纳秒级大功率脉冲激光二极管驱动设计

脉冲式激光雷达探测性能与激光光源发出的光脉冲有关,而 LD 驱动电路性能好坏直接决定了光脉冲的优劣.基于激光测距仪系统要求,文章选用超快速场效应管作为开关器件,建立驱动电路模型,对驱动电路设计与分析,经过多次试验,成功设计出最小脉宽为5．6ns,上升沿为2．2ns,峰值电流可达12A的脉冲电路.其中脉宽脉宽为16ns,上升沿为3ns,重频达到50KHz,驱动 LD峰值功率将近60W,成功用于激光雷达强激光光源发射部分.同时分析了影响电路的主要因素.     

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。     

微空心阴极放电机理及其在电热式推力器中的应用

近年来,微空心阴极放电（MHCD）技术的发展为研制适用于小卫星的先进新型微推力 器提供了可能。MHCD是微放电领域中一种新颖的非平衡高气压辉光放电,其优点是可以在高 气压下稳定放电,并且只需要非常低的电压（几百伏特）或者输入功率（百毫瓦数量级）。 本文针对MHCD,实验研究了微放电的电流-电压特性,并利用光学发射光谱的方法测量了微 等离子体中电子数密度和中性气体温度。结果表明,在稳定的辉光放电下,MHCD孔内的电子 数密度和中性气体温度随着压强和放电电流的增加而增大,电子数密度可达
10 14 cm -3 ,中性气体温度可达1000K。由此可以推断,微空心阴极放电较小 的尺寸结构与强烈并可控的气体加热相结合,完全可以开发应用在新型的电热式等离子体推 进上,研制成微空心阴极放电等离子体推力器。由于在微放电等离子体中加热了工质气体, 因此其性能可大大高于冷气推进。     

国外电推进系统空心阴极技术

介绍了国外离子和霍尔电推进系统空心阴极技术的现状.根据空心阴极的常规设计,分析了发射体源材料耗尽,发射体有效发射表面被难挥发沉积物覆盖,源材料活性分子不能到达发射体表面,触持极、顶板、加热器因溅射腐蚀损坏,加热器损坏,以及发射体化学中毒等影响空心阴极长寿命的因素.讨论了一体化阴极、小电流高效钡钨阴极、大电流钡钨阴极、LaB6阴极、L式储备阴极和Bi阴极等新技术.     

光控相控阵天线

研究了迅猛发展的新的相控阵理论和技术厦其前景，其中涉及控制相控阵天线的光纤和光电技术。在相控阵天线中光学图像形成和扫描保证实时（PMB）形成一维或二维、连续或色散的单波束或多波束方向图（RH），并且保证对不同辐射频率的最大方向图的方向进行无波动扫描。采用光学图像形成电路（Roc）的相控阵天线，在超宽瞬时通带（～1GHz）中既能以连续方式也能以超短脉冲（脉宽～1ps）方式工作于发射状态和接收状态。     

小卫星高分辨率成像系统

对小卫星对地观测高分辨率成像系统进行了综述。介绍了国内外有极高分辨率（0．5～1．0m）、高分辨率（1．8～2．5m）和中高分辨率（4-10m）小卫星光学成像系统的性能,并与合成孔径雷达（SAR）成像系统进行了比较。给出了小卫星光学成像系统、SAR高分辨率成像系统和卫星平台的关键技术。讨论了未来小卫星及其高分辨率成像系统技术的发展趋势。     

小型化电子回旋谐振微波离子推进器研究

常规的电推进技术是针对大卫星应用而研制的，体积大、功耗高，不能满足小卫星飞速发展的实际需要。针对小卫星对电推进器的要求，提出了利用电子回旋谐振微波放电技术，采用微波同轴放电腔体的小型化离子推进器。由于同轴传输线不存在截止波长，放电腔体的直径选择非常灵活，可以适应小卫星的低供电能力和对体积重量的要求。实验样机的直径为50mm，在微波功率为30W，加速电压1．2kV，减速电压0．2kV的条件下，等离子体的电子密度达到了4．6×10^16／m^3，推进器的离子束流也达到6mA。实验样机的体积大大低于常规波导谐振腔微波离子推进器，实现了小型化，基本满足了小卫星对电推进器的体积重量要求。     

低压低功率SiGe BiCMOS X波段低噪声放大器与IEEE 802．11a LNA的设计比较研究

介绍了一种采用0．25um SiGe BiCMOS工艺集成的低压低功率X波段低噪声放大器（LNA），比较了此种放大器与IEEE 802．11a LNA的设计。X波段LNA和IEEE 802．11a LNA的工作频率分别为10GHz和5．8GHz。所设计的LNA都采用了相同的结构和电压，并耗费同量的电流。两种LNA都只需要1．5V的电压，消耗1．5mW的直流功率。两种电路的差异是它们有不同的输入与输出匹配和负载。本文介绍的LNA在10GHz时的电压增益为11．49dB，噪声系数（NF）为3．84dB，输入反射损失为-15.37dB，输出反射损失为-17dB，P1dB为-3．75dBm。在5．8GHz时的电压增益为16．07dB，噪声系数为3．07dB，输入反射损失为-18．1dB，输出反射损失为-15．23dB，P1dB为-6．54dBm。两电路的关键特征是：低压、低功率和良好的噪声匹配。频率为IOGHz和5．8GHz时，噪声系数与最小噪声系数之差分别只有0．03dB和0．05dB。验证了一种高频（X波段）低成本设计，与其他技术（如GaAs、SiBJT、JFET、PHMET和MESFET等）相比，它是在SiGe BiCMOS中设计的。     

L波段高效小尺寸功率放大器载片设计

为了应对当前市场对功率器件更低成本、更小尺寸和更优性能的要求，设计了一款工作频率为1.2～1.4GHz的高效率小尺寸氮化镓（gallium nitride,GaN）基功率放大器载片。使用有源时域负载牵引系统对GaN管芯进行在片测试并提取管芯的非线性行为模型，在先进设计系统（advanced design system,ADS）软件中利用模型进行阻抗匹配电路设计和仿真，将功率放大器端口匹配到了目标阻抗50Ω。该载片采用谐波控制技术使功率放大器附加效率提高了6%～8%，采用高介电常数的陶瓷材料将载片电路集成在8mm×8mm。实测结果显示，放大器在漏源电压28V、100us脉宽和10%占空比脉冲输入的工作条件下，在小尺寸的载体上实现了输出功率大于56W，功率附加效率大于78%的高效率指标。     

电火箭空心阴极发射体寿命研究

分析了影响电火箭空心阴极发射体寿命的各种因素。论述了空心阴极放电时，其内部化学反应生成物的迁移、扩散、蒸发和溅射。讨论了发射体发射材料的损耗速率与温度的关系，指出知度降低发射体的工作温度是延长空心阴极寿命的有效措施，还讨论了工质气体纯度和真空环境对发射体寿命的影响。     

PLZT光致伸缩层合梁的非接触形状控制

以光电层合梁非接触形状控制问题为研究对象,阐述了PLZT光致伸缩驱动器的工作机理,建立了光-电-力-热耦合情况下的光电有限元模型,通过引入加强假定应变模式和假定自然应变法改善了单元的性能。在此基础上,以光致伸缩驱动器所受到的光强大小为设计变量,以光电层合梁的期望形状与控制形状的差值函数为目标函数,应用有限元法和遗传算法建立了求解基于PLZT光致伸缩驱动器层合梁非接触形状控制问题的一般方法。数值模拟的结果验证了该方法有效,表明该方法能够很好地实现光电层合梁结构的非接触形状控制。     

Field emission performance of multiwalled carbon nanotubes for a low-power spacecraft neutraliser

Field electron emission from aligned multiwalled carbon nanotubes has been assessed to determine if the performance, defined by power consumption, lifetime and emission current, is suitable for use in spacecraft charge neutralisation for field emission electric propulsion (FEEP). Carbon nanotubes grown by chemical vapour deposition (CVD) were mounted on a dual in line chip with a macroscopic (nickel mesh) extractor electrode mounted ～1 mm above the tubes. The nanotubes’ field emission characteristics (emission currents, electron losses and operating voltage) were measured at ～10^?4 Pa. An endurance test of one sample, running at a software-controlled constant emission current lasted >1400 h, approaching the longest known FEEP thruster lifetime. The emission corresponds to a current density of ～10 mA/cm² at a voltage of 150 V. These results, implementing mature extractor-electrode geometry, indicate that carbon nanotubes have considerable potential for development as robust, low-power, long-lived electron emitters for use in space.     

平流层飞艇的能源技术和平衡分析

平流层飞艇作为近空间对地观测平台的一种实现方案，主要依靠自身庞大体积产生的静浮力而不像其它飞行器依靠相对空气运动产生升力，所以飞艇能够以较慢的速度飞行甚至能够在空中长期保持定点悬停即相对地面静止。具有长时间在平流层自主飞行的能力，是平流层飞艇设计的一个重要目标。文章对平流层飞艇能源系统的构成、部件及能源平衡分析方法作了介绍。     

Countermeasure of the negative effects of weightlessness on physical systems in long-term space flights

The system of countermcasure of microgravity effects has been developed in Russia that allowed to perform safely long-term space flights. This system that includes different means and methods such as special regimens of physical exercises, axial loading (“Pingiun”) and antigravity suits, low body negative pressure device (LBNP, “Chibis”) and “cuffs” and others has been used with certain variations at certain stages of flight in 27 successfully accomplished space flights that lasted from 60 to 439 days. The pre-, in- and postflight studies performed in 57 crew members of these flights have shown that the system of countermeasure is effective in preventing or diminishing to a great extent almost all the negative effects of weightlessness in flights of a year and more duration and that the intensity and duration of changes recorded in different body systems after flights do not correlate significantly to flight durations, correlating strongly to the volume and intensity of physical exercises used during flight and especially during concluding stage of it.     

钛掺杂氧化镁薄膜二次电子发射倍增特性研究

氧化镁具有较高的二次电子发射系数，适合作为制备多级放大装置的二次电子发射材料。文章采用磁控溅射法制备高质量氧化镁薄膜和钛掺杂氧化镁薄膜，并对薄膜进行形貌表征，研究其二次电子发射倍增特性，包括氧化镁薄膜电子倍增器的增益特性以及增益衰减情况。结果表明:高压源电压和电流的增大均可提高电子倍增器的电流增益倍数；掺杂Ti不仅能提高电子倍增器的增益效能，且相比纯氧化镁薄膜，钛掺杂氧化镁薄膜的增益衰减明显放缓，能够将倍增器的寿命延长2倍以上。     

带有控制增益自校正的甚低轨道卫星自主轨道维持方法

为实现甚低轨道的长期稳定运行,分析了甚低轨道的摄动特性,设计了一种带有轨控增益校正的自主轨道维持方法。该方法可通过前一次轨控的结果对轨控增益进行校正,提高轨控算法对卫星质量、推力大小等不确定因素的鲁棒性,逐渐提高轨道控制的精度。对轨道控制的频率、每次轨控的时间长度及对偏心率的影响进行了分析,仿真结果表明:自主轨道维持方法能实现甚低轨道高度维持控制,在参数不确定的情况下,与传统算法相比可大幅提高轨道控制的精度,确保平均偏心率矢量收敛,满足甚低轨道卫星的长寿命要求。所设计的算法结构简单,运算量小,可由目前的星载计算机实现。     

Investigation of oxygen O2(a1Δg) emission on the nightside of Venus: Nadir data of the VIRTIS-M experiment of the Venus Express mission

The paper is devoted to studies of the oxygen 1.27 μm emission on the Venus nightside using nadir measurements with the imaging spectrometer VIRTIS. A map of the emission distribution in coordinates latitude-local time is drawn for the southern hemisphere, equatorial region, and low latitudes of the northern hemisphere on the basis of observations in the period from June 2006 to January 2008 (more than 600 runs). As it has been noted before, strong spatial and time variations of the emission were observed. Two maxima of the emission are found: the first one (expected) is observed near the antisolar point, and the second one (near 23:00 LT) is seen at latitudes of 30°–60° in the southern hemisphere. The average value of the emission intensity measured according to the nadir data is 1.0 ± 0.4 MR. The emission with the intensity exceeding the average one by a factor of 2–3 was detected at different times almost over the entire nightside of the southern hemisphere.     

Comparison of the effects induced by the ordinary (O-mode) and extraordinary (X-mode) polarized powerful HF radio waves in the high-latitude ionospheric <Emphasis Type="Italic">F</Emphasis> region

Using the results of coordinated experiments on the modification of the high-latitude ionosphere by powerful HF radio emission of the EISCAT/Heating facility, effects of the impact of powerful HF radio waves of the ordinary (O-mode) and extraordinary (Х-mode) polarization on the high-latitude ionospheric F region have been compared. During the experiments, a powerful HF radio wave was emitted in the magnetic zenith direction at frequencies within the 4.5–7.9 MHz range. The effective power of the emission was 150–650 MW. The behavior and characteristics of small-scale artificial ionospheric irregularities (SAIIs) during O- and X-heating at low and high frequencies are considered in detail. A principal difference has been found in the development of the Langmuir and ion–acoustic turbulence (intensified by the heating of the plasma and ion–acoustic lines in the spectrum of the EISCAT radar of incoherent scatter of radio waves) in the О- and Х-heating cycles after switching on the heating facility. It has been shown that, under the influence on the ionospheric plasma of a powerful HF radio wave of the Х-polarization, intense spectral components in the spectrum of the narrow-band artificial ionospheric radio emission (ARI) were registered at distances on the order of 1200 km from the heating facility.     

Search for the OH (X(2)Pi) Meinel band emission in meteors as a tracer of mineral water in comets: detection of N(2)(+) (A-X)

We report the discovery of the N(2)(+) A-X Meinel band in the 780-840 nm meteor emission from two Leonid meteoroids that were ejected less than 1000 years ago by comet 55P/Tempel-Tuttle. Our analysis indicates that the N(2)(+) molecule is at least an order of magnitude less abundant than expected, possibly as a result of charge transfer reactions with meteoric metal atoms. This new band was found while searching for rovibrational transitions in the X(2)Pi electronic ground state of OH (the OH Meinel band), a potential tracer of water bound to minerals in cometary matter. The electronic A-X transition of OH has been identified in other Leonid meteors. We did not detect this OH Meinel band, which implies that the excited A state is not populated by thermal excitation but by a mechanism that directly produces OH in low vibrational levels of the excited A(2)Sigma state. Ultraviolet dissociation of atmospheric or meteoric water vapor is such a mechanism, as is the possible combustion of meteoric organics.     

Superconducting magnets and mission strategies for protection from ionizing radiation in interplanetary manned missions and interplanetary habitats

First order evaluations for active shielding based on superconducting magnetic lenses were made in the past in ESA supported studies. The present increasing interest of permanent space complexes, to be considered in the far future as ‘bases’ rather than ‘stations’, located in ‘deep’ space (as it has been proposed for the L1 libration’s point between Earth and Moon, or for Stations in orbit around Mars), requires that this preliminary activity continues, envisaging the problem of the protection from cosmic ray (CR) action at a scale allowing long permanence in ‘deep’ space, not only for a relatively small number of dedicated astronauts but also to citizens conducting there ‘normal’ activities.Part of the personnel of such a ‘deep space base’ should stay and work there for a long period of time. It is proposed that the activities and life of these personnel will be concentrated in a sector protected from Galactic CR (GCR) during the whole duration of their mission. In the exceptional case of an intense flux of Solar Energetic Protons (SEP), this sector could be of use as a shelter for all the other personnel normally located in other sectors of the Space Base.The realization of the magnetic protection of the long permanence sector by well-established current materials and techniques is in principle possible, but not workable in practice for the huge required mass of the superconductor, the too low operating temperature (10–15 K) and the corresponding required cooling power and thermal shielding.However the fast progress in the production of reliable High Temperature Superconducting (HTS) or MgB₂ cables and of cryocoolers suitable for space operation opens the perspective of practicable solutions. In fact these cables, when used at relatively low temperature, but in any case higher than for NbTi and Nb₃Sn, show a thermodynamically much better behavior. Quantitative evaluations for the protection of the sector of the ‘Space Base’ to be protected from GCRs (and therefore from SEPs also) are presented.For possible large outer radius solutions it must in the meantime solve the problem of the assembling or deploying in space the conductors for returning the electric current.