湿热对PI/ MoS2 涂层性能的影响

对钛合金表面的PI/Mo S2涂层进行了湿热老化试验,在70℃、98%RH条件下存储长达27 d。采用衰减全反射红外光谱和透射红外光谱分别对涂层表面及涂层进行分析测试,利用X射线光电子能谱对涂层表面成分进行分析。通过球盘摩擦试验机考察了湿热老化对润滑涂层的真空及大气摩擦性能的影响。采用拉脱法测试了湿热老化前后涂层附着力。结果表明,湿热会导致PI/Mo S2润滑涂层表面的胶黏剂聚酰亚胺被水解侵蚀,膜层表面深度在50 nm以内的部分Mo S2被氧化。湿热试验前后涂层的真空耐磨寿命降低13%,大气耐磨寿命降低16%;真空摩擦因数略有增加且波动增大,而大气摩擦因数显著增加,涂层附着强度也略显降低。     

控制力矩陀螺磁悬浮转子的指数趋近积分滑模控制研究

针对微重力、动框架等多源扰动下磁悬浮控制力矩陀螺磁轴承转子系统的强非线性、参数摄动及未建模动态等问题,开展控制力矩陀螺的磁轴承转子鲁棒控制研究。建立了磁轴承转子轴向通道动力学模型与电磁力工作点线性化模型,分析了系统参数摄动及未建模动态,并在此基础上提出了一种非线性系统指数趋近积分滑模控制方法,设计了含有电流及位移的积分滑模平面,采用指数趋近律与饱和函数抑制抖振实现到达阶段滑模控制律。实验结果表明：采用该方法可有效抑制滑模的抖振现象,参数摄动时系统具有较佳动态性能,同时在转子转动、框架工作时保证系统良好鲁棒性。     

二元包覆的AP吸湿性及热分解性能研究

AP易吸潮结块而影响其使用性能,需对其进行疏水处理,降低其吸湿性。采用氧化石墨烯( GO)对AP进行一元包覆制备出AP/GO复合物,用氟硅烷( FAS：十二氟庚基丙基三甲氧基硅烷)对AP进行二元包覆制备出AP/GO/FAS复合物。吸湿率测试结果表明,在20℃、相对湿度为85%的条件下,AP粒径越大,吸湿率越小。对AP进行二元包覆后的复合物吸湿率均小于纯AP和一元包覆后的AP复合物的吸湿率,且GO质量分数为0.4%,FAS质量分数为1%时,二元包覆AP后的复合物的吸湿率最小。通过热分析测试结果可知,GO质量分数为0.4%、FAS质量分数为1%的AP/GO/FAS复合物的高温放热分解峰比纯AP提前了约32.9℃。     

沉积温度对CVD-SiC涂层显微结构的影响

介绍了采用化学气相沉积（CVD）方法在C/SiC复合材料表面制备SiC抗氧化涂层的情况.对不同工艺条件下制备出的SiC涂层,使用SEM,EDS和XRD分析了沉积层的物相和显微结构.结果表明：SiC涂层生长速度随沉积温度升高而升高,晶粒尺寸也随之增大;在较高沉积温度下,可以产生较大的沉积速度,但SiC涂层表面粗糙度将会增大.     

电磁监测试验卫星矢量磁场探测方法

电磁监测试验卫星是中国第一颗近地轨道电磁场科学探测试验卫星, 探测空间背景磁场是其重要任务之一. 空间背景磁场探测需要在卫星平台上对空间矢量磁场进行长期稳定准确探测, 电磁监测试验卫星采用磁通门磁强计和基于CPT效应的绝对磁场校准装置(Coupled Dark State Magnetometer, CDSM)分别探测空间相对矢量磁场以及绝对标量磁场, 通过数据处理, 使最终的矢量磁场探测数据具有准确性. 这种数据处理方法在理想模型下拥有解析解, 实施过程中载荷的噪声、 准确度及稳定性影响模型的准确性, 会产生数据校准误差. 通过对在轨磁场探测的模拟确定了这种数据处理方法的性能, 验证了在载荷设计性能的基础上电磁监测试验卫星的磁场探测可以实现1 nT的准确度.      

A hybrid attitude controller consisting of electromagnetic torque rods and an active fluid ring

In this paper, a novel hybrid actuation system for satellite attitude stabilization is proposed along with its feasibility analysis. The system considered consists of two magnetic torque rods and one fluid ring to produce the control torque required in the direction in which magnetic torque rods cannot produce torque. A mathematical model of the system dynamics is derived first. Then a controller is developed to stabilize the attitude angles of a satellite equipped with the abovementioned set of actuators. The effect of failure of the fluid ring or a magnetic torque rod is examined as well. It is noted that the case of failure of the magnetic torque rod whose torque is along the pitch axis is the most critical, since the coupling between the roll or yaw motion and the pitch motion is quite weak. The simulation results show that the control system proposed is quite fault tolerant.     

New one-axis one-sensor magnetic attitude control theoretical and in-flight performance

New one-axis magnetic attitude control is proposed. Only one attitude sensor providing any inertial direction measurements is necessary, magnetometer is not used. The control may be used as a backup capability in case main actuators or some attitude sensors fail. Sun pointing is achievable using only three-axis Sun sensor, so the control may be used to lower the power consumption during battery charging. Asymptotic stability of different equilibria depending on the satellite inertia tensor is summarized. In-flight results from “Chibis-M” microsatellite are provided proving general control performance.     

On the large-scale structure of the tail current as measured by THEMIS

The magnetic field structure and the spatial characteristics of the large-scale currents in the magnetospheric tail were studied during quiet and moderately disturbed geomagnetic conditions in 2009. The magnetic field of the currents other than the tail current was calculated in terms of a paraboloid model of the Earth’s magnetosphere, A2000, and was subtracted from measurements. It was found on the base of obtained tail current magnetic field radial distribution that the inner edge of the tail current sheet is located in the night side magnetosphere, at distances of about 10 R_E and of about 7 R_E during quiet and disturbed periods respectively. During the disturbance of February 14, 2009 (Dst_min ∼ −35 nT), the B_x and the B_z component of the tail current magnetic field near its inner edge were about 60 nT, and −60 nT that means that strong cross-tail current have been developed. The tail current parameters at different time moments during February 14, 2009 have been estimated. Solar wind conditions during this event were consistent with those during moderate magnetic storms with minimum Dst of about −100 nT. However, the magnetospheric current systems (magnetopause and cross-tail currents) were located at larger geocentric distances than typical during the 2009 extremely quiet epoch and did not provide the expected Dst magnitude. Very small disturbance on the Earth’s surface was detected consistent with an “inflated” magnetosphere.     

Analytical-HZETRN model for rapid assessment of active magnetic radiation shielding

The use of active radiation shielding designs has the potential to reduce the radiation exposure received by astronauts on deep-space missions at a significantly lower mass penalty than designs utilizing only passive shielding. Unfortunately, the determination of the radiation exposure inside these shielded environments often involves lengthy and computationally intensive Monte Carlo analysis. In order to evaluate the large trade space of design parameters associated with a magnetic radiation shield design, an analytical model was developed for the determination of flux inside a solenoid magnetic field due to the Galactic Cosmic Radiation (GCR) radiation environment. This analytical model was then coupled with NASA’s radiation transport code, HZETRN, to account for the effects of passive/structural shielding mass. The resulting model can rapidly obtain results for a given configuration and can therefore be used to analyze an entire trade space of potential variables in less time than is required for even a single Monte Carlo run. Analyzing this trade space for a solenoid magnetic shield design indicates that active shield bending powers greater than ∼15 Tm and passive/structural shielding thicknesses greater than 40 g/cm² have a limited impact on reducing dose equivalent values. Also, it is shown that higher magnetic field strengths are more effective than thicker magnetic fields at reducing dose equivalent.     

On the universality of asymptotic limits in the theory of field line diffusion and perpendicular transport of energetic particles

We discuss the random walk of magnetic field lines in astrophysical plasmas. Based on the standard theory of field line diffusion we show that there are two asymptotic limits. In these limits field line wandering is universal because in both regimes the field line diffusion coefficient depends only on fundamental length scales and absolute magnetic field strengths. As examples we discuss the field line diffusion coefficient for different prominent turbulence models namely the slab model, the two-dimensional model, and the Goldreich–Sridhar model. We show that the field line diffusion coefficient for the latter model agrees with the results obtained for slab and two-dimensional turbulence in limiting cases. We also discuss the transport of energetic particles perpendicular with respect to the mean magnetic field. Based on the unified nonlinear transport theory we consider again asymptotic limits. It is shown that one can identify four different regimes in which the transport is again universal. In all four cases perpendicular transport only depends on fundamental length scales of turbulence, magnetic field values, and the parallel diffusion coefficient.