Formation of the Outer Planets

Models of the origins of gas giant planets and ‘ice’ giant planets are discussed and related to formation theories of both smaller objects (terrestrial planets) and larger bodies (stars). The most detailed models of planetary formation are based upon observations of our own Solar System, of young stars and their environments, and of extrasolar planets. Stars form from the collapse, and sometimes fragmentation, of molecular cloud cores. Terrestrial planets are formed within disks around young stars via the accumulation of small dust grains into larger and larger bodies until the planetary orbits become well enough separated that the configuration is stable for the lifetime of the system. Uranus and Neptune almost certainly formed via a bottom-up (terrestrial planet-like) mechanism; such a mechanism is also the most likely origin scenario for Saturn and Jupiter.     

基于多目标决策模型的两栖攻击舰编队编成研究

两栖攻击舰编队编成不能照搬固定的模式,而应根据作战任务和威胁等因素进行合理配置。文章分析了两栖攻击舰编队的作战能力,并在此基础上构建了编成模型的指标体系。运用多目标决策理论,建立了两栖攻击舰编队编成的模型,通过计算得到了针对某作战行动中两栖攻击舰编队的最优编成方案,并将所得到的结果与日常性建制的编队编成进行了比较。     

Formation of Planetesimals and Accretion of the Terrestrial Planets

Planetesimals formed in the solar nebula by collisional coagulation. Dust aggregates settled toward the central plane, the larger ones growing by sweeping up smaller ones. A thin, dense layer of particles formed; shear-generated turbulence and differential motions induced by gas drag inhibited gravitational instability. Growth proceeded by collisions, producing planetesimals on a timescale of a few thousand years in the terrestrial zone. For bodies smaller than about a kilometer, motions were dominated by gas drag, and impact velocities decreased with size. At larger sizes gravitational interactions became significant, and velocities increased due to mutual perturbations. Larger bodies then grew more rapidly, this ``runaway' led to formation of tens to hundreds of lunar- to Mars-sized planetary embryos in the zone of terrestrial planets. The final accretion of these bodies into a few planets involved large impacts, and occurred on a timescale of 10⁷ to 10⁸ years. This scenario gives a reasonably consistent picture of the origin of the terrestrial planets, but does not account for the anomalously low eccentricities of the Earth and Venus. This revised version was published online in June 2006 with corrections to the Cover Date.     

Irregular Satellites in the Context of Planet Formation

All four giant planets in the solar system possess irregular satellites, characterized by large, highly eccentric and/or highly inclined orbits. These bodies were likely captured from heliocentric orbit, probably in association with planet formation itself. Enabled by the use of large-format digital imagers on ground-based telescopes, new observational work has dramatically increased the known populations of irregular satellites, with 74 discoveries in the last few years. A new perspective on the irregular satellite systems is beginning to emerge.We find that the number of irregular satellites measured to a given diameter is approximately constant from planet to planet. This is surprising, given the radically different formation scenarios envisioned for the gas giants Jupiter and Saturn compared to the (much less massive and compositionally distinct) ice giants Uranus and Neptune. We discuss the new results on the irregular satellites and show how these objects might be used to discriminate amongst models of giant planet formation.     

Dust Evolution in Protoplanetary Discs and the Formation of Planetesimals

After 25 years of laboratory research on protoplanetary dust agglomeration, a consistent picture of the various processes that involve colliding dust aggregates has emerged. Besides sticking, bouncing and fragmentation, other effects, like, e.g., erosion or mass transfer, have now been extensively studied. Coagulation simulations consistently show that \(\upmu\mbox{m}\)-sized dust grains can grow to mm- to cm-sized aggregates before they encounter the bouncing barrier, whereas sub-\(\upmu\mbox{m}\)-sized water-ice particles can directly grow to planetesimal sizes. For siliceous materials, other processes have to be responsible for turning the dust aggregates into planetesimals. In this article, these processes are discussed, the physical properties of the emerging dusty or icy planetesimals are presented and compared to empirical evidence from within and without the Solar System. In conclusion, the formation of planetesimals by a gravitational collapse of dust “pebbles” seems the most likely.     

航空兵编队与舰艇编队对抗数理战术

舰艇编队防空武器多样,防空区域层次明确,防空能力相对较强,在基于舰艇编队任务模式和编队组成分析基础上,对其防空系统策略进行研究;针对航空兵的快速机动性和战术灵活性,建立战术攻击策略库,结合基于毁伤等级的毁伤效果评估,进行了航空兵编队对舰艇编队数理战术研究,从而为战术决策提供依据,最后指出进一步研究的方向。     

航空术语的构词分析

以全国科学技术名词审定委员会公布的"航空科学技术名词"为览本,对航空术语的词性和构型进行分析,通过举例作出了某些详述,并推导出对外来术语的吸纳方法和原则。     

Low Velocity Collisions and the Growth of Planetesimals

The physics of low velocity collisions (5 m/s to 40 m/s) between basalt bodies ranging in size from 1 m to 10 km is studied in an effort to investigate the early phases of planetesimal accretions. To assess the importance of the internal structure of planetesimals on the outcome of the collisions, we model them either as solid spheres or as rubble piles with a filling factor of 0.5. The collisions are simulated using a three dimensional Smooth Particle Hydrodynamics (SPH) code that incorporates the combined effects of material strength and a brittle fragmentation model. This approach allows the determination not only of the mass of the largest fragments surviving the collisions but also their dynamical characteristics. We find that low velocity collisions are for equal incoming kinetic energy per gram of target material considerably more efficient in destroying and dispersing bodies than their high velocity counterparts. Furthermore, planetesimals modeled as rubble piles are found to be characterized by a disruption threshold about 5 times smaller than solid bodies. Both results are a consequence of a more efficient momentum transfer between projectile and fragments in collisions involving bodies of comparable sizes. Size and shape dependent gas drag is shown to provide relative collision velocities between similar meter-sized objects well in excess of the critical disruption threshold of either rubble piles or solid bodies. Unless accretion can proceed avoiding collisions between bodies of similar masses, the relative weakness of bodies in this size range creates a serious bottleneck for planetesimal growth. This revised version was published online in June 2006 with corrections to the Cover Date.     

Dynamics and Composition of Rings

Planetary rings are found around all four giant planets of our solar system. These collisional and highly flattened disks exhibit a whole wealth of physical processes involving dust grains up to meter-sized boulders. These processes, together with ring composition, can help understand better the formation and evolution of proto-satellite and proto-planetary disks in the early solar system. The present chapter reviews some fundamental aspects of ring dynamics and composition. The forthcoming exploration of the Saturn system by the Cassini mission will bring both high resolution and time-dependent information on Saturn’s rings.     

航空兵掩护编队对突击编队掩护效能分析建模

研究了掩护编队对突击编队的掩护效能问题,给出了掩护编队的掩护效能定义和模型,修正了无掩护时敌歼击机截击成功概率模型,结合改进后的空战交换比模型,建立了有航空兵掩护编队护航时敌歼击机截击成功概率模型和我突防概率模型,并通过仿真算例验证了模型的有效性和合理性。可为航空兵部队合理进行作战编组、科学制定兵力出动计划提供参考和借鉴。     

多导弹三维编队控制

 多导弹编队控制可极大提高多枚导弹协同作战的效能。重点研究了多导弹编队控制涉及的2个主要问题：编队结构问题和三维编队保持控制器设计问题。提出了改进的领弹-跟随弹编队模式,结合多级分布式控制策略,解决了领弹失效时队形无法保持的问题;设计了基于相对误差的三维非线性跟随弹编队控制器,得到相应的跟踪控制律。不管领弹如何机动,跟随弹与领弹的相对距离始终为指定的期望值,同时跟随弹的速度、航向角和滚转角也能与领弹保持一致,通过仿真验证了所设计的编队控制器具有鲁棒性和稳定性。     

原位钛基复合材料中TiB的生成热力学及动力学

采用自蔓延高温合成（SHS）、感应熔炼和熔模精铸相结合的方法，利用Ti—B—Al体系制备出了原位自生TiB增强的钛基复合材料。借助XRD、SEM和TEM分析了复合材料的物相和增强体的形态。结果表明：在复合材料中只存在TiB增强体和Ti，无TiAl3杂质相形成，TiB增强体呈柱状短纤维，这与其B27晶体结构有关，且增强体／基体界面清洁无杂质污染，并从热力学和动力学两方面论述了在Ti—B—Al体系中制备TiB增强体的生成机制：在Ti-B—Al体系中，Al首先受热熔化使得Ti和B相继溶解于Al液中；Ti与Al之间先行发生化学反应形成Ti—Al金属间化合物，放出的热量进一步引发了溶解于液相中的B和Ti产生高温自蔓延形成Ti—B化合物。以热力学理论分析，应最终形成TiB2，但实际上由于动力学影响，最终形成了TiB。     

主成分分析法在宏观经济评价中的应用

文章主要介绍了主成分分析方法基本思想及其计算步骤,并用主成分分析方法在综合评价方面进行了实证分析,最后提出了在实际应用中应该注意的问题.     

正电子素的络合作用

本文介绍了正电子素及其络合作用。讨论了正电子素络合反应速度常数的测量方法。比较了几种线性自由能的表达式。     

双焦点激光焊接工艺参数对焊缝成形影响

通过利用自行研制的分束焊接头将一束激光分为能量相当的两束激光,在沿焊缝方向上串联产生了两个焦点.通过该试验系统研究了在双焦点激光焊接过程中参数的变化对焊缝成形和熔深的影响规律,探索了双焦点激光焊接最佳工艺的参数调节,试验结果表明,双焦点激光焊接显著改善了焊接质量,焊缝的中心线开裂敏感性也降低.双焦点激光焊接过程中,激光功率、焊接速度、离焦量等参数的变化,均能对焊缝成形和熔深产生显著影响,进而影响焊缝的微观组织和宏观形状.     

Composition Variations in the Solar Corona and Solar Wind

Order of magnitude variations in relative elemental abundances are observed in the solar corona and solar wind. The instruments aboard SOHO make it possible to explore these variations in detail to determine whether they arise near the solar surface or higher in the corona. A substantial enhancement of low First Ionization Potential (FIP) elements relative to high FIP elements is often seen in both the corona and the solar wind, and that must arise in the chromosphere. Several theoretical models have been put forward to account for the FIP effect, but as yet even the basic physical mechanism responsible remains an open question. Evidence for gravitational settling is also found at larger heights in quiescent streamers. The question is why the heavier elements don't settle out completely. This revised version was published online in June 2006 with corrections to the Cover Date.     

无人机紧密编队队形构成控制

针对无人机编队飞行问题,通过借鉴Agent体系结构确定无人机编队的控制结构.建立了以航迹坐标系为参考坐标系的长机与僚机的相对运动模型,根据僚机距离长机最优位置的误差,利用李亚普诺夫稳定性理论设计队形构成中僚机的控制律.最后通过建立的六自由度非线性飞行仿真平台进行仿真验证,结果表明所设计的控制律能稳定引导无人机完成编队的队形构成.     

一种长期稳定的卫星编队队形优化设计方法

 对于卫星编队飞行设计长期稳定以节省控制燃料的队形是一项非常重要的工作，本文提出了一种队形长期稳定的优化设计方法。首先利用Hill方程设计出满足任务要求的相对位置和相对速度的约束关系，以剩下的自由相对位置或相对速度作为优化变量。优化目标选择为主从星在J2摄动下的各平均轨道根数相对漂移率最小。文中的优化算法采用改进的遗传算法，遗传算法作为一种通用的全局最优随机搜索算法，在解决一些复杂问题时它还存在着过早收敛和收敛速度慢的缺陷，针对此问题，本文提出一种改进的遗传算法。仿真结果表明利用这种优化设计方法设计的队形在各种摄动力下能够长期保持稳定。     

Wind in the Solar Corona: Dynamics and Composition

The dynamics of the solar corona as observed during solar minimum with the Ultraviolet Coronagraph Spectrometer, UVCS, on SOHO is discussed. The large quiescent coronal streamers existing during this phase of the solar cycle are very likely composed by sub-streamers, formed by closed loops and separated by open field lines that are channelling a slow plasma that flows close to the heliospheric current sheet. The polar coronal holes, with magnetic topology significantly varying from their core to their edges, emit fast wind in their central region and slow wind close to the streamer boundary. The transition from fast to slow wind then appears to be gradual in the corona, in contrast with the sharp transition between the two wind regimes observed in the heliosphere. It is suggested that speed, abundance and kinetic energy of the wind are modulated by the topology of the coronal magnetic field. Energy deposition occurs both in the slow and fast wind but its effect on the kinetic temperature and expansion rate is different for the slow and fast wind.     

基于Hill方程的编队初始化误差分析

Hill方程具有形式简单、方便编队队形设计和队形保持控制律的设计等优点.然而,由于Hill方程自身模型误差的存在,导致基于Hill方程初始化所建立的队形具有一定的误差.针对这个问题,基于保留二阶非线性项的、改进形式的Hill方程和考虑偏心率的Lawden方程,分别在非线性和偏心率的影响下,分析了初始化队形的长期漂移和相对运动误差问题,分别给出了针对非线性和偏心率影响的修正初始化相对速度,从而消除队形的长期漂移,修正或减小相对运动误差.最后通过数值仿真进行了验证.