地区爆发了一次冬季雷暴天气过程,搭载于FORMOSAT-2卫星上的ISUAL（Imager of Sprites and Upper Atmospheric Lightning）探测器有幸在这次雷暴上空记录到了两例红色精灵事件。本文利用ISUAL获取的红色精灵观测资料、多普勒天气雷达资料、美国国家闪电定位资料、超低频磁场数据、美国国家环境中心/气候预测中心提供的云顶亮温和探空数据等综合观测数据,对产生红色精灵的这次冬季雷暴特征和相关闪电活动规律进行了详细研究。结果表明,在两例红色精灵中,ISUAL均未观测到伴随的“光晕（halo）”现象,第一例为“圆柱状”红色精灵,第二例红色精灵由于发光较暗,无法判断其具体形态。产生红色精灵的母体雷暴是一次中尺度对流系统,该系统于27日15:00（协调世界时,下同）左右出现在阿肯色州北部附近,并自西向东移动。23:59系统发展到最强,最大雷达反射率因子（55～60 dBZ）的面积达到339 km2,之后开始减弱。03:03雷暴强度有所增加,随后云体便逐渐扩散,雷暴开始减弱,并在11:00完全消散。两例红色精灵发生分别在04:46:05和04:47:14,此时雷暴处于消散阶段,正负地闪频数均处于一个较低水平且正地闪比例显著增加,并且多位于云顶亮温?40°C～?50°C的层状云区上空。红色精灵的出现伴随着30～35 dBZ回波面积的增加。在红色精灵发生期间,雷达反射率大于40 dBZ的面积减少,10～40 dBZ的面积增加,表明红色精灵的产生与雷暴对流的减弱和层状云区的发展有关,这与已有的夏季红色精灵的研究结果类似。红色精灵的母体闪电为正地闪单回击,位于中尺度对流系统雷达反射率为25～35 dBZ的层状云降水区,对应的雷达回波顶高分别为2.5 km和5 km,峰值电流分别为+183 kA和+45 kA。根据超低频磁场数据估算两个母体闪电的脉冲电荷矩变化（iCMC）分别为+394 C km和+117 C km。超低频磁天线记录到了第一例红色精灵内部的电流信号,表明这例红色精灵放电很强。     

一例苏皖中尺度对流复合体模拟结果的诊断分析

利用2010年7月22日苏皖中尺度对流复合体（MCC）数值模拟输出结果,考察了模式对MCC的模拟能力,并对模拟结果做了动力和热力诊断分析,以揭示盛夏江淮下游MCC的特征。结果表明：1） 三重嵌套网格距为3.3 km的区域WRF模式的模拟效果较佳,结果与实况一致,并可利用模拟降水的范围及强度来确定MCC的位置及演变。2） 此MCC维持约10 h,其南北不对称,并随西太平洋副热带高压西伸北抬而随之北抬。MCC核心区对流层低层有水汽丰沛的入流,并有强辐合区,呈对流不稳定层结;中层有深厚的强上升运动,并因凝结潜热大量释放呈中性层结;高层则有出流;MCC核心区对流降水非常强。3） 在垂直剖面上,该核心区散度存在中低层辐合、高层辐散的柱状结构,此配置有利于强对流维持和加强,中低层以上有深厚的强上升气流柱,这些都是MCC核心区存在强对流的标志。该MCC的螺旋结构表明其中的强对流高度有组织。     

Long‐term annual surface heat and water balances over Canada and the United States South of 60°N: Reconciliation of precipitation,run‐off and temperature fields

Abstract

The analysis compares the observed field of run‐off (assumed correct) with adjusted precipitation over North America (as amended by den Hartog and LeDrew over Canada) and derives the principal hydroclimatological ratios for each five‐degree latitude‐longitude square. The amended precipitation field yields values of the Budyko dry ness index close to values suggested by the vegetation distribution. The Priestley‐Taylor parameter, α, lies between unity (equilibrium) and potential (1.26) values over much of humid North America, but exceeds these values in the northwest Pacific squares, where advective heating may be the cause. Other regions of strong seasonal advective heating (e.g. the Great Plains) do not appear to influence the distribution strongly. A weighted convective forcing temperature is derived, varying from 298 K in the extreme south to below 285 K in the north. This function (and the Bowen ratio) achieve improbable values in northern Labrador‐ Ungava. The precipitation, run‐off and net radiation régimes appear still to be out of balance in these squares. An adjustment of either precipitation or net radiation by about a tenth corrects the imbalance, but the method is not capable of deciding which field (or both) is in error. Over the rest of the continent the adjusted precipitation field now appears to be in balance with observed run‐off and temperature distributions.     

准噶尔盆地西北缘一次大到暴雨天气过程分析

摘要：通过分析2010年6月２8～２9日发生在准噶尔盆地西北缘的一次大到暴雨天气,揭示了形成这次强降水天气的环流背景特点、物理量和雷达回波特征。结果显示：冷暖气团在克拉玛依地区附近相遇产生的中尺度锋生现象触发了本次暴雨天气过程。表现最明显的特征是：高空槽移动缓慢,中层切变线不断南压、低层中尺度系统维持,冷暖气团在区域强烈交汇。暴雨区雷达速度场有明显的风场幅合。对流降水云团强度、移向变化的预测,是此类天气临近预报的关键和难点。     

地核能量的积累与释放

地核不仅具有巨量热能，而且有巨量旋转能，这是地球能量释放的内因；天文因素使地核产生周期性的南北振荡，是地球能量间歇性释放的外因。地质旋回与天文周期直接相关，可以根据天文周期预测未来的地质变化     

3. Solar System Formation and Early Evolution: the First 100 Million Years

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.     

Internal waves in a rotating stratified spherical shell: asymptotic solutions

Summary. Small amplitude oscillations of a rotating, density-stratified fluid bounded by a spherical shell are examined. No restrictions are placed on the thickness of the shell. The internal mode spectrum is examined in the complete rotation-stratification parameter range including the regime that is appropriate for a plausible stratification distribution in the Earth's fluid core. A mathematical model is derived in terms of an eigenvalue PDE of mixed type. The existence of oscillatory solutions is exhibited in the limits of no rotation and no stratification. The frequency spectrum is extended asymptotically away from these limiting cases. A reduction in the complexity of the PDE for modes oscillating at the inertial frequency is exploited. A variational formulation is constructed in which the stratification parameter is treated as an eigenvalue of the system for fixed wave frequency. The spectral information is again extended asymptotically away from these 'accessible' points. Although the PDE reduces to Laplace's tidal equations (LTE) only under stringent parameter restrictions, it is observed that aspects of the behaviour of low frequency LTE modes are reproduced in the general model.     

GEOCHEMICAL STUDY OF THE CORE S01 IN THE SOUTH CHINA SEA

Si, Ti, Al, Fe, Mn, Ca, Mg, K, Na, P and Sr, Ba, Rb, Ga, V, Zr, Cr, Ni, Co, Cu, Zn, Pb,Nb, Y, Th, La in the core S01 were analyzed and the pattems of their enrichment are discussed.Enrichment of Na, Fe, Mn, Ba, Cu elements in the core indicates volcanic material are an importantsoarce of the sediments in the area. The enrichment frequently varying with the deposition processshows bottom volcanism is frequent in the area and that the studied area is a margin basin with distinctoceanic characteristics. The abnormal enrichment of Mn at the layers(0-15 cm and 665-670 cm) of the core could beclosely related to and so, indicate, the wide deposition hiatus that have occurred in the West PacificOcean and adjacent margin seas since Late Pleistocene.     

Convective-conductive transitions and sensitivity of a convecting ice shell to perturbations in heat flux and tidal-heating rate: Implications for Europa

We investigate the response of conductive and convective ice shells on Europa to variations of heat flux and interior tidal-heating rate. We present numerical simulations of convection in Europa's ice shell with Newtonian, temperature-dependent viscosity and tidal heating. Modest variations in the heat flux supplied to the base of a convective ice shell, ΔF, can cause large variations of the ice-shell thickness Δδ. In contrast, for a conductive ice shell, large ΔF involves relatively small Δδ. We demonstrate that, for a fluid with temperature-dependent viscosity, the heat flux undergoes a finite-amplitude jump at the critical Rayleigh number Racr. This jump implies that, for a range of heat fluxes relevant to Europa, two equilibrium states—corresponding to a thin, conductive shell and a thick, convective shell—exist for a given heat flux. We show that, as a result, modest variations in heat flux near the critical Rayleigh number can force the ice shell to switch between the thin, conductive and thick, convective configurations over a ∼10⁷-year interval, with thickness changes of up to ∼10-30 km. Depending on the orbital and thermal history, such switches might occur repeatedly. However, existing evolution models based on parameterized-convection schemes have to date not allowed these transitions to occur. Rapid thickening of the ice shell would cause radial expansion of Europa, which could produce extensional tectonic features such as fractures or bands. Furthermore, based on interpretations for how features such as chaos and ridges are formed, several authors have suggested that Europa's ice shell has recently undergone changes in thickness. Our model provides a mechanism for such changes to occur.     

Corrections to Solar Thermal Structure when a Turbulent Magnetic Field is Included

Correction of non-ideal effect due to a magnetic fluctuating tensor is derived from the ideal MHD equations. The inclusion of a magnetic turbulent field leads to modifications of the hydrostatic equilibrium equation and thermodynamical variables such as the temperature T, the adiabatic exponent γ, the adiabatic temperature gradient △↓ad and the temperature gradient △↓. In particular, the modifications in the adiabatic and radiative temperature gradients will result in a change in the Schwarzchild criterion, hence in the location of the base of the convective zone. Incorporating the modifications, we construct a modified thermodynamical equilibrium structure of the Sun.