10cm氙离子推力器变推力特性研究

非重力阻尼的连续、快速、高精度补偿是实现重力梯度测量卫星精细重力场测量的关键技术之一,直接影响到整星工程任务的成败。针对重力梯度测量卫星在轨飞行期间对电推进系统宽范围连续变推力能力的应用需求,分析了10cm氙离子推力器推力调节响应特性。在此基础上,通过对阳极电流、励磁电流和阳极流率等推力高敏感响应参量的组合调节,开展了推力调节试验研究,验证了10cm氙离子推力器宽范围连续变推力调节能力,获得了1～20mN范围内的推力调节性能及其变化规律。试验结果表明：在采用地面供电、供气设备条件下,10cm氙离子推力器能够在100～597W的功率范围内实现0.98～20.29mN的推力宽范围调节,比冲175～3500s,推力分辨率优于50μN。研究为建立10cm氙离子电推进系统的推力控制数学模型及调节控制算法奠定基础。     

热控涂层电子辐照效应

研究防静电Kapton二次表面镜(ITO/Kapton/Al)、S781白漆两种典型热控涂层,在不同能量电子辐照后太阳吸收比退化情况,并利用X射线光电子能谱和扫描电子显微镜对样品表面的成分和形貌进行了分析。结果表明:相同电子注量下,不同能量电子对样品的太阳吸收比退化作用程度是有区别的。而样品光谱反射率、表面形貌、表面成分的损伤效应类似,说明不同能量电子辐照下,样品的退化机理是一致的。     

基于SOC的ACAS无线电高度信号激励测试的设计

本文介绍了一种以SOC为核心芯片用于机载防撞系统(ACAS)中符合ARINC552A标准无线电高度信号激励测试的软硬件设计方法.采用C8051F020型SOC芯片及OPA552等芯片搭建仿真电路,利用PDIUSBD12接口芯片建立与工控机的通讯,依据ARINC552A标准,用C51编写仿真控制程序,将仿真的ACAS无线...     

Zn含量对Mg-10Gd-4.8Y-0.6Zr合金组织和力学性能的影响

采用显微硬度和力学性能测试及金相显微镜、扫描电镜、透射电镜、X射线衍射等分析手段,研究了Zn含量对Mg-10Gd-4.8Y-0.6Zr合金挤压以及时效处理后合金组织和力学性能的影响。结果表明,在Mg-10Gd-4.8Y-0.6Zr合金中添加Zn元素,有利于细化合金晶粒,提高挤压态的强度。未添加Zn的合金T5态晶粒尺寸约为25μm,添加1%(质量分数,下同)Zn后,晶粒尺寸约为15μm,Zn含量为3%时,晶粒尺寸约为10μm。当Zn含量为1%时,合金挤压态和时效态的抗拉强度分别为337MPa,397MPa,屈服强度分别为128MPa,148MPa,伸长率分别为10.0%,5.0%,具有较好的综合性能。     

Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole

Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.     

带有太阳电池阵的卫星电源系统在轨测试方法

根据带有太阳帆板的地球同步卫星在轨测试需求,分析了星上电源系统的组成及技术状态;并以光照区可调节母线为例。给出了卫星电源系统在轨测试方法及相应的计算公式;最后,通过工程验证了该方法的正确性。     

导航计算机应用软件快速更新方法研究

目前,大多数嵌入式开发系统的软件更新必须通过硬件仿真器来实现,不便于系统的维护.良好的可维护性是嵌入式系统性能的一个重要方面,在一定程度上决定系统能否被广泛应用.本文针对南航导航研究中心自主开发的微小型导航计算机,研究了利用串行通信的方式实现应用软件快速更新的方法,解决了程序的定位、代码传输等问题,提高了系统的可维护性,体现了方法研究的实用价值.     

PIC16F877实现CAN总线分布式数据采集系统

叙述了一种采用CAN总线通信来实现分布式数据采集的设计方法;介绍了用PIC16F877通过SPI方式直接对MCP2510进行操作,与带智能适配卡的PC机实现CAN通信,并对CAN控制器MCP2510作了分析;给出了系统结构框图与部分硬件图,以及给出了软件设计思路。该基于CAN总线的分布式数据采集系统是一种高可靠性、实时性的系统。     

F-12 纤维/RE14复合材料压力容器成型工艺研究

研究讨论了缠绕过程中几种主要工艺参数对F— 12纤维 /RE14配方Φ15 0mm压力容器复合材料性能的影响。结果表明 :采用“交替”铺层方式缠绕成型 ,含胶量控制在 30 %～ 4 0 % (质量分数 ) ,缠绕张力控制在 15 0N～ 2 0 0N ,采用GPC谱图控制固化时机 ,得到的复合材料综合性能较好 ;用优化出的工艺参数进行了Φ4 80mm压力容器试验 ,结果表明其容器特性系数PV/W值为 37.0 2km ,纤维强度转化率高达73.2 6 %。     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.