An age-colour relationship for main-belt S-complex asteroids

Asteroid collisions in the main belt eject fragments that may eventually land on Earth as meteorites. It has therefore been a long-standing puzzle in planetary science that laboratory spectra of the most populous class of meteorite (ordinary chondrites, OC) do not match the remotely observed surface spectra of their presumed (S-complex) asteroidal parent bodies. One of the proposed solutions to this perplexing observation is that 'space weathering' modifies the exposed planetary surfaces over time through a variety of processes (such as solar and cosmic ray bombardment, micro-meteorite bombardment, and so on). Space weathering has been observed on lunar samples, in Earth-based laboratory experiments, and there is good evidence from spacecraft data that the process is active on asteroid surfaces. Here, we present a measurement of the rate of space weathering on S-complex main-belt asteroids using a relationship between the ages of asteroid families and their colours. Extrapolating this age-colour relationship to very young ages yields a good match to the colour of freshly cut OC meteorite samples, lending strong support to a genetic relationship between them and the S-complex asteroids.     

谈农用拖拉机常见故障的预防

本文叙述了农用拖拉机常见故障预防的知识。指出：拖拉机事故性损坏是可以 避 免的;自然损坏虽不能完全避免,但是只要掌握了零件的磨损规律,采取各种预防措施, 是可以大大减轻的。文章给出了零件磨损规律和建立计划预防修理制度的有关知识。     

多颗小行星探测顺序确定及轨迹优化

小行星探测日渐成为深空探测领域的一个研究热点。考虑小行星Kepler轨道以及小推力航天器的特点,从能量和相位的角度推导出多颗小行星探测顺序的确定准则,并利用优化算法对航天器的飞行轨迹进行了全局优化设计。算法在满足约束条件的前提下,使得航天器剩余质量与飞行时间的比值达到最大,并通过数值仿真算例验证了算法的可行性。结果表明:该算法综合利用遗传算法和局部优化算法具有精度高、计算简单的特点,可用于小行星探测的轨迹优化设计问题。     

可观测的引力双象

恒星作为引力透镜的重要性长期以来被忽视,已有文章指出,几乎所有河外天体都应由于某颗恒星的引力场对光线的偏折之故而形成双象。在大多数情况下,这样的双象的角距在毫角秒的数量级。有理由相信,当天文观测深入到毫角秒以下时,会出现好些奇特现象,特别是河外天体中两个小部分之间的表观速度很容易超过光速。     

黄土高原沟坡重力侵蚀的理论模型

重力侵蚀是黄土沟壑区土壤侵蚀的重要组成部分,其发生条件及侵蚀量受多种因素制约且具有一定随机性.本文通过运用水力学、土力学等力学方法对重力侵蚀主要影响因素进行分析,建立起沟坡重力侵蚀的概化力学模型,同时运用模糊及概率分析等数学方法将黄土沟坡的稳定问题转化为失稳概率,作为沟坡崩塌发生的预报条件,从而实现了考虑沟谷水流侧向切割,降雨入渗影响下的重力侵蚀模拟,为在黄土高原沟壑区进行水沙计算提供了基本方法.     

滚动松散物料重力透筛技术机理探讨

根据运动学原理，对双向运输筛分机物料的松散技术、透筛技术从理论上进行研究，运用实物实测试验的方法验证了筛分分级效果。该技术将筛分分级置于运输途中完成，将传统技术中运输和筛分两个截然不同的工序合并为一体，不仅起到经济、节能效果，而且加工能力、筛分质量、适用范围较传统技术有大幅度提高。     

Pre-biotic organic matter from comets and asteroids

Several authors have suggested that comets or carbonaceous asteroids contributed large amounts of organic matter to the primitive Earth, and thus possibly played a vital role in the origin of life. But organic matter cannot survive the extremely high temperatures (>10(4) K) reached on impact, which atomize the projectile and break all chemical bonds. Only fragments small enough to be gently decelerated by the atmosphere--principally meteors of 10(-12)-10(-6) g--can deliver their organic matter intact. The amount of such 'soft-landed' organic carbon can be estimated from data for the infall rate of meteoritic matter. At present rates, only approximately 0.006 g cm-2 intact organic carbon would accumulate in 10(8) yr, but at the higher rates of approximately 4 x 10(9) yr ago, about 20 g cm-2 may have accumulated in the few hundred million years between the last cataclysmic impact and the beginning of life. It may have included some biologically important compounds that did not form by abiotic synthesis on Earth.     

Compositional differences between meteorites and near-Earth asteroids

Understanding the nature and origin of the asteroid population in Earth's vicinity (near-Earth asteroids, and its subset of potentially hazardous asteroids) is a matter of both scientific interest and practical importance. It is generally expected that the compositions of the asteroids that are most likely to hit Earth should reflect those of the most common meteorites. Here we report that most near-Earth asteroids (including the potentially hazardous subset) have spectral properties quantitatively similar to the class of meteorites known as LL chondrites. The prominent Flora family in the inner part of the asteroid belt shares the same spectral properties, suggesting that it is a dominant source of near-Earth asteroids. The observed similarity of near-Earth asteroids to LL chondrites is, however, surprising, as this meteorite class is relatively rare ( approximately 8 per cent of all meteorite falls). One possible explanation is the role of a size-dependent process, such as the Yarkovsky effect, in transporting material from the main belt.     

改进的万有引力搜索算法

针对万有引力搜索算法对一些优化问题的搜索精度不高,容易出现早熟的问题,提出了改进的万有引力搜索算法.该算法借鉴生物界中雁群的飞行特征和加权平均法,扩大了搜索范围,加强了粒子间的合作与竞争.通过对6个基准函数的仿真测试,MATLAB仿真结果表明新算法能更有效地提高全局搜索能力.     

牵引车液力传动系统的设计计算

液力变矩器和柴油机的匹配是否得当,直接影响到整车的牵引性能和经济性能.分析了车辆液力变矩器的牵引特性及其与发动机的匹配特性,并进行了牵引特性的计算和热平衡计算,可以按此方案确定出合适的车辆液力传动系统.     

Spin vector alignment of Koronis family asteroids

Studies of asteroid families--groups of asteroids that formed from the fragmentation of larger bodies--are of broad interest to solar system researchers because they can provide insights into collisional processes, as well as the interior structures, strengths, and compositions of asteroids. It is generally accepted that members of the Koronis family were created by collisional disruption of a homogeneous parent body and therefore share the same formation age and subsequent collisional history. The temporal variations in observed brightness of the Koronis family members (a consequence of their rotation) are, however, larger than expected. Preferential alignment of spin vectors had been proposed as a possible explanation, but recent modelling predicted that family formation yields random spin vectors among the resulting fragments. Both hypotheses have been untested by observations. Here I show that the actual distribution of spin vectors among the largest members of the Koronis family falls within markedly nonrandom 'spin clusters'. Reconciling models of family formation and evolution with the unexpected alignments of spin obliquity and correlations with spin rates presents a new challenge in understanding asteroid collisional processes.     

重力加速度测量三种方法的比较研究

重力加速度的准确测量对于物理学、大地测量学、计量学来说,都有着十分重要的意义,而目前测量重力加速度的方法有许多种,在此就一些测量重力加速度的常用方法以及自行设计的方法进行探讨.研究结果表明:3种方法中操作比较简单的是自由落体法;但是从相对误差看,自由落体法的相对误差Eg=2.05%,单摆法的相对误差Eg=0.2515%,而平抛运动法的相对误差Eg=2.29%,即单摆法的相对误差最小.     

Efficient disruption of small asteroids by Earth's atmosphere

Accurate modelling of the interaction between the atmosphere and an incoming bolide is a complex task, but crucial to determining the fraction of small asteroids that actually hit the Earth's surface. Most semi-analytical approaches have simplified the problem by considering the impactor as a strengthless liquid-like object ('pancake' models), but recently a more realistic model has been developed that calculates motion, aerodynamic loading and ablation for each separate particle or fragment in a disrupted impactor. Here we report the results of a large number of simulations in which we use both models to develop a statistical picture of atmosphere-bolide interaction for iron and stony objects with initial diameters up to approximately 1 km. We show that the separated-fragments model predicts the total atmospheric disruption of much larger stony bodies than previously thought. In addition, our data set of >1,000 simulated impacts, combined with the known pre-atmospheric flux of asteroids with diameters less than 1 km, elucidates the flux of small bolides at the Earth's surface. We estimate that bodies >220 m in diameter will impact every 170,000 years.     

电动拖拉机车内电磁辐射环境仿真

针对电动拖拉机车内电磁辐射干扰源多、电磁环境复杂的问题,提出一种多软件联合仿真的方法.首先在Hypermesh中对三维模型进行几何处理,建立有限元模型,然后基于电磁辐射基本理论在HFSS和FEKO中建立主要干扰源的等效电磁模型,最后在软件FEKO中对某款电动拖拉机车内电磁辐射性能做了仿真分析,得到了100～550 MHz电动拖拉机车身的表面电流分布规律和驾驶舱内驾驶人员头部、胸部和脚部的电场强度分布情况.结果表明:拖拉机车身的表面电流具有局部突出的特性,在250 MHz左右车身前部表面电流最大,其值为0.50 A·m^-1;在450 MHz左右驾驶舱后部表面电流最大,其值为0.42 A·m^-1;拖拉机车内在脚部附近的电场强度最大,其值为1.79 V·m^-1,对应频率为122 MHz.     

引力场方程的新标架形式及定域化的引力场能量动量张量

本文通过引入标架空间定叉了引力场场强张量和引力场拉格朗日密度,根据最小作用量原理导出了引力场运动方程的一种新的半度规形式(或称标架形式)及具有标架空间和坐标空间的双重协变的引力场能量动量张量.我们用这种定域化的能量表达式和球对称真空外部场席瓦兹希德解(当β1+β2=0,B3=0时)计算出在r≥R区域中的球对称引力场的总能量为E=MC2 1-√1-2GM/C2R/1+√1-2GM/C2R.它把爱因斯坦引力理论作为一个特例(满足条件β1=β2=β3=0)包含其中,是对爱因斯坦度规引力理论的重大发展.本文通过求解球对称真空外部场解得到以下结论:满足条件β1+β2=0,β3=0时的球对称真空外部场解就是席瓦兹希德外部解,基于球对称真空外部场解的任何检验Einstein引力场方程的实验验证都无法确定Einstein引力场方程是唯一正确的.最后根据粒子在引力场中的运动方程确定了待定常数的值为β1=2β,β2=β3=0.本文得到的引力理论与平移引力理论具有相同的形式.本文建立的引力理论采用的几何是黎曼几何,没有采用平移引力理论中的weitzenbock几何,并且对其中的能量问题和待定常数问题作了更深入的讨论.