一种用戴维南定理分析含受控源电路的方法

本文探讨了一种用戴维南定理分析含受控漂电路的方法。指导思想是将受控源当作独立源,以便求等效电路,特别是求等效入端电阻较为方便。     

金属橡胶技术应用研究

金属橡胶作为一种先进的新型功能材料,它主要为了满足航空航天飞行器上的特殊需要,解决高低温、高压、高真空及剧烈振动等环境下的密封、减振、过滤等疑难问题。通过开展金属橡胶材料在军机密封技术和阻尼隔振技术两方面的应用研究,从根本上解决液压系统在低温条件下的活动密封泄漏问题,彻底解决因橡胶隔振器存在易腐蚀、易老化、耐高低温能力差等不足造成管路事故频发的问题。     

偏转弹头导弹动力学建模

偏转弹头控制是一种新型的导弹控制方式,精确动力学模型的建立对于导弹性能、稳定性和控制的分析是必不可少的。本文采用多体动力学建模方法中的凯恩(Kane)方法对偏转弹头导弹建立了动力学模型。首先建立合适的坐标系,选取8个变量的速率为广义速率,之后推导了弹身弹头的运动学方程,接着得到广义主动力和广义惯性力,其中将控制弹头偏转的作动力矩视为主动力矩而非理想约束考虑进广义主动力的计算中,最终得到导弹的8个标量动力学方程。推导过程显示凯恩方法比牛顿-欧拉方法推导过程更为简化。利用得到的精确动力学模型进行动态仿真,通过比较研究了采用弹头质心位于弹头偏转铰链中心假设下的简化模型对导弹动态响应的影响,结果显示,在弹头偏转较慢时简化模型会带来较大的动态响应误差。     

基于约束运动理论的航天员舱外救生中的姿态运动控制

航天员舱外救生或作业时相对母体航天器经常要进行大角度姿态机动或姿态保持,利 用欧拉四元数描述姿态无奇异性且冗余度小。然而航天员舱外调姿时通常含有一定的约束或 是沿着某种预定轨迹,而且欧拉四元数在计算过程中可能发散。基于Udwadia和Kalaba 提出的约束运动理论,分析了航天员和航天器的相对姿态的描述方法,直接用四元数对航天 员的姿态进行动力学建模,将四元数2范数为1的约束加入到动力学方程里。利用该约束运动 理论推导和仿真了航天员姿态欧拉角奇异时的姿态跟踪控制方法。该控制方法对航天员肢体 变化引起的转动惯量等参数的改变具有鲁棒性,能通过平衡解稳定参数的选取方便地对控制 系统的性能进行调节,且计算量小。
     

等参化FVDAM在复合材料湿热应力分析中的应用

在等参化有限元体积直接平均法（FVDAM）中引入等效湿胀系数,建立了复合材料湿热耦合的细观应力场分析模型。计算了湿热环境中不同纤维体积含量和湿含量复合材料的细观应力场。结果表明：湿热环境中复合材料界面径向应力最大值发生于纤维密集区的相邻纤维间的界面处,最小值出现在基体富区;初始吸湿对热残余应力有释放作用,最终吸湿的影响将超过热残余应力,界面应力状态也随之改变。计算所得细观应力场与有限元（FEM）法有较好的一致性。     

On the dynamics of the heliosphere on intermediate and long time-scales

A time-dependent, three-dimensional model of the dynamics of the heliosphere as a result of solar activity and a time-varying local interstellar medium is presented. The model is based on a recent version of the well known ZEUS code and employs parallel processing. It includes the solar and interstellar plasma components as well as neutral atoms, and contains the heliospheric magnetic field in a kinematic fashion. We study the dynamics of the heliosphere due to solar activity on periods of months to years up to the so-called Schwabe (11-year) cycle as well as due to time variations of the local interstellar medium, all of which have drawn increasing attention during recent years, as the significance of their direct or indirect effect on the Earth and its environment is under lively debate.     

Space weather and commercial airlines

Space weather phenomena can effect many areas of commercial airline operations including avionics, communications and GPS navigation systems. Of particular importance at present is the recently introduced EU legislation requiring the monitoring of aircrew radiation exposure, including any variations at aircraft altitudes due to solar activity. With the introduction of new ultra-long-haul “over-the-pole” routes, “more-electric” aircraft in the future, and the increasing use of satellites in the operation, the need for a better understanding of the space weather impacts on future airline operations becomes all the more compelling. This paper will present the various space weather effects, some provisional results of an ongoing 3-year study to monitor cosmic radiation in aircraft, and conclude by summarising some of the identified key operational issues, which must be addressed, with the help of the science community, if the airlines want to benefit from the availability of space weather services.     

Attempt to identify a source mechanism of Mercury’s sodium exosphere by a spectrometer using Fabry–Perot etalon

The Mercury’s Sodium Atmosphere Spectral Imager (MSASI) on BepiColombo (BC) will address a range of fundamental scientific questions pertaining to Mercury’s exosphere. The measurements will provide new information on regolith–exosphere–magnetosphere coupling as well as new understanding of the dynamics governing the exosphere bounded by the planetary surface, the solar wind and interplanetary space. MSASI is a high-dispersion visible spectrometer working in the spectral range around sodium D2 emission (589 nm). A tandem Fabry–Perot etalon is used to achieve a compact design. We presents a design of the spectral analyzer using Fabry–Perot interferometer. We conclude that: (1) The MSASI optical design is practical and can be implemented without new or critical technology developments; (2) The thermally-tuned etalon design is based on concepts, designs and materials that have good space heritage.     

Gnevyshev gap, Forbush decreases, ICMEs and solar wind electric field: relationships

We have studied annual frequency distribution of the Forbush decreases for three solar cycles (20, 21, 22); most are associated with the fast ICMEs and SSCs. The frequency varies in step with the solar cycle but the distribution has a notable gap embedded in it, near the maximum of the cycle leading to two peaks in Forbush decreases per cycle. We show that the gap coincides with the epoch of solar polar field reversal. There is an indication of an odd/even cycle effect in the frequency distribution of Forbush decreases and the associated SSCs. We find that two peaks in Forbush decrease and SSC distributions are separated by the Gnevyshev gap; second peaks occur well before the onset of the high-speed streams in the descending phase of a cycle which do not cause Forbush decreases but do contribute to a peak in the geomagnetic activity index Ap. We compare Forbush decrease and SSC distributions with the corresponding distribution of the solar wind electric field and find that a large amplitude of the electric field of itself does not cause a Forbush decrease to occur unless it is also associated with a fast ICME/SSC.     

RPC-MIP: the Mutual Impedance Probe of the Rosetta Plasma Consortium

The main objective of the Mutual Impedance Probe (MIP), part of the Rosetta Plasma Consortium (RPC), is to measure the electron density and temperature of Comet 67P/Churyumov-Gerasimenko’s coma, in particular inside the contact surface. Furthermore, MIP will determine the bulk velocity of the ionised outflowing atmosphere, define the spectral distribution of natural plasma waves, and monitor dust and gas activities around the nucleus. The MIP instrumentation consists of an electronics board for signal processing in the 7 kHz to 3.5 MHz range and a sensor unit of two receiving and two transmitting electrodes mounted on a 1-m long bar. In addition, the Langmuir probe of the RPC/LAP instrument that is at about 4 m from the MIP sensor can be used as a transmitter (in place of the MIP ones) and MIP as a receiver in order to have access to the density and temperature of plasmas at higher Debye lengths than those for which the MIP is originally designed.