钣金件快速精确加工中的激光切割工艺分析

针对δ0．5mm～δ6mm钣金件的结构特点,通过比较常用加工工艺和激光切割过程工艺．选出适合实际的优化方案。验证了不同切割参数对切割质量的影响。在工艺参数为：脉冲功率2．4kW、脉冲宽度约10ms、功率密度10^7W/cm^2的情况下,激光切割δ0．5mm～δ6mm钣金件获得了良好的切割质量,尺寸精度控制在误差（±100μm）范围内。工艺方案合理,生产率高。     

Chaotic exchange of solid material between planetary systems: implications for lithopanspermia

Abstract We examined a low-energy mechanism for the transfer of meteoroids between two planetary systems embedded in a star cluster using quasi-parabolic orbits of minimal energy. Using Monte Carlo simulations, we found that the exchange of meteoroids could have been significantly more efficient than previously estimated. Our study is relevant to astrobiology, as it addresses whether life on Earth could have been transferred to other planetary systems in the Solar System's birth cluster and whether life on Earth could have been transferred from beyond the Solar System. In the Solar System, the timescale over which solid material was delivered to the region from where it could be transferred via this mechanism likely extended to several hundred million years (as indicated by the 3.8-4.0?Ga epoch of the Late Heavy Bombardment). This timescale could have overlapped with the lifetime of the Solar birth cluster (～100-500?Myr). Therefore, we conclude that lithopanspermia is an open possibility if life had an early start. Adopting parameters from the minimum mass solar nebula, considering a range of planetesimal size distributions derived from observations of asteroids and Kuiper Belt objects and theoretical coagulation models, and taking into account Oort Cloud formation models, we discerned that the expected number of bodies with mass>10?kg that could have been transferred between the Sun and its nearest cluster neighbor could be of the order of 10(14) to 3·10(16), with transfer timescales of tens of millions of years. We estimate that of the order of 3·10(8)·l (km) could potentially be life-bearing, where l is the depth of Earth's crust in kilometers that was ejected as the result of the early bombardment. Key Words: Extrasolar planets-Interplanetary dust-Interstellar meteorites-Lithopanspermia. Astrobiology 12, 754-774.     

脉冲TIG焊参数对铝合金焊缝组织与性能的影响

通过采用脉冲变极性TIG焊接方法对1.5 mm厚的5A06铝合金和L3纯铝以及3 mm厚的5A06铝合金和5A06铝合金试板进行焊接试验,研究了在其它两个条件不变的情况下脉冲频率、基值电流和占空比分别对焊缝组织与力学性能的影响规律。研究结果表明:当脉冲频率为100 Hz,基值电流为峰值电流的10%～33%,占空比为50%～66%时,焊缝具有良好的组织和力学性能。     

Large and Fast Variations of Parameters in the Magnetosheath: 3. Amplitudes and Transverse Profiles of Low and High Frequency Variations of the Plasma and Magnetic Field

We present the results of experimental studies of high frequency (with periods of seconds and tens of seconds) and low frequency (with periods of minutes and tens of minutes) large variations of the ion flux and magnetic field magnitude in the magnetosheath. It is shown that, on average, the relative amplitudes of these variations are approximately two times higher than similar values characteristic for the undisturbed solar wind. The averaged spatial profile of these values and their variations across the magnetosheath is obtained, as are the dependencies of normalized plasma fluxes and their variations on the place of entrance of a given plasma element into the magnetosheath. Using one particular example, a good coincidence between the time profiles of ion fluxes measured aboard two spacecraft separated by a distance of 10R _E along the magnetosheath is demonstrated.     

高压太阳电池阵静电放电产生脉冲信号的特性研究

研究高压太阳电池阵静电放电产生脉冲信号的特性,有助于深入了解太阳电池阵充放电形成机制。在试验中,利用电子枪模拟GEO空间带电环境,辐照太阳电池样品表面。利用电流探头CT-2、单极子天线和数字存储示波器测量静电放电所产生的脉冲电流、辐射电场并记录其波形。试验结果表明:太阳电池在静电放电过程中产生了脉冲宽度为几μs的瞬态电流,其峰值幅度为几A;辐射电场的脉冲信号持续时间几百ns至几个μs,其峰值幅度达数百V/m。脉冲信号的时域特征表现为脉冲群,其波形具有陡峭的前沿,能量分布的频率范围主要集中在0.1~50 MHz之间。最后根据上述研究对在轨静电放电测试仪的设计提出建议。     

一种带上电时序控制及过脉宽保护功能的大功率调制电路研究

大功率脉冲调制电路根据雷达系统所需脉冲宽度及重频将连续电压信号调制为脉冲工作电压,可以改善GaN功率器件的效率与可靠性。为了提升调制发射脉冲信号的上升下降沿速度,提高大功率调制电路可靠性,提出一种新型带上电时序控制及过脉宽保护功能的大功率调制电路,该电路包括上电时序控制电路、过脉宽保护电路、大功率调制电路。通过对电路进行理论分析,给出详细参数并计算该电路参数,并对关键参数进行仿真及实测验证,该电路具有调制电压高,上升下降沿速度快等特点。经过测试验证,调制电压最高100V,调制频率最高可达500KHz,峰值工作电流超过20A,上升沿、下降沿小于30ns。具有广阔的应用前景。     

Space-time structure of ion-cyclotron waves in the topside ionosphere as observed onboard the <Emphasis Type="Italic">ST</Emphasis>-<Emphasis Type="Italic">5</Emphasis> satellites

Results of observations of ion-cyclotron (IC) waves onboard the ST-5 satellites in the topside ionosphere (heights from a few hundred up to thousands of km) are presented. In this project, three identical micro-satellites were located during three months in 2006 in almost identical orbits with distances between them from first thousands to hundreds of km. All ion-cyclotron wave packets detected by two-three probes were observed at crossing one and the same latitude, which manifests their narrow localization in latitude with a characteristic scale from the first tens to 100 km. In no event IC waves were recorded with comparable amplitudes by all three satellites. At the same time, in the case of ST-5 flight near the ground-based induction magnetometer, a long emission in the same frequency range on the ground corresponded to a burst of IC waves in the topside ionosphere. This can indicate to the fact that an IC instability develops not continuously, but in the pulsing regime with a characteristic time of up to ∼10 min. A change in the rotation direction when a satellite crosses the wave structure is a characteristic feature of the polarization structure of registered transverse waves. The detected effects are discussed from the point of view of the existing models of generation and waveguide propagation of IC waves.     

Delayed gratification habitable zones: when deep outer solar system regions become balmy during post-main sequence stellar evolution

Like all low- and moderate-mass stars, the Sun will burn as a red giant during its later evolution, generating of solar luminosities for some tens of millions of years. During this post-main sequence phase, the habitable (i.e., liquid water) thermal zone of our Solar System will lie in the region where Triton, Pluto-Charon, and Kuiper Belt objects orbit. Compared with the 1 AU habitable zone where Earth resides, this "delayed gratification habitable zone" (DGHZ) will enjoy a far less biologically hazardous environment - with lower harmful radiation levels from the Sun, and a far less destructive collisional environment. Objects like Triton, Pluto-Charon, and Kuiper Belt objects, which are known to be rich in both water and organics, will then become possible sites for biochemical and perhaps even biological evolution. The Kuiper Belt, with >10(5) objects > or =50 km in radius and more than three times the combined surface area of the four terrestrial planets, provides numerous sites for possible evolution once the Sun's DGHZ reaches it. The Sun's DGHZ might be thought to only be of academic interest owing to its great separation from us in time. However, approximately 10(9) Milky Way stars burn as luminous red giants today. Thus, if icy-organic objects are common in the 20-50 AU zones of these stars, as they are in our Solar System (and as inferred in numerous main sequence stellar disk systems), then DGHZs may form a niche type of habitable zone that is likely to be numerically common in the Galaxy.     

State transition matrix approximation with geometry preservation for general perturbed orbits

This paper presents a method for approximating the state transition matrix for orbits around a primary body and subject to arbitrary perturbations. The primary objective of this method is to provide an accurate state transition matrix for orbits with realistic perturbations, which has a sufficiently simple form for implementation onboard spacecraft. The averaging method is employed to isolate the high and low frequency spectra of the perturbation terms, and construct a functional form of the approximate state transition matrix composed only of elementary analytic functions. In addition to the methodology of the approximation, it is shown that the symplectic property, which is a fundamental mathematical structure of Hamiltonian systems, can be incorporated into this method. This not only reduces the number of parameters required for approximations but also makes it possible to preserve the physically true structure of the state transition matrix. The resulting state transition matrix approximation is valid for tens of orbital revolutions without having to update the parameters. Numerical simulations show that this method is valid for arbitrary eccentricity orbits with semimajor axis ranging from LEO up to around 10 Earth radii when applied to Earth orbits.     

重复频率脉冲激光辐照下光学薄膜元件 温升的有限元分析

文章采用有限元ANSYS程序分析了在重复频率脉冲激光辐照下光学薄膜元件表面的温度变化。结果表明激光脉宽相同时,重复频率越高,相同辐照时间薄膜元件表面温度累积就越大;占空比一样时,脉宽越大,相同辐照时间元件温升越高。重复频率表现出来的只是温度的累积效果,脉宽的影响效果远大于重复频率引起的温度累积。     

Atomic oxygen simulation and analysis

A technique has been developed for creating in the laboratory suprathermal, neutral atomic beams by means of grazing-incidence collisions between ion beams and metal surfaces. Residual ions are deflected by applied electric fields. The resulting neutral beams are pure, well-focused and mono-energetic. Energies from a few eV to tens of keV are obtainable. The technique permits the beams to be used in conjunction with electron and photon irradiation for studies of synergistic effects. Of particular interest is the creation of a low-energy, neutral, atomic-oxygen beam, which is of importance to space-related research.     

嫦娥一号卫星的初步科学成果与嫦娥二号卫星的使命

嫦娥一号卫星于2007年10月24日在西昌卫星发射中心成功发射,2009年3月1日受控落月,在轨运行495d,一共取得了1.37Tbyte的原始科学探测数据,在此基础上生产出4Tbyte科学应用数据产品。通过对这些科学探测数据的初步分析和应用研究,已经获得了包括＂我国首次月球探测工程全月球影像图＂等在内的一系列科学成果,圆满实现了预期的各项科学目标,为推动我国月球与行星科学的研究和后续月球探测工程的开展奠定了重要基础。嫦娥二号卫星在嫦娥一号卫星取得圆满成功之后,进行了一系列技术改进,作为探月二期工程的先导星,将于今年年底前发射升空。嫦娥二号卫星从发射到第一次近月制动所经历的时间由13d缩短为5d,环月轨道高度由200km降低为100km,CCD相机的像元分辨率由120m提高到10m,激光高度计测量月面高程由1次/s提高到5次/s。嫦娥二号卫星将重点开展对月面着陆区地形地貌的精细探测,试验验证相关关键技术,为探月二期月面软着陆奠定科学和技术基础。     

一箭多星发射卫星空间距离测量与预报技术

多星空间距离测量是一箭多星发射的一项重要任务。由于站点分布限制和轨道条件约束,国内多数卫星存在地面不可监测弧段,传统的地基测定轨方法无法满足全弧段连续性要求。针对上述问题,对星间距离测量技术进行了研究,提出了利用GPS进行星间距离测量的方法;并提出利用基于GPS数据的简化动力学模型法及多项式拟合法进行星间距离测量和预报,结果显示,预报10min的位置精度为数十米量级。该方法突破了地基测控可见区的限制,实现了全弧段的轨道确定,并规避了GPS接收机可能存在的短时中断或由于通信原因不能实时获得测量结果的风险;可为分析确定多颗卫星间的安全距离提供参考。     

基于全脉冲的周期信号样本提取技术

现代电子战中,传统的辐射源分选识别方法无法在密集的信号环境中快速有效地对复杂体制雷达进行分选识别,造成系统漏警。基于上述情况,提出了一种基于脉冲样本序列自提取的分选算法。这种算法利用雷达信号脉冲序列的周期性和相关性,实现对模板序列的自动提取,从而可实现全脉冲序列中小样本数或脉间规律复杂的雷达信号的分选。仿真实验表明,在全脉冲数据量级适中的情况下,该算法可以有效提取目标模板序列。     

一种超宽带脉冲信号发生器的设计

介绍超宽带(UWB)技术,利用阶越恢复二极管(SRD)产生超宽带窄脉冲信号的微带结构电路,获得了纳秒级的超短、快速前沿的1ns单极性UWB脉冲。分析讨论电路原理与设计方法,实测结果显示该电路产生的脉冲信号具有良好的波形,并且脉冲拖尾的震荡起伏很小,适用于超宽带无线通信的窄脉冲信号形成电路。     

CARS燃烧诊断系统的时序控制器研究

研制了一台用于相干反斯托克思喇曼光谱CARS（Coher-ent Anti-Stokes Raman Scattering）相干反射系统的时序控制器，使激光发射同步输出脉冲与数采系统中LCI外触发输入脉冲电平匹配；可以选择采集同步发射的激光信号。其有单选、奇数、偶数、全选四种工作模式，可应用于单脉冲CARS实验，实现时间分辨光谱，同时还可以降低噪音，提高信噪比。     

激光驱动接力移除空间碎片的小卫星星座及可行性研究

在众多空间碎片移除技术中,天基激光烧蚀驱动是一种高效的、有广阔应用前景的移除技术,特别是针对移除海量的、尺寸在1~10 cm的危险碎片而言,更是具有独特优势。然而,这一技术对高能激光器单脉冲能量、光束质量、发射镜口径等要求很高,目前的硬件水平还达不到实用指标要求,制约了其天基应用。为了克服这些硬件技术障碍,本文另辟蹊径,利用小卫星概念,提出了由不同轨道高度小卫星平台组成小卫星星座,通过在每个小卫星平台上的激光驱动接力来逐步降低碎片轨道高度,最终达到移除空间碎片的小卫星接力移除星座的构想。基于现有的激光器性能参数,根据激光烧蚀驱动碎片动力学模型计算了单个卫星平台的移除能力,结果显示,10 J单脉冲能量激光器和0.5 m直径发射镜,能够对20 km范围内、尺寸小于10 cm碎片进行有效驱动。进而,针对空间碎片密集度高而应用最广的800 km轨道高度区域,设计了由分布在不同轨道高度的30颗小卫星组成接力驱动移除星座系统方案,通过仿真模拟计算验证了星座系统的移除碎片的可行性。该研究利用目前热门的小卫星星座,降低了天基激光移除空间碎片技术对硬件的性能要求,为该技术的应用提供了新的思路和途径,所提出的小卫星接力驱动星座系统方案也有工程参考价值。     

一种估计线性调频信号参数的方法

合成孔径雷达实际发射的脉冲信号并非标准的线性调频信号 ,而是带有高次相位误差的调频信号。在高次相位误差较大的情况下 ,将对成像质量产生影响。因此 ,必须对发射信号的线性调频项和高次相位误差进行测试。文中提出利用一维相位解缠和多项式拟合测试发射脉冲信号参数的方法 ,仿真结果表明 ,具有较高的估计精度和较好的实用性     

Low-gravity environment in Spacelab

This paper presents residual and system-generated accelerations with results from g-jitter spectral measurements in the Spacelab Engineering Model. An overview (classification, brief discussion, and assessment of magnitudes) of the various constituents of the perturbative acceleration field inside the Spacelab Module is presented, both steady and fluctuating components being considered. Results of local g-jitter spectral measurements taken in the Spacelab Engineering Model (EM-1)/Long Module Configuration are presented for frequencies from less than 1 to 200 Hz. The measured results for the system-generated perturbative accelerations exhibit, in the time domain, amplitudes of the order of 10(-3) g (peak value 3.6 x 10(-3) g). Spectral values of 4 x 10(-4) g are obtained in the frequency range up to 100 Hz; up to 10 Hz, however, the spectral values remain about an order of magnitude smaller, and also between 100 and 200 Hz the perturbation level is significantly lower than below 100 Hz. Measured results from simulated crew activities show, in the time domain, a peak amplitude of 2.6 x 10(-2)g, the spectral values being 6 x 10(-3)g below 100 Hz and 1 x 10(-3)g below 10 Hz for typical perturbances.     

Orientation of Sharp Fronts of the Solar Wind Plasma

Based on simultaneous observations performed by several spacecraft, we evaluate the orientation of sharp (with a duration of a few minutes) and large (tens and hundreds percent of the mean value) fronts of the solar wind plasma (changes in the ion flux and ram pressure). The orientation of the fronts is determined with respect to the Sun–Earth line and to two planes in space for several tens of the largest (in amplitude) changes of the ion flux. A considerable fraction of these fronts (about 50%) has an inclination to the plane perpendicular to the Sun–Earth line that exceeds 30°.