考虑俯仰时鸭式布局飞机突风载荷系数计算

采用离散突风模型，通过解飞机运动微分方程，分析计算了飞机在考虑纵向转动时的突风过载系数，与ＮＡＣＡＲ１２０６的计算模型相比，本文的模型考虑了因俯仰而产生的升为增量和因俯仰使飞机迎角变化而产生的升力增量，并以ＡＤ２００双座鸭式布局轻型飞机为例，分析和计算了飞机俯仰对突风过载系数的影响。尽管轻型飞机穿过一个突风的时间相对较长，但对具有静稳定性的飞机，特别是对于通常具有前翼先失速特点的鸭式布局飞机．飞机的俯仰对飞机的最大过载影响不大。ＡＤ２００飞机突风过载计算结果表明：飞机的纵向转动对鸭式布局飞机的突风过载系数的影响很小，可忽略不计，即ＮＡＣＡＲ１２０６给出的突风载荷系数计算公式对鸭式布局轻型飞机是足够精确的。     

用脉冲光屏法测量高温等离子体流场中的粒子

粒子场测量技术目前广泛用于气液、气固两相流中，但是在等离子体流场中的粒子测量目前尚未很好解决。本文采用序列脉冲激光屏多次曝光摄影法，克服了流场的严重干扰，在电弧加热器等离子体流场中，对飞行速度达２０００ｍ／ｓ的粒子实验获得成功，得到某一截面内粒子的尺寸、空间分布及数密度等参数。     

机载光电跟踪系统基于遗传算法的模糊控制器优化设计研究

分析了机载光电跟踪系统的构成，并对机载光电跟踪系统的最主要成部分－陀螺平台框架系统设计了基于GA（遗传算法）的模糊控制器，由于遗传算洒可以搜索整个空间，不易陷入局部最优解，不受搜索空间的限制性假设的约束，因此本文通过遗传算法对模糊控制器的控制规则，参数以及量化因子和比例因子进行了优化，在对模糊控制器设计的过程中，为了提高模糊控制的精度并加速遗传算法的收敛速度，还采用了变论域的方法，通过对系统详细的仿真研究，验证了基于GA的模糊控制器设计的良好控制效果。     

Studies of electron and ion temperatures at 500 km altitude during sunrise using Indian SROSS C2 satellite

Solar dependence of electron and ion temperatures (T_e and T_i) in the ionosphere is studied using RPA data onboard SROSS C2 at an altitude of ∼500 km and 77°E longitude during early morning hours (04:00–07:00 LT) for three solar activities: solar minimum, moderate and maximum during winter, summer and equinox months in 10°S–20°N geomagnetic latitude. In winter the morning overshoot phenomenon is observed around 06:00 LT (T_e enhances to ∼4000 K) during low-solar activity and to T_e ∼ 3800 K, during higher solar activity. In summer, it is observed around 05:30 LT, but the rate of T_e enhancement is higher during moderate solar activity (∼2700 K/hr) than the low-solar activity (∼1700 K/hr). During equinox, this phenomenon is delayed and is observed around 06:00 LT (∼4200 K) during all three activities.     

The response of sporadic E-layer to the total solar eclipse of July 22, 2009 over the equatorial ionization anomaly region of the Indian zone

The digital ionosonde located in Bhopal (23.2°N, 77.2°E), India has been used to investigate the responses of the Es layer in the equatorial ionization anomaly (EIA) crest to the total solar eclipse (TSE) of July 22, 2009. Results show the presence of intense Es layer during and after the eclipse period. The gravity waves induced by the solar eclipse propagated upward in the Es layer and produced the periodic disturbance. The results of the wavelet analysis display the presence of dominant oscillation of about 24–32, 16–20 and 8 min. The appearance of intense sporadic-E concomitantly with the signatures of gravity wave suggests that the wind shear introduced by the solar eclipse induced gravity wave might be the plausible mechanism behind the intensification of Es-layer ionization.     

Mission analysis and performance comparison for an Advanced Solar Photon Thruster

The so-called “compound solar sail”, also known as “Solar Photon Thruster” (SPT), is a design concept, for which the two basic functions of the solar sail, namely light collection and thrust direction, are uncoupled. In this paper, we introduce a novel SPT concept, termed the Advanced Solar Photon Thruster (ASPT), which does not suffer from the simplified assumptions that have been made for the analysis of compound solar sails in previous studies. After having presented the equations that describe the force on the ASPT and after having performed a detailed design analysis, the performance of the ASPT with respect to the conventional flat solar sail (FSS) is investigated for three interplanetary mission scenarios: an Earth–Venus rendezvous, where the solar sail has to spiral towards the Sun, an Earth–Mars rendezvous, where the solar sail has to spiral away from the Sun, and an Earth-NEA rendezvous (to near-Earth asteroid 1996FG3), where a large change in orbital eccentricity is required. The investigated solar sails have realistic near-term characteristic accelerations between 0.1 and 0.2 mm/s². Our results show that an SPT is not superior to the flat solar sail unless very idealistic assumptions are made.     

Various methods of calibration of the STEREO/WAVES antennas

On October 25th, 2006, NASA’s two STEREO spacecraft were launched which are designed to increase our knowledge of the physics of the solar system. On board they carry a sophisticated radio experiment, called S/WAVES. The key technology, used by S/WAVES is the direction finding capability in addition to the use of two spacecraft which makes it possible to triangulate radio sources. Direction finding requires the reception properties of the antennas to be known very accurately. We applied several different methods to calibrate the S/WAVES antennas. In this paper the methods are described and compared and the results are presented and discussed with respect to advantages and disadvantages of the different methods.     

A polytropic model for the solar wind

The solar wind fills the heliosphere and is the background medium in which coronal mass ejections propagate. A realistic modelling of the solar wind is therefore essential for space weather research and for reliable predictions. Although the solar wind is highly anisotropic, magnetohydrodynamic (MHD) models are able to reproduce the global, average solar wind characteristics rather well. The modern computer power makes it possible to perform full three dimensional (3D) simulations in domains extending beyond the Earth’s orbit, to include observationally driven boundary conditions, and to implement even more realistic physics in the equations. In general, MHD models for the solar wind often make use of additional source and sink terms in order to mimic the observed solar wind parameters and/or they hide the not-explicitly modelled physical processes in a reduced or variable adiabatic index. Even the models that try to take as much as possible physics into account, still need additional source terms and fine tuning of the parameters in order to produce realistic results. In this paper we present a new and simple polytropic model for the solar wind, incorporating data from the ACE spacecraft to set the model parameters. This approach allows to reproduce the different types of solar wind, where the simulated plasma variables are in good correspondence with the observed solar wind plasma near 1 AU.     

Investigations on temperature distribution of satellite surfaces affected by solar absorptivity

Based on the Monte Carlo ray-tracing method, the network coefficients of thermal network model describing the radiation heat transfer among satellite surfaces is solved by considering the surface material optical characters. It is superiority to the conventional Gebhart’s method in view of the grey body and the diffuse reflection assumptions. The zone leveling method is used to discrete the governing equations and the solar absorpivity is separated and considered to be an important correction parameter. Effects of the solar incidence round angle, the zenith angle and the ratio of absorpivity to emissivity (RAE) on temperature distribution are numerically simulated and discussed in detail. The higher or the lower the RAE may be lead to the alternative heating and cooling tend with a larger heating or cooling velocity of main body surfaces than the solar array surfaces. Furthermore, maximum temperature of main body is almost larger than solar arrays. Under the same RAE, solar incidence angle make a great effect on the uniform character of temperature distribution.