绕飞慢自旋小天体的航天器运动分析

针对可以用三轴椭球体近似建模的小天体,给出了非球形引力势函数,建立了航天器绕飞小天体的轨道动力学方程。利用Jacobi积分常数绘制了探测器在小天体周围的零速度曲线,并分析了探测器的可能运动区域,给出了航天器不碰撞小天体的边界条件。针对绕飞慢自旋小天体的情况,基于平均轨道根数的近似解分析了小天体扁率和椭率的摄动影响,并给出了几条冻结轨道及其稳定条件。     

航空用有机玻璃(PMMA)的非线性热粘弹-塑性本构关系

实验测定了航空用有机玻璃T=-40～40℃,ε_t=1.0×10_-4～1.0×10_-1s_-1范围内单轴压缩循环的应力-应变曲线。提出一种考虑温度和应变率效应的非线性粘弹性变形和塑性变形相耦合的本构关系,给出了完备的微分和积分形式的关系方程组,用于拟合各不同温度和应变率的实测曲线,获得了良好吻合的结果。     

Observations of low-energy electrons from AE-C in the south polar cusp during the geomagnetic storm of September 21, 1977

The AE-C spacecraft skimmed through the southern polar cusp at a 400 km altitude during a large geomagnetic storm on September 21, 1977. This period has been designated as a special IMS period, and the AE-C data were acquired close to the times that data were acquired by the DMSP satellite at nearly the same location over the southern polar cap, and by the GEOS satellite located near the noon-meridian in the northern hemisphere. Low energy electrons (1-500 eV) were measured with the photoelectron spectrometer experiment experiment onboard AE-C. This instrument was operated in the mode which measured precipitating electron fluxes and backscattered electron fluxes in alternating 4s intervals with two sensors. A region of intense precipitating electron fluxes was observed near 0924 UT on September 21, 1977 extending from 69 degree invariant latitude at 1100 MLT to 72 degree invariant latitude at 1152 MLT. From the spectra of the precipitating electrons, this region is identified as the southern polar cusp. Since the K _p equals 7- during this time, the displacement of the cusp down to these low latitudes is not unreasonable. Particle data obtained from the DMSP satellite on orbits close to AE-C, confirm that the position of the cusp was rapidly changing during this period, and was displaced to latitudes equatorward of the quiet time position. A second region of intense fluxes of precipitating electron was observed by AE-C at approximately 0933 UT from 69 degree invariant latitude near 1700 MLT to 66 degree invariant latitude near 1730 MLT. This region of low energy electron fluxes is characterized by slightly harder energy spectra and is interpreted as being the afternoon auroral zone. The remarkable and fortunate location of the AE-C, DMSP, and GEOS spacecraft during this special IMS period will allow future correlative studies aimed at the determination of the shape of the magnetosphere during very disturbed conditions.     

考虑静水压力和LODE 角的塑性模型 在GH4169 合金上的应用

针对典型盘用镍基高温合金GH4169,采用Bai-Wierzbizki(B-W)塑性理论对其塑性变形行为进行建模和应用评估。B-W塑性理论假设金属材料塑性变形仍服从von Mises屈服准则,但屈服函数考虑了静水压力和LODE角(偏应力第3不变量)对塑性行为的影响。采用Abaqus/Explicit商业有限元软件编制了该塑性模型的用户材料子程序,设计开展了GH4169合金的光滑、缺口圆棒和缺口平板拉伸试验,基于有限元分析和优化方法确定了B-W模型相关材料参数,对GH4169合金光滑和缺口拉伸响应曲线进行有限元预测,并与试验结果进行对比分析。结果表明:B-W模型预测的GH4169合金缺口圆棒和平板拉伸响应曲线与试验结果非常吻合,而基于传统von Mises塑性模型预测的GH4169合金缺口拉伸响应曲线均明显高于试验曲线。     

Radiative and hybrid cooling of infrared space telescopes

The designs of cold space telescopes, cryogenic and radiatively cooled, are similar in most elements and both benefit from orbits distant from the Earth. In particular such orbits allow the anti-sunward side of radiatively-cooled spacecraft to be used to provide large cooling radiators for the individual radiation shields. Designs incorporating these features have predictedT _tel near 20 K. The attainability of such temperatures is supported by limited practical experience (IRAS, COBE). Supplementary cooling systems (cryogens, mechanical coolers) can be advantageously combined with radiative cooling in hybrid designs to provide robustness against deterioration and yet lower temperatures for detectors, instruments, and even the whole telescope. The possibility of such major additional gains is illustrated by the Very Cold Telescope option under study forEdison, which should offerT _tel5 K for a little extra mechanical cooling capacity.     

Potential experiments with superconducting magnets in Earth orbit

Several experiments that can be performed in Earth orbit with a superconducting magnet are discussed. They are divided into 2 classes, pure plasma physics experiments that can be performed in near Earth orbit and planetary magnetosphere simulation experiments that are best conducted in weak background fields distant from the Earth. The later are all based on the Minimag concept where plasma is directed toward a large dipolar magnet in Earth orbit to form a model miniature magnetosphere. Several experiments that cannot be performed in ground based laboratories and tests that cannot be made in the real magnetosphere can be carried out in Earth orbit. The creation of a miniature model of the magnetosphere (Minimag) forms the basis for several of these experiments.     

A Closed-Form Solution for Doppler Satellite Navigation

Doppler satellite navigation relies on an initial position estimate with an iterative solution. A closed-form solution of this problem, which forms the basis of a complete analytic treatment, is presented. The solution is exact for arbitrary satellite orbits with an ellipsoid Earth model.     

An improved numerical method for constructing Halo/Lissajous orbits in a full solar system model

An improved numerical method that can construct Halo/Lissajous orbits in the vicinity of collinear libration points in a full solar system model is investigated. A full solar system gravitational model in the geocentric rotating coordinate system with a clear presentation of the angular velocity relative to the inertial coordinate system is proposed. An alternative way to determine patch points in the multiple shooting method is provided based on a dynamical analysis with Poincare′sections. By employing the new patch points and sequential quadratic programming, Halo orbits for L_1, L_2, and L_3 points as well as Lissajous orbits for L_1 and L_2 points in the EarthMoon system are generated with the proposed full solar system gravitational model to verify the effectiveness of the proposed method.     

航空发动机管壳式燃-滑油散热器换热特性计算

采用无量纲关系曲线(Re~St·Pr2/3)计算管壳式燃-滑油散热器管程、壳程表面传热系数,基于效率-传热单元数法建立了管壳式燃-滑油散热器换热特性计算模型;以航空发动机某管壳式燃-滑油散热器少量试验数据为基础,拟合得到了该型散热器管程和壳程Re~St·Pr2/3关系曲线,并将该关系曲线应用于另一结构类似的管壳式燃-滑油散热器换热特性计算.算例计算表明:计算值与试验数据吻合较好,管程、壳程出口温度相对误差均不超过6.5%,总换热量相对误差不超过7.4%.该方法可应用于航空发动机管壳式燃-滑油散热器设计及验证阶段的换热特性计算.      

某型增强型复合材料发射筒强度特性评估

为了评估复合材料发射筒的设计是否满足使用要求,建立了某型复合材料发射筒的三维有限元仿真计算模型,并对该型发射筒在吊装、运输、发射工作状态下的受力与变形情况进行了分析评估,得出该型复合材料发射筒在这些过程中的最大变形,采用最大应力准则推导出复合材料发射筒的最小安全系数.评估结果表明:3种工况下,该型复合材料发射筒的最大变...     

An Overview of the Instrument Suite for the Deep Impact Mission

A suite of three optical instruments has been developed to observe Comet 9P/Tempel 1, the impact of a dedicated impactor spacecraft, and the resulting crater formation for the Deep Impact mission. The high-resolution instrument (HRI) consists of an f/35 telescope with 10.5 m focal length, and a combined filtered CCD camera and IR spectrometer. The medium-resolution instrument (MRI) consists of an f/17.5 telescope with a 2.1 m focal length feeding a filtered CCD camera. The HRI and MRI are mounted on an instrument platform on the flyby spacecraft, along with the spacecraft star trackers and inertial reference unit. The third instrument is a simple unfiltered CCD camera with the same telescope as MRI, mounted within the impactor spacecraft. All three instruments use a Fairchild split-frame-transfer CCD with 1,024× 1,024 active pixels. The IR spectrometer is a two-prism (CaF₂ and ZnSe) imaging spectrometer imaged on a Rockwell HAWAII-1R HgCdTe MWIR array. The CCDs and IR FPA are read out and digitized to 14 bits by a set of dedicated instrument electronics, one set per instrument. Each electronics box is controlled by a radiation-hard TSC695F microprocessor. Software running on the microprocessor executes imaging commands from a sequence engine on the spacecraft. Commands and telemetry are transmitted via a MIL-STD-1553 interface, while image data are transmitted to the spacecraft via a low-voltage differential signaling (LVDS) interface standard. The instruments are used as the science instruments and are used for the optical navigation of both spacecraft. This paper presents an overview of the instrument suite designs, functionality, calibration and operational considerations.     

在制品库存优化控制

分析了在制品库存的作用、应设立的位置及最佳容量.建立了离散制造系统在制品库存之比例积分控制模型.再以摩托车曲轴箱体生产线为例评价了控制效果,表明在需求动态变化时PI控制较之传统的正负反馈控制能更好地使在制品库存平稳化.     

同心筒式发射装置附加弹射力影响因素分析

采用同心筒式发射装置发射导弹时,弹底会受到附加弹射力的作用,其值主要取决于排气狭缝宽度、增力装置、导流锥等因素.利用动量方程积分形式推导出附加弹射力的理论公式,分析各种因素对附加弹射力的影响,并利用数值模拟技术进行验证.结果表明:筒底所承受冲击力与弹底所受的附加弹射力呈正相关;减小内外筒间缝隙可提高弹底所受的附加弹射力;加导流锥能降低筒底所受的冲击力.导流锥母线越光滑,筒底所受到的冲击力就越小;增加导流锥后,燃气流动达到稳定状态的时间与无导流锥时所需的时间近似于相等.      

Fundamental parameters of the W Serpentis stars

Application of digital cross-correlation spectroscopy to the spectra of the W Serpentis binaries SX Cas and RX Cas has allowed an accurate determination of the orbits and rotations of the (mass-losing) K-subgiant secondary components. The distortion of the primary radial-velocity curves due to the influence of the prominent accretion disks in these systems has been modelled to first order. This enables us to estimate k ₁, and thereby the mass ratio q 0.30, to within ± 20%. The absolute radii of the secondaries are derived independently from the observed rotations and periods, assuming synchronous rotation. They show that the stars fill their Roche lobes, or at least very nearly so. Rough fits to the available photometry shows both primaries to be unevolved mid-B stars; that in RX Cas appears completely obscured by the disk. Preliminary spectroscopic data for W Ser and W Cru show some promise for similar analyses of these systems.     

How Important are the Equations of Motion in a Chaotic System?

We inquire whether some important features might be lost in studying the gravitational n–body problem because chaos makes it impossible to follow exact phase trajectories. We test this by comparing deliberately crude `integrations' with published results from more precise methods. A general tendency found with high-quality integrations is that a central singularity forms at finite time. The time until that singularity forms is fairly reproducible for systems started from a more or less standard form. We find the same tendency with crude methods, although the time to reach that singularity from the usual initial conditions is less accurately reproduced with cruder methods.     

New Perspectives on Auroral Morphology

The visual aurora takes on a variety of forms. Aurora has a tendency to appear first as very thin, highly structured forms. Over time, these tend to diffuse creating much thicker forms. It is suggested that the extreme variety of auroral forms can be understood in terms of one acceleration mechanism to produce a narrow, field-aligned beam and another process that scatters electrons into trapped orbits. The scattering is due to beam- plasma interactions that generate waves on the upper-hybrid resonance curve. These waves are effective in scattering electrons from parallel to perpendicular directions. The diffuse forms are therefore caused by precipitation of quasi-trapped electrons that have drifted from the field lines on which they were accelerated. Electrons scattered into trapped orbits may also constitute the seed population for the electron radiation belts. It is also suggested that the electron beams are accelerated by inertial Alfven waves that propagate current filaments from the turbulent region in the near-Earth plasma sheet to the auroral zone ionosphere. Electrons can be accelerated by becoming trapped in inertial Alfven waves whose phase velocity increases as they propagate toward the Earth. Specific numerical simulations that could give substance to these suggestions are proposed.     

非稳态油膜力作用下转子振动的分岔与稳定性分析

 利用新的短轴承非稳态油膜力模型分析转子系统的动力学特性, 并通过数值模拟, 得到了该系统随转动角速度变化产生的分岔和混沌特性。利用非线性动力学分析中的打靶法求该系统的周期解, 并利用Floquet 主导特征乘子判断不同周期轨道的失稳方式, 同时发现在系统的运动中存在着倍周期分岔和第二Hopf分岔及鞍结分岔。通过打靶法和Runge-Kutta 方法发现该系统在一定的角速度范围内存在加3 周期分岔。     

Polynomial Representation of NURBS and Its Application to High Frequency Scattering Prediction

This article presents a method that uses physical optics (PO) techniques to compute the monostatic radar cross section (RCS) of electrically large conducting objects modeled by non-uniform rational B-spline (NURBS) surfaces. At the beginning, a new algorithm to convert recursive B-spline basis function into piecewise polynomials in power form is presented. Then, algorithm computes the polynomial representation of B-spline basis functions and NURBS surface geometric parameters are obtained. The PO integral over NURBS surfaces of an electrically large conducting object is used to predict the object's RCS. The NURBS surface is divided into small piecewise polynomial parametric patches by isoparametric curves, and the PO integral expression over the parametric domain of each polynomial parametric patch is reduced to an analytical expression which permits an accurate and effective computation of the PO integral by using a modified Ludwig's algorithm. The RCS of the object can be obtained by adding up the PO integral contribution of each polynomial parametric patch. The effectiveness of this method is verified by numerical examples.     

Structure of reconnection layers in the magnetosphere

Magnetic reconnection can lead to the formation of observed boundary layers at the dayside magnetopause and in the nightside plasma sheet of the earth's magnetosphere. In this paper, the structure of these reconnection layers is studied by solving the one-dimensional Riemann problem for the evolution of a current sheet. Analytical method, resistive MHD simulations, and hybrid simulations are used. Based on the ideal MHD formulation, rotational discontinuities, slow shocks, slow expansion waves, and contact discontinuity are present in the dayside reconnection layer. Fast expansion waves are also present in the solution of the Riemann problem, but they quickly propagate out of the reconnection layer. Our study provides a coherent picture for the transition from the reconnection layer with two slow shocks in Petschek's model to the reconnection layer with a rotational discontinuity and a slow expansion wave in Levy et al's model. In the resistive MHD simulations, the rotational discontinuities are replaced by intermediate shocks or time-dependent intermediate shocks. In the hybrid simulations, the time-dependent intermediate shock quickly evolves to a steady rotational discontinuity, and the contact discontinuity does not exist. The magnetotail reconnection layer consists of two slow shocks. Hybrid simulations of slow shocks indicate that there exists a critical number,M _c, such that for slow shocks with an intermediate Mach numberM _IM _c, a large-amplitude rotational wavetrain is present in the downstream region. For slow shocks withM _I<M _c, the downstream wavetrain does not exist. Chaotic ion orbits in the downstream wave provide an efficient mechanism for ion heating and wave damping and explain the existence of the critical numberM _c in slow shocks.