信息系统群演化的综合环境SEE的研究

旨在通过对系统构架各视角的研究，开发一个信息系统综合演化环境，从而提供针对各类系统演化特征的通用的解决方案，并利用方法论的手段规范、指导和维护系统(群)的演化活动。本文首先论述了大型系统中各个系统和组件变化及改进活动中存在的问题，分析相关的研究及面临的挑战，从而提出系统群演化的概念。然后文章概括了系统群演化的特征，提出解决以上问题的思想方法，即开发“信息系统群演化的综合环境(Synthetic environment of evolution，SEE)”，将各种演化活动纳入规范，指导系统群的演化活动；在此基础上，进一步就实现SEE的关键技术给出了描述及运用的范例。     

跨介质航行器波浪环境入水流场演变和运动特性研究

跨介质航行器是一种既可以在空中飞行又可以在水下潜航的新概念航行器,基于仿生学原理,提出一种通过改变外形实现水空介质跨越的航行器模型,通过入水试验装置和计算流体动力学方法,对航行器带攻角从空气到水的介质跨越过程进行了试验和数值仿真研究,得到了跨介质入水过程航行器的运动姿态和入水空泡形态,并通过数值仿真得到了航行器的升力、阻力、速度和加速度演化规律。同时基于数值模拟方法对有波浪情况和静水情况下航行器入水过程空泡演变以及运动特性进行对比。结果表明:提出的航行器构型在水中具有较好的姿态调整能力,波浪的有无和波高的不同都会对航行体入水运动特性造成影响。     

卫星脉冲推力最优逃逸返回轨迹的非线性规划

重点研究了卫星通过轨道机动逃避碰撞、拦截并经一段时间后返回原轨道的逃逸方式。利用非线性规划理论建立了脉冲推力能量最省的逃逸轨迹规划模型，并考虑非球形摄动的影响对模型进行了修正。通过仿真验证了模型的正确性及求解的可行性，并分析了非球形摄动因素对逃逸过程的影响。     

实时微分控制的算法研究

实时微分控制是进行航天器轨道控制的主要方法。本文在费景高所提出的算法基础上 ,提出了一种有效的改进算法 ,扩大了算法的适用范围。文章对算法的稳定性进行了研究 ,并给出了此算法在弹道导弹显式制导中的应用实例。     

系统参数对电动力绳系动力学的影响

将电动力绳系(EDT)的主星质量、子星质量、绳系质量以及绳系中的电流视为系统参数,研究这些参数对系统的摆动动力学和轨道动力学的影响。哑铃模型下的电动力绳系摆动动力学方程存在不稳定的周期解,通过Floquet理论来衡量周期解的不稳定程度,从而研究各系统参数对摆动动力学的影响。建立了用春分点轨道元素的形式描述的电动力绳系轨道动力学方程,并以降轨时间来衡量电动力绳系的降轨效率,从而研究系统参数对轨道动力学的影响。运用算例对周期解迁移矩阵的特征值、降轨时间随各系统参数的变化关系进行了仿真,分别得出了各系统参数对系统摆动动力学和轨道动力学的影响。综合本文的仿真结果,并考虑实际发射及空间运行中的其它因素,对电动力绳系的设计和降轨策略提出了建议。     

机动卫星星座对多区域目标成像任务规划

针对太阳同步圆轨道卫星星座对地观测任务,研究了在卫星机动情况下对多区域目标的成像任务规划算法.首先提出了单颗卫星对单个点目标的观测方法,解析分析了点目标可见性,并给出了卫星变轨策略;进而通过把区域目标划分为多个条带,将问题转化为卫星对点目标观测问题,结合单星单目标观测方法分析区域目标各条带的可见性;最后建立优化问题模型...     

Effects of in-track maneuver on Sun illumination conditions of near-circular low Earth orbits

By developing approximate analytical models considering the J₂ perturbation, the effects of an in-track maneuver on the orbital Sun illumination conditions of near-circular low Earth orbits are analyzed. First, two approximate models for the variations in orbital sunshine angles are developed, one for variations at a given time and the other for variations at a given argument of latitude. Next, two approximate models for variations in orbital arc in Earth shadow are developed, one considers the small eccentricity and the other uses the zero eccentricity. Finally, the developed approximate models are applied to analyzing the Sun illumination conditions of a typical in-track maneuver mission on a near-circular low Earth orbit. From the results obtained, three major conclusions can be drawn. First, the variations in orbital sunshine angles at a given time may reach tens of degrees when the drifting time reaches hundreds of orbital periods, and the approximate model for that situation cannot effectively approach the numerical results. Second, the variations in orbital sunshine angles for any given argument of latitude are only a couple of degrees even when the drifting time reaches 500 orbital periods, and the approximation model developed can effectively approach the numerical results. Third, for variations in orbital arc in Earth shadow, the approximate model considering the small eccentricity has simple expressions and can effectively approach the numerical results; in contrast, the approximate model using the zero eccentricity has relatively worse precision.     

Halo White Dwarfs and Baryonic Dark Matter

We describe the formation of hot intergalactic gas along with baryonic remnants in galaxy halos. In this scenario, the mass and metallicity of the hot intracluster and intragroup gas relates directly to the production of baryonic remnants during the collapse of galactic halos. We construct a schematic but self-consistent model in which early bursts of star formation lead to a large remnant population in the halo, and to the outflow of stellar ejecta into the halo and ultimately the Local Group. We consider local as well as high redshift constraints on this scenario. This study suggests that the microlensing objects in the Galactic halo may predominantly be 0.5M white dwarfs, assuming that the initial mass function for early star formation favored the formation of intermediate mass stars with m 1M. However, the bulk of the baryonic dark matter in this scenario is associated with the ejecta of the white dwarf progenitors, and resides in the hot intergalactic medium.     

The Primordial Helium-4 Abundance from Observations of a Large Sample of Blue Compact Dwarf Galaxies

We use a sample of 45 low-metallicity H II regions in blue compact dwarf (BCD) galaxies to determine the primordial helium abundance YP with a precision better than 5%. We have carefully investigated the physical effects which may make the He I line intensities deviate from their recombination values such as collisional and fluorescent enhancements, underlying He I stellar absorption and absorption by Galactic interstellar Na I. By extrapolating the Y vs. O/H and Y vs. N/H linear regressions to O/H = N/H = 0, we obtain YP = 0.244±0.002 and 0.245±0.001, respectively, higher than previous determinations (YP = 0.230 - 0.234). Part of the difference comes from the fact that previous investigators have not taken into account underlying He I stellar absorption, especially in the NW component of the BCD I Zw 18 which, because of its extremely low metallicity plays a key role in the determination of YP. We derive a slope dY/dZ = 2.3±1.0, considerably smaller than those derived before. With this smaller slope and taking into account the errors, chemical evolution models with an outflow of well-mixed material can be built for star-forming dwarf galaxies which satisfy all the observational constraints. Our YP gives _bh ₅₀ ² = 0.058±0.007,f consistent with the lower limit set by dynamical measurements and X-ray observations of clusters of galaxies. It is also consistent, within the framework of standard big bang nucleosynthesis theory, with measurements of primordial 7Li in galactic halo stars and with the D/H abundance measured in absorption systems toward quasars by Burles and Tytler (1997).     

The use of Gaussian equations of motions of a satellite for local gravity anomaly recovery

The orbital elements of a low Earth orbiting satellite and their velocities can be used for local determination of gravity anomaly. The important issue is to find direct relations among the anomalies and these parameters. Here, a primary theoretical study is presented for this purpose. The Gaussian equations of motion of a satellite are used to develop integral formulas for recovering the gravity anomalies. The behaviour of kernels of the integrals are investigated for a two-month simulated orbit similar to that of the Gravity field and steady-state ocean circulation explorer (GOCE) mission over Fennoscandia. Numerical investigations show that the integral formulas have neither isotropic nor well-behaved kernels. In such a case, gravity anomaly recovery is not successful due to large spatial truncation error of the integral formulas. Reformulation of the problem by combining the orbital elements and their velocities leads to an integral with a well-behaved kernel which is suitable for our purpose. Also based on these combinations some general relations among the orbital elements and their velocities are obtained which can be used for validation of orbital parameters and their velocities.