基于嵌套网格的舰载直升机流场仿真及风限图计算

为保证舰载直升机的安全,本文基于嵌套网格方法,针对CG-47提康德罗加级巡洋舰搭载UH-60"黑鹰"直升机的机舰组合进行了流场仿真。研究了此组合在不同风向角及风速下的着舰流场,并结合飞行力学模型计算了直升机操纵量和姿态角。根据安全着舰判据,绘制了此组合的理论风限图。结果表明:滚转角及周期变距操纵量均随来流速度增加,俯仰角则受到来流和舰上建筑的多重影响。风向角越小,最大着舰速度越大,且总体左侧大于右侧。     

爆炸破片作用下 舰载导弹战斗部的安全性数值模拟

文章主要针对爆炸破片作用下,垂直发射系统中舰载导弹战斗部的安全性进行分析,分别讨论了破片的质量、速度、侵彻角度和破片的数量等因素作用下,舰载导弹外防护设置以及战斗部的响应特性。结果表明:在临界起爆条件附近,炸药的点火增长对撞击速度的变化很敏感。同时,入射角对其是否引爆威胁战斗部的影响也很大;当两破片间距小于破片直径时,破片撞击战斗部形成的冲击波会相互叠加,压力峰值增大,更容易引爆战斗部,而当两破片间距大于1.7倍的破片直径时,此时两破片产生的冲击波叠加效应降低。     

时空守恒元和解元方法的爆震波一维数值模拟

运用基元化学反应模型和流体力学的基本原理，建立了脉冲爆震发动机一维非定常反应流数学模型。应用一种改进的时空守恒元和解元(CESE)方法建立控制方程的差分格式，针对化学反应源项的刚性问题，在对非线性源项进行线性化处理的基础上，应用隐式梯形方法实现源项的积分。对氢氧爆震波的形成和传播过程进行数值计算，结果表明，应用CESE方法和基元化学反应模型能够成功地模拟氢氧爆震波的精细结构。     

A few metrological aspects of the Gaia mission

The ESA space astrometry mission Gaia is designed to measure the positions, parallaxes and proper motions of more than one billion stars of our Galaxy brighter than 20 magnitude. The expected astrometric accuracies are in the range 7–25 μas for the point-like sources down to 15 mag. To achieve this staggering performance, several issues of highly accurate metrology must be solved and implemented on the spacecraft. In this paper, I discuss first some constraining principles to perform global astrometry in space, and then a couple of examples of the metrological issues currently faced by the design or to be encountered during the operations. One concerns the optimisation of the sky coverage with a scanning instrument like Gaia, and the other deals with the instrument stability and how the stringent requirements are met in practice.     

扭矩扳子检定装置量值传递相关问题探讨

通过对扭矩量值传递中有关器具工作原理及工作时受力的分析,指出了用扭矩扳子检定装置检定扭矩扳子时检定结果难以一致的原因,给出了解决办法,并进行了验证。     

疲劳裂纹扩展随机过程的统计分析

证明了两种疲劳裂纹扩展随机模型 (即以时间为参量的随机过程模型和以裂纹长度为参量的随机过程模型 )在描述裂纹扩展随机过程方面的统一性。建立了由试验数据估计平稳对数正态随机过程相关参数的方法,可以直接由试验数据估计疲劳裂纹扩展随机过程的相关参数。针对 4种机型含紧固孔试件谱载荷下的疲劳裂纹扩展试验数据,给出了用文中方法估计的相关参数和用随机模拟法估算的置信区间。     

Application of CCD drift-scan photoelectric technique on monitoring GEO satellites

Geosynchronous Earth Orbit (GEO) satellites are widely used because of their unique characteristics of high-orbit and remaining permanently in the same area of the sky. Precise monitoring of GEO satellites can provide a key reference for the judgment of satellite operation status, the capture and identification of targets, and the analysis of collision warning. The observation using ground-based optical telescopes plays an important role in the field of monitoring GEO targets. Different from distant celestial bodies, there is a relative movement between the GEO target and the background reference stars, which makes the conventional observation method limited for long focal length telescopes. CCD drift-scan photoelectric technique is applied on monitoring GEO targets. In the case of parking the telescope, the good round images of the background reference stars and the GEO target at the same sky region can be obtained through the alternating observation of CCD drift-scan mode and CCD stare mode, so as to improve the precision of celestial positioning for the GEO target. Observation experiments of GEO targets were carried out with 1.56-meter telescope of Shanghai Astronomical Observatory. The results show that the application of CCD drift-scan photoelectric technique makes the precision of observing the GEO target reach the level of 0.2″, which gives full play to the advantage of the long focal length of the telescope. The effect of orbit improvement based on multi-pass of observations is obvious and the prediction precision of extrapolating to 72-h is in the order of several arc seconds in azimuth and elevation.     

关于地球卫星运动中的坐标系附加摄动问题

关于卫星运动中的坐标系附加摄动，早期是从两种赤道坐标系中卫星轨道根数的差别采用大量球面三角公式的方法导出的，本文将改用与当今高精度数值解中的坐标转换关系，在岁差章动等参数完全一致的情况下，简要清晰地导出相应的坐标系附加摄动解，既容易被读者接受，又便于与对应的数值解进行比对。     

A Detailed Analysis of the Operational Orbit of the Hipparcos Satellite

An analysis of the orbital evolution of the ESA's Hipparcos satellite is presented. Hipparcos operated between August 1989 and March 1993 in a highly elliptical orbit: a geostationary transfer orbit with increased perigee height. The requirements of the scientific mission included high accuracy knowledge of the position and velocity vectors of the spacecraft as a function of time. Through a study of the variations in the total orbital energy, the loss of energy during the mission as a result of non-conservative forces is recovered. These are explained as largely due to atmospheric drag during perigee passages. Apparent variations in the drag coefficient are in agreement with orientation variations of the satellite during those perigee passages. Two different models used for calculating the atmospheric drag give significantly different results, confirming earlier findings by other users of those models. This revised version was published online in August 2006 with corrections to the Cover Date.