应用电磁弹射器的舰载机起飞性能分析

针对应用电磁弹射器的舰载机弹射起飞过程,综合考虑了电磁弹射器的推力、舰载机前起落架突伸力和载舰的运动,建立了舰载机弹射起飞的数学模型,并据此,分析了上述各种因素对舰载机弹射起飞安全性的影响,计算得到在满足舰载机弹射起飞安全准则的条件下,各种起飞因素应该满足的适应范围。研究分析表明：在风浪较大的恶劣天气条件下,通过适当地增加电磁弹射器的电磁推力和前起落架的突伸力,可以有效抑制舰载机的航迹下沉现象,确保舰载机的安全起飞过程。     

GH4199合金渗铝工艺研究

主要针对渗铝工艺中不同渗铝温度、保温时间对GH4199合金组织、性能影响进行试验,试验结果表明渗层组织由表及里分别为：表层主要为富铝的NiAl相,向内的过渡层和扩散层为富Cr相、碳化物、NiAl相和Ni3Al相等。渗层厚度的变化主要与温度和时间有关,同一渗铝温度下,随着渗铝时间的增加渗铝层深度增加;同一渗铝时间,随着渗铝温度的提高渗铝层深度增加。经渗铝处理后,室温拉伸强度提高,拉伸塑性降低。900℃拉伸强度降低,拉伸塑性提高;持久寿命稍降低,塑性提高。     

The Magnetic Field of Mercury

The magnetic field strength of Mercury at the planet’s surface is approximately 1% that of Earth’s surface field. This comparatively low field strength presents a number of challenges, both theoretically to understand how it is generated and observationally to distinguish the internal field from that due to the solar wind interaction. Conversely, the small field also means that Mercury offers an important opportunity to advance our understanding both of planetary magnetic field generation and magnetosphere-solar wind interactions. The observations from the Mariner 10 magnetometer in 1974 and 1975, and the MESSENGER Magnetometer and plasma instruments during the probe’s first two flybys of Mercury on 14 January and 6 October 2008, provide the basis for our current knowledge of the internal field. The external field arising from the interaction of the magnetosphere with the solar wind is more prominent near Mercury than for any other magnetized planet in the Solar System, and particular attention is therefore paid to indications in the observations of deficiencies in our understanding of the external field. The second MESSENGER flyby occurred over the opposite hemisphere from the other flybys, and these newest data constrain the tilt of the planetary moment from the planet’s spin axis to be less than 5°. Considered as a dipole field, the moment is in the range 240 to 270 nT-R _M ³ , where R _M is Mercury’s radius. Multipole solutions for the planetary field yield a smaller dipole term, 180 to 220 nT-R _M ³ , and higher-order terms that together yield an equatorial surface field from 250 to 290 nT. From the spatial distribution of the fit residuals, the equatorial data are seen to reflect a weaker northward field and a strongly radial field, neither of which can be explained by a centered-dipole matched to the field measured near the pole by Mariner 10. This disparity is a major factor controlling the higher-order terms in the multipole solutions. The residuals are not largest close to the planet, and when considered in magnetospheric coordinates the residuals indicate the presence of a cross-tail current extending to within 0.5R _M altitude on the nightside. A near-tail current with a density of 0.1 μA/m² could account for the low field intensities recorded near the equator. In addition, the MESSENGER flybys include the first plasma observations from Mercury and demonstrate that solar wind plasma is present at low altitudes, below 500 km. Although we can be confident in the dipole-only moment estimates, the data in hand remain subject to ambiguities for distinguishing internal from external contributions. The anticipated observations from orbit at Mercury, first from MESSENGER beginning in March 2011 and later from the dual-spacecraft BepiColombo mission, will be essential to elucidate the higher-order structure in the magnetic field of Mercury that will reveal the telltale signatures of the physics responsible for its generation.     

快速响应侦察的测控通信与地面站布设研究

快速响应侦察是空间快速响应技术的一个重要应用,而合理布设地面站以保障侦察卫星的发射测控和快速数据回收是侦察任务顺利完成的基础。通过分析近地快速覆盖轨道和近地重复覆盖轨道的对地覆盖特性,针对发射测控和快速数据回收提出了地面站的布设原则,结合我国领土特点给出了这2类轨道的地面站布设方案,并求解了该方案所能提供的发射测控弧段长度和侦察数据返回时间。分析表明,在我国境内布设地面站以保障快速响应侦察卫星的发射测控和快速数据回收是可行的,其数据返回时间小于1个轨道周期。     

Elemental Abundances in Coronal Structures

A great deal of evidence for elemental abundance variations among different structures in the solar corona has accumulated over the years. Many of the observations show changes in the relative abundances of high- and low-First Ionization Potential elements, but relatively few show the absolute elemental abundances. Recent observations from the SOHO satellite give absolute abundances in coronal streamers. Along the streamer edges, and at low heights in the streamer, they show roughly photospheric abundances for the low-FIP elements, and a factor of 3 depletion of high-FIP elements. In the streamer core at 1.5 R·, both high- and low-FIP elements are depleted by an additional factor of 3, which appears to result from gravitational settling. This revised version was published online in June 2006 with corrections to the Cover Date.     

基于Linux军用TCP/IP协议栈设计与实现

提出一种在嵌入式Linux操作系统上运行TCP/IP协议的解决方案。介绍了Linux内核,在此基础上结合嵌入式系统特点,对TCP/IP协议栈进行简化,提出总协议栈的体设计。根据军用通讯要求着重讨论了网络协议的安全问题,参考现在通用的网络安全模式PGP,对TCP/IP协议栈进行修改,主要是在应用层中加入了加密、认证以及密钥分配过程。加密过程采用DES和RSA组合算法,保证其安全性、可行性以及时效性。     

粉末耐热钛合金组织性能及成形技术

采用热等静压技术及旋转电极粉,采用预合金粉粉末冶金工艺开展了粉末耐热钛合金TC11(Ti-6.5AJ-3.5Mo-1.5Zr-0.3Si)制备技术研究,研制出了全致密粉末TC11合金,通过热处理工艺研究优化粉末TC11材料的组织和性能.利用光学显微镜,对其组织进行了分析,用SEM观察了旋转电极粉末形貌,对室温及高温(550℃)拉伸性能及弹性模量等进行了测试分析.粉末TC11合金的组织和性能与同批次TC11锻棒材料进行了对比研究.利用特殊模具成形,开展了粉末TC11构件近净成形技术的研究,实现了整体大尺寸、带网格加强筋的薄壁粉末TC11合金航天飞行器舱体件近净成形,且未检测出内部缺陷.研究结果表明,粉末TC11合金具有与锻造材料相当的拉伸性能,而弹性模量更优,其金相组织均匀细致,形成了网篮组织,并有围绕其分布的等轴α.粉末TC11合金及合适的近净成形技术可在高性价比、高可靠性的轻质耐热航天飞行器构件制备中得到应用.     

微量Al 掺杂对2D C/ SiC 性能的影响

以二维编织碳纤维碳布为预制体,采用聚铝碳硅烷(PACS)为聚合物前驱体,应用化学气相渗透(CVI)结合聚合物浸渗-裂解(PIP)工艺制备微量Al掺杂2D C/SiC复合材料。研究微量Al掺杂对C/SiC微观结构、力学、热膨胀和氧-乙炔焰烧蚀性能的影响。结果表明:掺杂微量Al未改变C/SiC的微观结构和热膨胀性能,也未降低其韧性和强度;但微量Al掺杂提高了C/SiC的抗烧蚀性能,含微量Al的SiC氧化形成微量Al熔于SiO2的固熔体,微量Al提高了SiO2的黏度和致密度,减小SiO2挥发,较未掺杂Al的C/SiC相比,线烧蚀率降低了26%。     

Introduction

Space Science Reviews -     

Solar Wind Electron Proton Alpha Monitor (SWEPAM) for the Advanced Composition Explorer

The Solar Wind Electron Proton Alpha Monitor (SWEPAM) experiment provides the bulk solar wind observations for the Advanced Composition Explorer (ACE). These observations provide the context for elemental and isotopic composition measurements made on ACE as well as allowing the direct examination of numerous solar wind phenomena such as coronal mass ejections, interplanetary shocks, and solar wind fine structure, with advanced, 3-D plasma instrumentation. They also provide an ideal data set for both heliospheric and magnetospheric multi-spacecraft studies where they can be used in conjunction with other, simultaneous observations from spacecraft such as Ulysses. The SWEPAM observations are made simultaneously with independent electron and ion instruments. In order to save costs for the ACE project, we recycled the flight spares from the joint NASA/ESA Ulysses mission. Both instruments have undergone selective refurbishment as well as modernization and modifications required to meet the ACE mission and spacecraft accommodation requirements. Both incorporate electrostatic analyzers whose fan-shaped fields of view sweep out all pertinent look directions as the spacecraft spins. Enhancements in the SWEPAM instruments from their original forms as Ulysses spare instruments include (1) a factor of 16 increase in the accumulation interval (and hence sensitivity) for high energy, halo electrons; (2) halving of the effective ion-detecting CEM spacing from ∼5° on Ulysses to ∼2.5° for ACE; and (3) the inclusion of a 20° conical swath of enhanced sensitivity coverage in order to measure suprathermal ions outside of the solar wind beam. New control electronics and programming provide for 64-s resolution of the full electron and ion distribution functions and cull out a subset of these observations for continuous real-time telemetry for space weather purposes. This revised version was published online in June 2006 with corrections to the Cover Date.