空间目标逆轨网捕拦截停泊轨道的优化设计

为了提高对空间目标的拦截成功率,可采用拦截器从停泊轨道转移进入拦截轨道逆轨网捕拦截的方式。利用椭圆弹道理论,讨论和分析了该拦截方式停泊轨道优化问题的描述、模型的建立及优化的方法。计算结果表明,对该拦截方式所建立的模型和采用的优化方法满足逆轨拦截对轨道设计的要求,可为空间快速拦截应用提供理论借鉴和参考。     

简单二体引力模型用于空间目标轨道面交线确定的效果分析

在空间目标碰撞预警分析中，准确地计算出空间目标的轨道面交线是进行地心距筛选、时间差筛选的前提，目前较多使用的快速确定轨道面交线的方法为简单二体引力模型。深入分析该模型，比较了其计算的空间目标轨道面交线与STK计算结果的差异，指出了简单二体引力模型在计算空间目标轨道面交线时的局限性，认为轨道摄动是影响轨道面交线计算准确性的主要原因，应该采用更能反映空间目标实际运动规律的改进的二体引力模型的方法。     

地月空间DRO与HEO(3∶1/2∶1)共振轨道延拓求解及其稳定性分析

针对地月空间共振轨道延拓求解及稳定性分析问题,首先从远离与接近月球的地心开普勒共振轨道(月球公转周期与轨道周期符合1∶1、2∶1与3∶1的比例关系)得到圆形限制性三体模型中的两组轨道初值,然后通过增大与减小"近地点距"的延拓方法得到圆形限制性三体周期轨道族。研究发现:逆行绕月的远距逆向轨道(DRO)可由1∶1开普勒共振轨道延拓得到,延拓过程中轨道共振比从1∶1逐渐演变为2∶1与3∶1,并展现出明显的非开普勒轨道特性;另外,一类大偏心轨道(HEO)通过2∶1与3∶1地心开普勒共振轨道的延拓得到,但仍可看作受摄的开普勒轨道。采用周期轨道Monodromy矩阵的特征值分析了DRO和HEO的稳定性,同时描述了各自轨道运动特点,可为相关的空间应用任务设计提供理论依据。与此同时,澄清了不同参考模型中"共振比"的概念以及同一共振比可能对应不同类型共振轨道的现象。     

三体模型下二维平面地月转移轨道设计与特性分析

为提高地月转移轨道搜索速度和提供精确的初值猜测,在三体模型下研究了双脉冲地月转移轨道的快速设计方法及其轨道特性。首先基于三体模型建立了地心旋转系下地月转移轨道系统模型,选择物理意义明显的地月转移加速速度增量和地心旋转系对准角作为控制变量;其次在二体模型假设下给出控制变量的初值估计方法,提出了不同运行方向地月转移轨道的搜索策略,并采用序列二次规划算法对4种类型地月转移轨道进行求解,分析其控制变量差异;最后分析了转移时间、近地点高度和近月点高度对地月转移轨道的影响,以及月球引力对二体模型下初值估计的修正量。仿真结果表明,本文提出的设计方法能快速准确地搜索出指定类型的地月转移轨道,同时其轨道特性分析结论可为后续月球探测任务地月转移轨道选择提供依据。     

近空间高超声速流场通量分裂型DSMC-IP方法

针对近空间高超声速流场的特点,采用Van Leer格式对直接模拟蒙特卡洛-信息保存(DSMC-IP)方法质量守恒方程中的计算格式进行改进.将局部马赫数作为分裂通量的标准,并重构单元分界面两侧的左右输运通量,使得计算格式具有通量分裂的特点,解决了DSMC-IP方法在高超声速流场计算中的应用问题.将改进后的通量分裂型DSMC-IP方法引入非结构网格中,对二维近空间高超声速流场进行数值模拟.计算结果表明:通量分裂型DSMC-IP方法所得出的数值结果与实验值及参考值符合较好,明显降低了直接模拟蒙特卡洛(DSMC)方法所带来的统计耗散.当来流气体的稀薄程度增加时,其非平衡效应也更加明显,而通量分裂型DSMC-IP方法的计算结果与参考值相差均在10%以内,良好地反映了非平衡条件下的流场特征,验证了通量分裂型DSMC-IP方法的可行性和有效性.      

高超声速飞行器钝舵缝隙流动数值模拟研究

目前,带缝隙钝舵的缝隙引起的流场结构和气动加热规律变化,还很不明确,需要研究缝隙诱导所形成旋涡的空间分布特征和旋涡运动对物面气动加热的影响规律。通过分析高超声速钝舵缝隙气动加热问题,基于无缝隙钝舵,建立一种带缝隙钝舵简化模型。使用有限体积方法求解可压缩Navier-Stokes方程,通量采用van Leer通量向量分裂方法计算。插值采用MUSCL方法,时间项采用LU-SGS隐式方法。结果表明:无缝隙钝舵流场结构相对简单,带缝隙钝舵流场结构同无缝隙钝舵相比要更为复杂,舵轴上游缝隙内会出现马蹄形涡串结构,相应地在缝隙的上下表面均会出现马蹄形高热流区;受缝隙诱导分离再附流动的影响,在舵轴迎风面以及舵体侧面后部均形成了局部高热流区。     

关于超声速剪切流动的数值模拟

本文通过采用混合型的四阶精度频谱关系保持格式和基于信号特征传播的边界处理方法,对对流马赫数分别为0.5、0.9和1.4的时间发展和超声速空间发展的剪切流动进行了数值模拟,目的是对剪切层不稳定结构的演化方式、相同对流马赫数下时间发展和超声速空间发展的剪切流动的异同作初步研究.研究表明,对时间发展的剪切流动来说(1)当Mc=1.4时,剪切层内流动演化的形态为首先压力等值线在其极值点处产生中心型结构,且极大值点和极小值点交替分布.然后中心型结构进一步发展并产生横向分裂,从而在剪切层内等压力线出现鞍点结构.随后剪切层内重新产生中心型的压力极值点结构,进而又出现鞍点结构.如此发展下去,剪切层内的压力等值线呈现中心和鞍点的组合.剪切层外的压缩波沿特征线方向传播并加强,形成类激波的结构,最后在流场中包含许多压缩和膨胀波.在计算时间内流向的周期性未受破坏.(2)当Mc=0.5时,初始的流向的周期结构经过一定时间后将丧失其稳定性.在计算域为两个扰动周期的情况下,扰动形成的旋涡的后期演化表现为涡的对并.(3)对Mc=0.9的流动,演化图象介于前两者之间.对具有相同对流马赫数的空间问题来说,由于粘性和非线性发展对周期性的破坏,随着空间距离的增长,流动演化与时同问题的差异增大.相比较而言,高对流马赫数的时间问题与空间问题的差异明显大于低Mc下的差异.     

关于大行星（或月球）轨道器的冻结轨道

关于人造地球卫星的冻结轨道问题早已为人们所熟知，而且已有相应的卫星在轨运行。在考虑该冻结轨道形成时，主要依据地球扁率J3项与J2项的相对关系，这是由地球非球形引力场的特征所决定的，原理十分清楚，但其原理和结论不能随意地用于其他大行星(或月球)的轨道器。在一般情况下，对于低轨卫星形成冻结轨道的条件，非球形引力位中的奇次带谐项(J21 1，l≥1)将起重要作用。不仅仅是一个J3项，例如月球轨道器，J3，J5，J7和J9均有不可忽视的影响，而且与轨道倾角有一定的关系。为此，本文根据轨道理论对冻结轨道的存在性及其有关问题作进一步的分析，给将来的深空探测提供轨道设计的有关信息和依据。     

太空发电站大型柔性结构控制系统设计

太空发电站作为千米级空间超大尺度柔性结构,针对其超长梁和膜结构的三轴稳定姿态控制以及地球静止轨道的定点运行,设计了一套姿态轨道控制系统。首先运用等效简化的方法将主次桁架结构进行简化,建立了简化模型,进而利用简化模型的模态信息实现了多柔性体动力学建模。分析了大尺度柔性结构在姿态和轨道方面所受到的空间扰动,主要包括太阳光压摄动、重力梯度摄动等因素,并据此设计了以电推进器为执行机构的三轴稳定的姿态控制系统和分散式的轨道控制系统。仿真估算结果表明,控制系统能够满足姿态、轨道控制要求,但燃料消耗较大。     

基于三体Lambert算法的平动点交会轨道设计

针对未来建设地月系L2点空间站的需求,提出利用三体Lambert算法研究地月系L2点附近轨道的交会问题,包括设计同一Halo轨道上不同相位两航天器之间的交会转移轨道以及设计不同振幅Halo轨道之间的交会转移轨道。针对现有三体Lambert算法求解长时间轨道转移问题收敛性差的缺陷,提出利用遗传算法求解初始参考轨道,进而通过同伦牛顿-拉夫逊迭代求解目标转移轨道的方法。计算结果表明,该方法能够有效解决长时间交会轨道转移问题,可以为地月空间平动点区域空间站建设提供参考。     

Supernovae and the origin of the solar system

This review concentrates on recent ideas involving a relationship between the early solar system and supernova explosions. It summarizes briefly the data that has helped inspire those ideas. Because the true relationship is still unknown and generates controversy, the distinct ideas are introduced singly in the historical context of their origins, and the active sense of surprise and controversy is visible. Quotations from pivotal papers are used as part of the exposition. The subject involves equally the isotopic anomalies detected in meteorites and the dynamic events of galactic evolution, nucleosynthesis, and protosolar collapse. Whatever the correct situation is, new connections have been found between the origin of the elements and the formation of the solar system. The objective of this review is to enable interested space scientists to quickly identify the competing points of view and the experiments and theories that have led to them.     

Gamow and the physics and evolution of stars

The high temperature sensitivity of thermonuclear reactions and the neurrino emission at the final stages of stellar evolution (urca process) are the most crucial Gamow's contribution to the physics and evolution of stars. G. Gamow made one of a few first attempts in astrophysics to get a comprehensive picture of stellar evolution from the main sequence (thenormal stars in his terminology) through the formation of white dwarfs, gravitational collapse of stellar cores and supernova explosions.     

Plasma-induced sputtering of an atmosphere

Magnetospheric ions, solar wind ions, and locally produced pick-up ions can impact the atmospheres of objects in the solar system, transferring energy by collisions with atmospheric atoms and molecules. This can result in an expansion of the atmospheric corona with a fraction of the energetic atoms or molecules being lost (sputtered) from the atmosphere. The expanded corona presents a larger target to the incident plasma, which in turn enhances pick-up ion formation and collisional ejection. In this manner a significant flux of atoms or molecules can be lost from an atmosphere, affecting its long-term evolution. This has been shown to be an important process for the dynamics and evolution of the atmosphere of lo, which is bombarded by the Jovian magnetospheric plasma, and for loss of atmosphere from Titan. Sputtering by pick-up ion bombardment has been shown to remove material from the atmosphere of Mars affecting the observed isotope ratios, and energetic O⁺ precipitation affects the Earth's thermosphere. The physics of ion bombardment of a gas which leads to atmospheric sputtering is described here. Analytic expressions derived from transport equations are shown to be useful for estimating the sputtering rate. These are compared to results from transport and Monte-Carlo calculations.     

空间物体的若干法律问题研究

对空间物体的概念、特征进行了研究，探讨了空间物体与空间碎片以及航空航天物体之间的关系，从而明确了空间物体的内涵与外延。此外，对空间物体发射国和空间物体的登记制度进行了研究，提出区分不同情况确定发射国和通过协议划分损害赔偿责任的创新观点。     

Magnetohydrodynamic discontinuities in space plasmas: Interrelation between stability and structure

It is believed that shock waves and other discontinuous flows form the basis of a wide range of phenomena in space medium. We review the results concerning the particular property of MHD discontinuities, the interrelation between their stability and structure. Such an interrelation is associated primarily with the requirement of their evolutionarity. For a non-evolutionary discontinuity the amplitudes of reflected and refracted waves caused by a small amplitude incident wave are not determined unambiguously from the conservation laws at the discontinuity surface. Since the problem of the further time evolution of the initial small perturbation does not have a unique solution, such a discontinuity cannot exist in a real medium as a single steady-state configuration. Therefore it is unstable with respect to a disintegration into several discontinuities or to a transition to some more general unsteady flow. This is confirmed by the fact that, in the studied cases, the non-evolutionary shock transitions can, while the evolutionary ones cannot, be represented as a set of several discontinuities and waves of rarefaction. One more fundamental property of the non-evolutionary shocks that argues for their non-existence is that they do not have a unique structure for all values of the dissipative transport coefficients. At the same time, the possibility of their existence cannot be excluded when the shock has a unique structure or when the disintegration is forbidden for some reasons. Besides the non-evolutionarity, which is a direct reason for a disintegration, there is an indirect one. It can be shown that the hydrodynamic shocks without magnetic field that are corrugationally unstable also allow the shock transitions through more than one discontinuity. This suggests that the shocks unstable in the ordinary sense, for which the small perturbation grows with time, do not exist at all, but they disintegrate into stable ones. However, the physical mechanism that distinguishes between these two scenarios remains unclear. The interrelation between the stability and structure of MHD discontinuities thus governs their nonlinear evolution. This fact is essential when describing shock waves and other discontinuous flows in the space medium.     

Projectile Detection of Luminous and Nonluminous Bodies

In a large hyperballistics range, detection of projectiles atstations becomes more complex. Range length permits variation of projectile luminosity and requires greater area for detection. A technique has been devised, using electrooptics, triggering instrumented stations with luminous or nonluminous projectiles. The phototube circuit response, effect of velocity, and effect of light screen thickness on performance are discussed. Data on performance are presented for velocities of 10 000 to 21 000 feet per second. Performance is predicted for velocities of 40 000 and 60 000 feet per second. Nonluminous models as small as 3/16-inch diameter spheres have been detected at a velocity of 21 000 feet per second.     

Low Velocity Collisions and the Growth of Planetesimals

The physics of low velocity collisions (5 m/s to 40 m/s) between basalt bodies ranging in size from 1 m to 10 km is studied in an effort to investigate the early phases of planetesimal accretions. To assess the importance of the internal structure of planetesimals on the outcome of the collisions, we model them either as solid spheres or as rubble piles with a filling factor of 0.5. The collisions are simulated using a three dimensional Smooth Particle Hydrodynamics (SPH) code that incorporates the combined effects of material strength and a brittle fragmentation model. This approach allows the determination not only of the mass of the largest fragments surviving the collisions but also their dynamical characteristics. We find that low velocity collisions are for equal incoming kinetic energy per gram of target material considerably more efficient in destroying and dispersing bodies than their high velocity counterparts. Furthermore, planetesimals modeled as rubble piles are found to be characterized by a disruption threshold about 5 times smaller than solid bodies. Both results are a consequence of a more efficient momentum transfer between projectile and fragments in collisions involving bodies of comparable sizes. Size and shape dependent gas drag is shown to provide relative collision velocities between similar meter-sized objects well in excess of the critical disruption threshold of either rubble piles or solid bodies. Unless accretion can proceed avoiding collisions between bodies of similar masses, the relative weakness of bodies in this size range creates a serious bottleneck for planetesimal growth. This revised version was published online in June 2006 with corrections to the Cover Date.