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.     

TC-1和Geotail对亚暴过程中近地等离子体片磁扰动的联合观测

以2004年9月28日02:53:20 UT的亚暴为例, 通过TC-1在磁尾约12.5 R_e 和Geotail卫星在近地磁尾等离子体片约8～9 R_e的联合观测, 研究亚暴触发过程中近地磁尾等离子体片中等离子体波动特征. 结果表明, 亚暴触发区是近地磁尾中心等离子体片中较小的一个区域, 在亚暴触发区中低混杂不稳定性在近地磁尾等离子体片中存在, 准垂直传播的低混杂波发生在亚暴触发过程中, 而亚暴触发过程中近地磁尾等离子体片外边界区内的磁场偶极化信号和扰动都非常微弱. 在亚暴触发和亚暴膨胀相过程中出现了多次具有不同特征的磁场偶极化现象.      

磁暴对赤道地区L波段电离层闪烁的影响研究

利用赤道地区Vamimo站闪烁数据, 选取两次典型大磁暴时段重点分析, 对比磁暴发生前、发生时以及发生后连续几天电离层幅度闪烁强度和发生率的变化, 引入瑞利elax-elax泰勒不稳定性(Rayleigh-Taylor, R-T不稳定性)线性增长率γ₀, 对磁暴影响闪烁的机制进行初步探讨. 结果表明, 磁暴可能触发闪烁发生, 也可能抑制闪烁发生, 这既与观测季节有关, 也与磁暴不同发展阶段的地方时有关. 触发发生于闪烁少发季节磁暴主相所在的午夜至黎明时段, 可能是磁层穿透电离层的东向电场所致; 抑制发生于闪烁多发季节磁暴恢复相所在的午夜前时段, 可能是西向电场作用的结果. 磁暴发生时的电场变化可能是抑制或触发闪烁的主导因素, 但仍需进一步分析研究.      

航空发动机叶片柔性抛光技术

 基于发动机叶片结构特点及其抛光工艺要求,为实现叶片型面及阻尼台自动化抛光,满足其型面及进排气边尺寸、粗糙度等质量要求,消除叶片型面波纹对抛光工艺的影响,对砂带柔性抛光工艺装备技术进行研究,提出基于抛光力控制的砂带柔性磨头抛光工艺方法,并对其抛光工艺过程、抛光力控制进行研究,通过对叶片自动化抛光编程及抛光轨迹路径规划技术研究,最终实现发动机叶片高效柔性抛光工艺。抛光试验结果表明,柔性自动化抛光后叶片型面尺寸精度可达±0.06 mm,粗糙度低于R_a0.4,与传统手工抛光方法相比,大大提高其抛光效率及表面质量稳定性,降低劳动强度,且减少粉尘污染。     

类芬顿反应在碳化硅光学材料研抛中的作用

本文讨论了以零价铁代替亚铁盐形成类芬顿反应(Fenton-Kind process)体系应用于碳化硅光学材料抛光过程中的反应机理,通过双转子研抛机床对SiC光学材料进行了研抛实验,验证了类芬顿反应能够有效地提高SiC材料的加工效率和加工质量。通过对比不同磨料粒度研抛液加工结果,获得了SiC材料研抛过程中化学与机械作用规律。     

一种利用剩磁标定的星光/磁测备份自主导航方法

针对空间机动平台GNSS导航系统易受干扰的缺陷,提出一种基于剩磁标定的磁测/星光备份的自主导航方案。当GNSS信号完好时,利用GNSS高精度测量信息和磁强计/星敏带剩磁干扰的联合测量信息不仅可实时估计出机动平台导航参数,同时准确标定出运行环境的剩余磁场强度;当GNSS信号受干扰中断时,在剩磁准确标定的基础上启用磁场/星光备份自主导航方案完成机动平台的导航参数实时估计。由仿真结果可知,当GNSS信号正常时该导航方案具备较高的剩磁标定精度,三轴标定误差为0.026nT,0.293nT,0.107nT;而当GNSS信号受干扰时,备份导航方案三轴位置估计误差为87.3m,172.5m,65.2m,三轴速度估计误差为0.78m/s,0.86m/s, 1.04m/s。 仿真结果表明该方案具备较强的可行性。     

Global Hybrid Simulation of Magnetic Reconnection in the Magnetosheath

A three-dimensional (3-D) global hybrid simulation is carried out for the generation and structure of magnetic reconnection in the magnetosheath due to interaction of an interplanetary Tangential Discontinuity (TD) with the bow shock and magnetosphere. Runs are performed for solar wind TDs possessing different initial half-widths. As the TD propagates through the bow shock toward the magnetopause, it is greatly narrowed by a two-step compression processes, a "shock compression' followed by a subsequent ``convective compression'. In cases with a relatively thin solar wind TD, 3-D patchy reconnection is initiated in the transmitted TD, forming magnetosheath flux ropes. Multiple components of ion particles are present in the velocity distribution in the magnetosheath merging, accompanied by ion heating. For cases with a relatively wide initial TD, a dominant single X-line appears in the subsolar magnetosheath after the transmitted TD is narrowed. A shock analysis is performed for the detailed structure of magnetic reconnection in the magnetosheath. Rotational Discontinuity (RD)/Time-Dependent Intermediate Shock (TDIS) are found to dominate the reconnection layer, which and some weak slow shocks are responsible for the ion heating and acceleration.