Do we understand the inner magnetotail dynamics during substorms?

Substorm evolution of the near-Earth (|X|<15 R_E) plasma sheet has been emphasized recently because the inner tail is thought to link closely to the substorm auroral activity in the ionosphere during the early stage of substorms. In this paper, we discuss how the inner tail substorm phenomena during the late substorm growth phase and early expansion phase are accounted for by the two prevailing substorm models, namely, the near-Earth neutral line model and the current disruption model. We find that the late growth phase features are more satisfactorily accounted for by the current disruption model than by the near-Earth neutral line model. In addition, detailed observations on current disruption show evidence inconsistent with the proposed idea of dipolarization being due to plasma flow braking from reconnection in the mid-tail region, which poses a difficulty to the near-Earth neutral line model as well.     

PAMELA observational capabilities of Jovian electrons

PAMELA is a satellite-borne experiment that has been launched on June 15th, 2006. It is designed to make long duration measurements of cosmic radiation over an extended energy range. Specifically, PAMELA is able to measure the cosmic ray antiproton and positron spectra over the largest energy range ever achieved and will search for antinuclei with unprecedented sensitivity. Furthermore, it will measure the light nuclear component of cosmic rays and investigate phenomena connected with solar and earth physics. The apparatus consists of: a time of flight system, a magnetic spectrometer, an electromagnetic imaging calorimeter, a shower tail catcher scintillator, a neutron detector and an anticoincidence system. In this work a study of the PAMELA capabilities to detect electrons is presented. The Jovian magnetosphere is a powerful accelerator of electrons up to several tens of MeV as observed at first by Pioneer 10 spacecraft (1973). The propagation of Jovian electrons to Earth is affected by modulation due to Corotating Interaction Regions (CIR). Their flux at Earth is, moreover, modulated because every 13 months Earth and Jupiter are aligned along the average direction of the Parker spiral of the Interplanetary Magnetic Field.PAMELA will be able to measure the high energy tail of the Jovian electrons in the energy range from 50 up to 130 MeV. Moreover, it will be possible to extract the Jovian component reaccelerated at the solar wind termination shock (above 130 MeV up to 2 GeV) from the galactic flux.     

复杂外形网格生成技术及应用

以某型双立尾战斗机为例,给出了实际复杂型号飞行器结构网格生成的一种分块方案及实现过程,用一种矢性三次多项式插值的方法生成相邻块公共交界面的网格,用Hilgenstock方法修正源项,求解椭圆型方程生成块内空间网格,使网格线与边界面夹角、与边界面间距控制为期望的值.在所生成的双立尾战斗机分块结构网格中求解Euler方程,获得了合理的全机气动力系数、翼面压力分布和绕流图谱结果.     

歼击机特殊部件设计载荷谱编制技术

介绍了用飞行模拟仿真法编制新机设计载荷谱的技术途径和特点.重点阐述了整体油箱压力/应力谱和垂尾阵风侧滑机动谱等歼击机特殊部件设计载荷谱编制技术.整体油箱载荷谱编制的关键在于各种载荷状态的压力计算,还应考虑地-空-地循环.垂尾谱不能完全由飞行模拟获得,而必须以空测统计数据为基础.     

基于FGN输入流的G/D/1排队模拟

传统的排队理论不适于分析高速网络表现出的自相似流量.通过实验仿真,主要考察平均等待时间和在队列分别为无限和有限情形下的队列尾部特征等参数,并对以FGN为输入流的G/D/1排队模型作了定性分析.结果表明在输入流的强度和方差基本相等且系统利用律大于某一阈值的情况下,队列平均等待时间随Hurst参数增大而显著增长.同时指出在相同的条件下考察队列尾部特征,具有有限队列长度的G/D/1排队模拟结果要远优于无限队列长度下的理论分析结果.      

The Halley dust model

The properties of dust ejecta from Comet Halley are studied on the basis of (a) evidence from the comet's past apparitions and (b) analogy with recent, physically similar comets. Specifically discussed are the light curve and spectrum, discrete phenomena in the head, the physical properties of the nucleus (size, albedo, rotation, surface temperature, and morphology), and an interaction between the nucleus and dust atmosphere. Also reviewed are constraints on the size and mass distributions of dust particles, information on submicron-size and submillimeter-size grains from the comet's dust tail and antitail, and the apparent existence of more than one particle type. Similarities between the jet patterns of Halley and the parent comet of the Perseid meteor stream are depicted, and effects of the surface heterogeneity (discrete active regions) on the dust flow are assessed. Current dust models for Halley are summarized and the existence of short-term variations in the dust content in the comet's atmosphere is suggested.     

降落伞充气过程研究方法综述

文章介绍了降落伞充气过程的研究方法 ,包括完全试验方法、半试验半理论方法及完全理论方法。其中 ,着重介绍了半试验半理论方法及完全理论方法的内容及发展状况。在介绍各种研究方法的同时 ,阐述了降落伞充气过程包含的复杂物理现象、研究难点及解决方法 ;最后指出了当前充气过程研究的热点及发展趋势。     

The plasma regime at comet Giacobini-Zinner

This review of the plasma regime sampled by the encounter of the International Cometary Explorer spacecraft (ICE) with the comet Giacobini-Zinner, discusses the shock, or bow wave, ion pickup, ionization mechanisms, and the cometary plasma tail.

The observations are consistent with the existence of a weak shock, which may be pulsating, but do not exclude the suggestion by Wallis and Dryer that the shock, though present around the sub-solar point, is in process of decaying to a wave on the flanks.

Pickup of cometary ions provokes, by means of several mechanisms, ion cyclotron, mirror, beam and electrostatic instabilities which cause strong turbulence in the inner coma, as indicated in the power spectra of the magnetic field in the coma and the surrounding volume. Heavy mass loading and consequent slowing down of the solar wind is observed. Acceleration of ions by a stochastic mechanism is indicated.

Ionization of cometary neutrals occurs principally by photoionization and charge exchange. Alfvens critical velocity mechanism, likely operates only in the inner coma not visited by ICE. A steep increase of nearly two orders of magnitude in electron density occurs in the tail, where electron velocity distributions show evidence of entry of electrons from the solar wind. The turbulence there is damped by the high ion density and low temperature.

In general, the vicinity of the comet is filled with plasma phenomena and a rich variety of corresponding atomic and molecular processes can be studied there. Comparison between the ICE, Giotto, and Vega observations forms a most valuable future study.     

直升机飞行数值仿真中尾桨动力学模型探讨

针对常规单旋翼带尾桨直升机,通过对尾桨挥舞运动方程,尾桨动力入流模型,旋翼和机身在尾桨处侧沅的分析与计算,探讨尾桨动力学模型中不同因素对于直升机整机直线飞行状态的配平和驾驶员纵输入动态响应数值仿真精度的影响程度,为不同目的飞行数据仿真中尾桨动力学模型选取提供参考,本文以ＵＨ－６０Ａ直升机的算例进行了对比分析。     

Ground-based observations of the dust emission from comet Halley

A preliminary analysis of the dust emission from comet Halley is presented based on large scale observations of its dust tail. Selected images obtained between February 22 and May 10, 1986 are compared to synchrone-syndyne graphs to infer the history of the dust production and the properties of the dust, at least qualitatively. Quantitative modeling of the dust tall has also been initiated and preliminary results are shown for the cases of isotropic and anisotropic (jet) dust production.     

Active stars and systems

The most notable manifestations of stellar activity are reviewed with particular emphasis on the merging picture of solar-type activity in physical conditions different from those in the Sun. Evidence for starspots, plages and high-level coronal emissions is presented from observations covering a wide range of spectral bands: from X-ray to radio wavelengths. The main physical parameters of the active areas in the active stars, when compared with solar values, indicate that the basic requirement for activity phenomena to develop is the presence of observationally elusive localized magnetic fields on and above the stellar surface. The importance of coordinated programs involving simultaneous observations from the ground and from space - aiming at empirical and theoretical modeling of activity phenomena - is stressed.     

一种模拟长期失重影响的大鼠尾部悬吊模型

本文改进了Morey-Holton和wronski的大鼠尾部悬吊方法,还总结出了一套不致对尾部造成损伤的长期尾部悬吊技术。用此方法,完成了五批(每批10只)为期90—120天的悬吊实验。结果表明:引起的应激程度轻微;悬吊组大鼠体重增长与对照大鼠接近。可用来对长期失重生理影响及其机理进行研究。     

Modeling the radiation belts: what are the important physical processes to be taken into account in models?

During active periods, physical processes acting on particle dynamics are well known to have several origins and can play a role at different times, different locations, and with different time scales. As their effects can be opposite, it is necessary to identify them and their relative importance:

• the particle sources (plasmasheet or direct solar wind entry)

• the particle losses (precipitation or drift loss)

• the particle transport and acceleration (convection access, magnetic or electric pulse or variation and recirculation).

The various phenomena are explained and results are presented. In particular, we demonstrate that classical diffusion models like the Salammbo code can account for all these phenomena.     

Measurements of the artificially stimulated precipitation of electrons from the inner radiation belt in the experiment “SPOLOKH-2”

Evidence for an enhancement of the electron flux associated with a barium chaped charge release from “SPOLOKH-2” rocket payload, launched from Volgograd (L = 2.2) on June 29, 1978, will be presented. There is also evidence for a periodic train of particle bursts occurring with about 11 second period during more than 100 seconds after the release. The observed phenomena is interpreted as a “trigger-effect”.     

哈雷彗星等离子体彗尾亮度分布的理论分析

本文借助Nazarchuk的扩散理论模型和有关资料, 分析了1986年1月4日哈雷彗星等离子体彗尾的尾轴方向及其垂直方向的相对亮度分布, 推算出CO+离子的平均寿命、纵向(沿尾轴)和横向扩散系数, 估算了磁场强度, 最后进行一些讨论.      

有界双重控制导弹微分对策制导律

针对有界控制导弹采用鸭舵或尾舵单一控制形式存在的劣势,基于双边优化微分对策理论,推导了一种有界双重控制导弹微分对策制导律。该制导律不仅将鸭舵与尾舵两组舵面的控制有效融合在一起,而且实现了有界控制命令最优的分配设计。分析了该微分对策制导律的对策空间,并从弹目机动性能比和控制系统时间常数比之间的关系,给出了鞍点解的存在条件。考虑非完全信息情形,完成了目标加速度滤波器和拦截性能衡量指标的设计。采用Monte Carlo法进行了制导性能的仿真验证,结果表明:所设计的有界双重控制导弹制导律与采用单一的鸭舵控制或尾舵控制的导弹相比不仅机动性要求较低,且具有较高的命中概率。      

等离子体彗尾动力学的数值研究

本文基于可压缩磁流体动力学模型,数值研究了尾瓣巾具有超Alfven速流动的等离子体彗尾的动力学特征。结果表明,等离子体片和尾瓣之间的剪切等离子体流动将会激发流动撕裂模不稳定性,引起彗尾等离子体片中发生磁场重联,形成磁岛和高密度的等离子体团。进而模拟了太阳风引起的局部驱动力对等离子体彗尾中磁场重联的影响,其特征时间远大于流动撕裂模。我们认为一些观测到的等离子体彗尾中的四块和彗尾截断事件可能主要与彗尾中剪切等离子体流动所引起的流动撕裂模不稳定性有关。      

钻尖数控刃磨中的尾隙角研究

通过对尾隙角的分析研究,提出了作用尾隙角的概念,给出了作用尾隙角的计算方法,研究了刃磨参数对作用尾隙角的影响.给出了作用尾隙角在数控刃磨求取刃磨参数中的应用方法.研究表明,尾隙角是关系到钻头钻削性能的重要参数,数控刃磨中的几个刃磨参数对它的影响程度由大至小的次序为θ、C_y、σ、ω、C_x.     

Improving magnetosphere in situ observations using solar sails

Past and current magnetosphere missions employ conventional spacecraft formations for in situ observations of the geomagnetic tail. Conventional spacecraft flying in inertially fixed Keplerian orbits are only aligned with the geomagnetic tail once per year, since the geomagnetic tail is always aligned with the Earth-Sun line, and therefore, rotates annually. Solar sails are able to artificially create sun-synchronous orbits such that the orbit apse line remains aligned with the geomagnetic tail line throughout the entire year. This continuous presence in the geomagnetic tail can significantly increase the science phase for magnetosphere missions. In this paper, the problem of solar sail formation design is explored using nonlinear programming to design optimal two-craft, triangle, and tetrahedron solar sail formations, in terms of formation quality and formation stability. The designed formations are directly compared to the formations used in NASA’s Magnetospheric Multi-Scale mission.