星基空间人造飞行器探测概率分析

随着空间飞行器数量的日益增多,空间碰撞的概率也逐步加大。为了确保自身飞行器的安全,同时为了减少对目前在轨的飞行器的干扰,通过某种途径来感知空间飞行器的信息,包括轨道和结构外形等参数,是十分必要的。除了地基手段对空间飞行器进行观测外,星基空间飞行器探测是一种不可或缺的补充手段。文章通过对所掌握的空间飞行器数据库,给出了基于地球低轨道观测卫星情况下,星基空间飞行器探测概率的统计结果。     

满足一定约束条件的登月飞行轨道的设计

讨论满足约束条件的登月飞行轨道的设计问题，将约束条件分类为只与太阳，月球，地球，飞行器和观测站之间的相对位置有关的运动学约束条件以及小及到飞行器轨道云动的动力学约束条件，在考虑登月飞行轨道的特征后，给出一种设计满足约束条件的标准飞行轨道的方法，并将方法应用于不同约束条件下的我国登月飞行以及月球卫星的轨道预测计。     

满足约束条件的月球卫星飞行轨道的初步设计

讨论满足约束条件的月球卫星飞行轨道的设计问题，将约束条件分类为只与太阳，月球，地球，飞行器和观测站之间的相对位置有关的运行学约束条件以及涉及到飞行器轨道运行的动力学约束条件，在考虑月球卫星轨道的受力情况后，给出一种准确快速地计算和设计满足约束条件的标准飞行轨道的方法，并应用于不同约束条件下月球卫星的轨道预设计，初步讨论了轨道设计的误差分析，轨道跟踪及实时精密定轨等正在进行的其它相关工作。     

首个太空“经济适用房”落成

2011年9月29日21时16分n3秒,我国长征二号FT1运载火箭携带“天宫”一号目标飞行器升空。21时25分45秒,天宫一号目标飞行器准确进入近地点200千米、远地点346千米、倾角42．7。的预定轨道。9月30日1时58分,     

脉冲星在空间飞行器定位中的应用

利用脉冲星钟模型能高精度地预报脉冲星脉冲到达太阳系质心的时间。基于脉冲星时、空参考架可实现各类空间飞行器的自主导航。讨论了脉冲星钟的模型和脉冲星导航系统的框架结构,描述了脉冲星导航的基本原理和算法。指出脉冲星导航系统对脉冲星脉冲到达探测器时刻的测量精度,是决定空间飞行器位置解算精度的关键因素。脉冲星导航观测采用的原子钟如果足够稳定,则空间飞行器位置的解算方法可以简化。在脉冲星导航系统计时观测精度达到或优于几十微秒量级时,脉冲星视差、相对论效应的影响是不可忽略的。对脉冲星导航系统开发设计中的关键技术和进一步研究的主要问题进行了初步分析和讨论。     

环月飞行器精密定轨的模拟仿真

以中国正在实施的探月计划“嫦娥1号”工程为背景，分析了在中国联合S波段(USB)测控网和甚长基线射电干涉(VLBI)跟踪网的现有空间分布、观测精度水平下的环月飞行器精密定轨．采用的方法是模拟仿真计算，即首先模拟观测数据，然后在计入各误差源的影响后进行求解，并对解算结果进行比较．模拟仿真的工具是美国宇航局哥达德飞行中心的空间数据分析软件系统GEODYN．环月飞行的主要误差源是月球重力场，为此首先讨论了目前精度最高的月球重力场模型JGL165P1的(形式)误差．在模拟了测距、测速以及VLBI的时延、时延率数据后，计入月球重力场的误差进行精密轨道确定．定轨时采用了减缩动力学(reduced dynamic)方法，即选用合适的经验加速度参数吸收重力场误差对定轨的影响．结果表明对于一个不将月球重力场作为主要科学目标的探月计划(如“嫦娥1号”)，减缩动力学方法是一个简单、有效地提高环月飞行器定轨精度的方法．     

一句话新闻

美国宇航局12月10日宣布将在,2011年发射一个月球探测器,引力分布和内部探测器（Gravity Recovery and Interior Laboratory,GRAIL）,将把两个飞行器送往月球,精确测量它的引力场分布和内部结构,精度比以往探测器高一千倍。     

“天宫一号”过境观测指南

随着“天宫一号”目标飞行器（下文简称天宫）和“神舟八号”飞船顺利发射并成功对接,我国又掀起了一股航天热潮。同时,许多人都很好奇,我们在地面上能不能用肉眼看到天宫,又能否用相机拍下它的倩影呢？答案是肯定的,不过要想看到其形状几乎不可能,且听我慢慢道来。     

美军试射新型天地往返飞行器

2010年年4月22日,美国用宇宙神-5火箭从锦罗里达州卡纳维拉尔角空军基地,发射了波音公司为美国空军研制的无人X-37B轨道试验飞行器-1（OTV-1）,用于进壬多种技术试验,为研制军用航天飞机做准备。     

实用恒星参考系统

本文介绍了一个新的星场参考星快速检索系统,利用它可以快速得到星场星的标准坐标和球面坐标,同时生存作星图的数据文件,以供恒星证认使用。此系统能满足照相和CCD等天体测量工作的需要。特别是对于各种空间飞行器的天文实时定位能提供一个精确而快速的参考坐标系统。     

Excitation of plasma waves by bodies moving in ionized atmosphere

A body moving in an ionized atmosphere acquires an electric charge through the processes of accretion of charged particles and emission of electrons by high energy photons. The moving charged body may then interact with the charged particles of the atmosphere and any pervading magnetic field to excite plasma waves. Of particular interest is the situation in which the body collects an ionized cloud in front of it. The motion of this ionized cloud in the atmosphere induces an electrostatic instability and causes a column of ionized gas to move ahead of the body. The electrostatic instability is conducive to the excitation of electrostatic oscillations which if already present are further enhanced. A magnetic field along the direction of motion assists in the formation of the ionized cloud. If the pervading magnetic field is of suitable weak strength, it may excite extraordinary electromagnetic waves. A pervading transverse magnetic field of suitable strength may cause the excitation of magnetohydrodynamic waves.     

Dynamics of multibody chains in circular orbit: non-integrability of equations of motion

This paper discusses the dynamics of systems of point masses joined by massless rigid rods in the field of a potential force. The general form of equations of motion for such systems is obtained. The dynamics of a linear chain of mass points moving around a central body in an orbit is analysed. The non-integrability of the chain of three masses moving in a circular Kepler orbit around a central body is proven. This was achieved thanks to an analysis of variational equations along two particular solutions and an investigation of their differential Galois groups.     

Determination of the potential in a synodic system

Determination of the potential field in a fixed (inertial) system may be accomplished by the solution of a homogeneous linear partial differential equation when a family of orbits of a body moving in the field is given. This partial differential equation was presented and thoroughly analyzed earlier. The present paper discusses the same problem in a rotating system where the centrifugal and Coriolis effects render the pertinent partial differential equation in general non-homogeneous and non-linear. A linear, though non-homogeneous, partial differential equation for the determination of the synodic potential is obtained only in the special case of iso-energetic families of orbits.     

Parametric dependence of the stationary solutions in the restricted 2 + 2 body problem

The restricted gravitational 2 + 2 body problem, is a particular case of the N body problem and it may be used to approximate the dynamical behaviour of binary asteroids or dual sattelites moving in the gravitational field of two primaries Pi, i = 1,2. By considering oblate primaries, five parameters are needed to describe the model, namely the reduced mass μ of the primary P2, the reduced masses μ1 and μ2 of the minor bodies and the oblatenesses Ii, i = 1,2 of the primaries. This work deals with the effect of those parameters on the location of the stationary solutions. This revised version was published online in July 2006 with corrections to the Cover Date.     

Analysis of the potential field and equilibrium points of irregular-shaped minor celestial bodies

The equilibrium points of the gravitational potential field of minor celestial bodies, including asteroids, comets, and irregular satellites of planets, are studied. In order to understand better the orbital dynamics of massless particles moving near celestial minor bodies and their internal structure, both internal and external equilibrium points of the potential field of the body are analyzed. In this paper, the location and stability of the equilibrium points of 23 minor celestial bodies are presented. In addition, the contour plots of the gravitational effective potential of these minor bodies are used to point out the differences between them. Furthermore, stability and topological classifications of equilibrium points are discussed, which clearly illustrate the topological structure near the equilibrium points and help to have an insight into the orbital dynamics around the irregular-shaped minor celestial bodies. The results obtained here show that there is at least one equilibrium point in the potential field of a minor celestial body, and the number of equilibrium points could be one, five, seven, and nine, which are all odd integers. It is found that for some irregular-shaped celestial bodies, there are more than four equilibrium points outside the bodies while for some others there are no external equilibrium points. If a celestial body has one equilibrium point inside the body, this one is more likely linearly stable.     

Further results for astrophysics from the cosmology within the framework of the Projective Unified Field Theory

Recently the 5‐dimensional Projective Unified Field Theory (PUFT) of the author (Schmutzer 1995a, Schmutzer 1995b) has been applied to a closed homogeneous isotropic cosmological model with the result of a cosmology without big bang (Schmutzer 1999a, Schmutzer 1999b). Continuing this approach, in this paper following subjects are treated: recalculation of numerical values of cosmological quantities, exact solution of the field equations to a point‐like body, motion of a test body in such a field, definition of the empirical effective gravitational factor (“constant”), Einstein effects compared to the empirical situation, adiabatic approximation of the motion of an orbiting testbody under the influence of the expanding cosmos (transition of the ellipses to circles, decrease of the radius of the orbiting bodies, decrease of the excentricity, increase of the frequency of orbiting objects etc.), heat production in a moving body induced by the cosmological expansion with application to various cosmic objects.     

The conditions for the existence of the electric field opposite to the current along the magnetic field lines in the thin plasma

The flow of the current along the magnetic field lines in the thin plasma directed opposite to the electric field is considered. The particles moving to the equatorial plane are supposed to have mirror points above the region of absorption (the ionosphere) and the particles moving to the ionosphere are supposed to have mirror points below the region of absorption. The current, therefore, flows. The functions of the distribution of the electrons and ions are considered to be mono-energetic. The energies of the electrons and the ions and their densities on the boundary of absorption are estimated for the potential difference and for the current density which are typical for the auroral field lines.     

Gravitational potential of solid bodies in the solar system

The gravitational potential of a solid body is expanded without approximation in any moving reference frame, in terms of harmonic coefficients relative to fixed axis in the body.     

Adiabatic motion of an electron bunch in the magnetosphere

The motion of a space-limited energetic electron bunch injected along geomagnetic field lines is studied. Dimensions of a bunch moving in a weakly inhomogeneous medium are shown to change so that a product of the bunch and background densities divided by a square of the magnetic field appears to be an adiabatic invariant. The bunch decelerates when its density tends to the background electron density.     

Breakup of moving clusters in the galactic disk

Numerical simulations are used to analyze the breakup of moving groups in the Galactic disk through the internal velocity dispersion of the group components and the tidal effect of the external regular gravitational Galactic field and giant molecular clouds. The initial locations of the group centroids correspond to well-known moving streams: the Hyades, the Pleiades, the Ursa Major cluster, and the group HR 1614. The mean group breakup times have been found as a function of the adopted limiting group size. The interactions of stream stars with giant molecular clouds reduce significantly the group lifetime.