气溶胶对雷暴云起电以及闪电发生率影响的数值模拟

本文利用二维耦合气溶胶模块的雷暴云起电模式,结合一次南京雷暴个例,进行250 m分辨率雷暴云起电模拟实验,探讨了气溶胶浓度对雷暴云空间电荷分布以及闪电发生率的影响。在这个气溶胶模块中,假定一个三模态的气溶胶对数分布,考虑了气溶胶活化过程。结果显示:(1)随着气溶胶浓度增大,雷暴云电荷结构保持为三极型。(2)当气溶胶浓度从50 cm-3增加至1000 cm-3时,水成物粒子浓度上升,雷暴云电荷量和闪电发生率增加明显。(3)气溶胶浓度在1000~3000 cm-3范围时,云水竞争限制了冰晶的增长,导致雷暴云上部主正电荷堆电荷量降低。云滴和霰粒子浓度缓慢上升促进中部主负电荷堆和底部次正电荷堆电荷量继续增大。闪电发生率保持稳定。(4)当气溶胶浓度大于3000 cm-3时,水成物粒子浓度稳定,云内的电荷量以及闪电发生率保持为一定量级。     

Tropical Cyclone Energy Dispersion and Possible Self Maintenance Mechanism of the Synoptic Scale Wave Trains

The interaction between tropical cyclone (TC) and the large-scale mean flows such as the inter-tropical convergence zone (ITCZ) is investigated using a three-dimensional primitive equation model. Once a TC develops in the vicinity of the ITCZ region where satisfies both barotropic and baroclinic instabilities, the southeastward energy dispersion from the TC may disturb the ITCZ and thus help its breakdown. Cumulus convection can be organized in the region of cyclonic circulation, and the interaction between convective heating and the perturbation circulation may enhance the development of the waves, leading to the generation of a new tropical cyclone to the east. While the TC moves to the high latitude, the ITCZ will reform. Though repeating of this process, a synoptic-scale wave train oriented in the northwest-southeast direction can be generated and self-maintained. The results suggest that the mutual interaction among the low-frequency background flow, wave train pattern and TCs provides a possible mechanism for the origin of the summer synoptic scale wave train pattern over the western North Pacific.     

Swift时代伽马射线暴的观测和理论

伽马射线暴是宇宙中最剧烈的爆发现象之一.Swift卫星的快速定位和Fermi卫星的宽、高能段观测,使得伽马暴的观测可以全波段进行.通过Swift的观测可以对伽马暴现象的本质有进一步的理解,而Fermi卫星提供了一些暴高能光子的辐射数据,为进一步研究暴的辐射机制和伽马暴以及它的余辉提供了有力的依据.介绍了Swift和Fermi卫星发射后一些伽马暴的观测和理论研究进展.     

银河系卫星星系研究进展

对银河系内卫星星系进行全面的"人口普查"具有重要的意义。目前已经发现了二十几个卫星星系,其光度范围分布很广,最暗的矮星系比球状星体还暗。叙述了卫星星系的光度分布、空间分布和动力学性质。总结了观测和理论研究进展,并讨论了星流和伽玛射线在研究银河系结构和暗物质性质方面的贡献。表明了卫星星系的统计分布能用来很好地限制冷暗物质理论和星系形成的相关物理过程,同时指出当前研究的局限性和可能的发展方向。     

Impact megadomes and the origin of the martian crustal dichotomy

We show that a sufficiently energetic impact can generate a melt volume which, after isostatic adjustment and differentiation, forms a spherical cap of crust with underlying depleted mantle. Depending on impact energy and initial crustal thickness, a basin may be retained or impact induced crust may be topographically elevated. Retention of a martian lowland scale impact basin at impact energies ∼3 × 10²⁸-3 × 10²⁹ J requires an initial crustal thickness greater than 10 km. Formation of impact induced crust with size comparable to the martian highlands requires a larger impact energy, ∼1-3 × 10³⁰ J, and initial crustal thickness <20 km. Furthermore, we show that the boundary of impact induced crust can be elliptical due to a spatially asymmetric impact melt volume caused by an oblique impact. We suggest the term “impact megadome” for topographically elevated, impact induced crust and propose that processes involved in megadome formation may play an important role in the origin of the martian crustal dichotomy.     

论四川盆地地下卤水资源开发利用的现状及对策

四川盆地地下卤水资源储量大,卤水浓度较高,并含有I、Br、K、Li等多种有用组分。地下卤水多沿构造隆起部位富集,并具有天然气和卤水同层的特点。指出目前对地下卤水开发利用发展不均的现状,以及多以制盐为主,开发利用单一等现象。提出深化对地下卤水资源量的评价,加强对地下卤水综合利用的研究,组成跨行业的开发实体等建议。     

扬子克拉通西缘穹状变形变质体的类型与成因

扬子克拉通西缘呈分散状产出的一系列穹状变形交质体，按其结构特征与成因，可将其划分为变质核杂岩，岩浆核杂岩，片麻岩穹隆和构造穹隆四种类型。造山后期—期后，深部上隆，浅部伸展，局部岩浆活动和造山期深熔花岗岩底辟侵位所引起的地壳局部隆升与伸展，是形成该区变质核杂岩和岩浆核杂岩的主要原因；片麻岩穹隆和构造穹隆，则分别为双向挤压收缩体制下，局部熔融—重熔花岗岩同构造被动侵位，和单纯的构造变形与叠加变形形成。它们具不同的时、空分布和控矿特征，是扬子克拉通西缘造山过程中不同构造坏境，不同演化阶段和不同构造体制下的产物。     

Metallicity and kinematical clues to the formation of the Local Group

The kinematics and elemental abundances of resolved stars in the nearby Universe can be used to infer conditions at high redshift, trace how galaxies evolve and constrain the nature of dark matter. This approach is complementary to direct study of systems at high redshift, but I will show that analysis of individual stars allows one to break degeneracies, such as between star formation rate and stellar Initial Mass Function, that complicate the analysis of unresolved, distant galaxies (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Highly reducing conditions during core formation on Mercury: Implications for internal structure and the origin of a magnetic field

The high average density and low surface FeO content of the planet Mercury are shown to be consistent with very low oxygen fugacity during core segregation, in the range 3-6 log units below the iron-wüstite buffer. These low oxygen fugacities, and associated high metal content, are characteristic of high-iron enstatite (EH) and Bencubbinite (CB) chondrites, raising the possibility that such materials may have been important building blocks for this planet. With this idea in mind we have explored the internal structure of a Mercury sized planet of EH or CB bulk composition. Phase equilibria in the silicate mantle have been modeled using the thermodynamic calculator p-MELTS, and these simulations suggest that orthopyroxene will be the dominant mantle phase for both EH and CB compositions, with crystalline SiO₂ being an important minor phase at all pressures. Simulations for both compositions predict a plagioclase-bearing “crust” at low pressure, significant clinopyroxene also being calculated for the CB bulk composition. Concerning the core, comparison with recent high pressure and high temperature experiments relevant to the formation of enstatite meteorites, suggest that the core of Mercury may contain several wt.% silicon, in addition to sulfur. In light of the pressure of the core-mantle boundary on Mercury (∼7 GPa) and the pressure at which the immiscibility gap in the system Fe-S-Si closes (∼15 GPa) we suggest that Mercury’s core may have a complex shell structure comprising: (i) an outer layer of Fe-S liquid, poor in Si; (ii) a middle layer of Fe-Si liquid, poor in S; and (iii) an inner core of solid metal. The distribution of heat-producing elements between mantle and core, and within a layered core have been quantified. Available data for Th and K suggest that these elements will not enter the core in significant amounts. On the other hand, for the case of U both recently published metal/silicate partitioning data, as well as observations of U distribution in enstatite chondrites, suggest that this element behaves as a chalcophile element at low oxygen fugacity. Using these new data we predict that U will be concentrated in the outer layer of the mercurian core. Heat from the decay of U could thus act to maintain this part of Mercury’s core molten, potentially contributing to the origin of Mercury’s magnetic field. This result contrasts with the Earth where the radioactive decay of U represents a negligible contribution to core heating.     

Planetesimal formation by turbulent concentration

The formation of 1-1000 km diameter planetesimals from dust grains in a protoplanetary disk is a key step in planet formation. Conventional models for planetesimal formation involve pairwise sticking of dust grains, or the sedimentation of dust grains to a thin layer at the disk midplane followed by gravitational instability. Each of these mechanisms is likely to be frustrated if the disk is turbulent. Particles with stopping times comparable to the turnover time of the smallest eddies in a turbulent disk can become concentrated into dense clumps that may be the precursors of planetesimals. Such particles are roughly millimeter-sized for a typical protoplanetary disk. To survive to become planetesimals, clumps need to form in regions of low vorticity to avoid rotational breakup. In addition, clumps must have sufficient self gravity to avoid break up due to the ram pressure of the surrounding gas. Given these constraints, the rate of planetesimal formation can be estimated using a cascade model for the distribution of particle concentration and vorticity within eddies of various sizes in a turbulent disk. We estimate planetesimal formation rates and planetesimal diameters as a function of distance from a star for a range of protoplanetary disk parameters. For material with a solar composition, the dust-to-gas ratio is too low to allow efficient planetesimal formation, and most solid material will remain in small particles. Enhancement of the dust-to-gas ratio by 1-2 orders of magnitude, either vertically or radially, allows most solid material to be converted into planetesimals within the typical lifetime of a disk. Such dust-to-gas ratios may occur near the disk midplane as a result of vertical settling of short-lived clumps prior to clump breakup. Planetesimal formation rates are sensitive to the assumed size and rotational speed of the largest eddies in the disk, and formation rates increase substantially if the largest eddies rotate more slowly than the disk itself. Planetesimal formation becomes more efficient with increasing distance from the star unless the disk surface density profile has a slope of −1.5 or steeper as a function of distance. Planetesimal formation rates typically increase by an order-of-magnitude or more moving outward across the snow line for a solid surface density increase of a factor of 2. In all cases considered, the modal planetesimal size increases with roughly the square root of distance from the star. Typical modal diameters are 100 km and 400 km in the regions corresponding to the asteroid belt and Kuiper belt in the Solar System, respectively.