小天体伴飞的常推力控制

小天体探测的轨道控制和保持非常重要.深空探测中常采用推力大小不可变的小推力发动机进行轨道控制,本文研究利用常推力实现小天体伴飞的控制方法.同时考虑太阳和小天体的引力,提出一种常推力实现伴飞位置保持的阈值控制方法,当误差超过阈值时进行主动控制.该控制方法实现探测器的位置保持需要控制周期长,消耗推进剂少,实现简单.     

Shoemaker crater as the source of most ejecta blocks on the asteroid 433 Eros

The loose material--regolith--on the surfaces of asteroids is thought to represent ballistically emplaced ejecta from impacts but the identification of source craters and the detailed study of the regolith modification have been hampered by the limited spatial resolution and area coverage of the few asteroids imaged by spacecraft. Here we report the results of global mapping of the asteroid 433 Eros from high-resolution images obtained by the NEAR-Shoemaker spacecraft. Based on the images and ejecta-emplacement models, we suggest that most large ejecta blocks on Eros originate from a relatively young 7.6-km-diameter crater. A large fraction of the ejecta from impacts pre-dating that crater has apparently been buried or eroded. The images also show evidence for the action of a variety of sorting environments for regolith particles after they are deposited on the surface.     

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.     

A collision in 2009 as the origin of the debris trail of asteroid P/2010 A2

The peculiar object P/2010?A2 was discovered in January 2010 and given a cometary designation because of the presence of a trail of material, although there was no central condensation or coma. The appearance of this object, in an asteroidal orbit (small eccentricity and inclination) in the inner main asteroid belt attracted attention as a potential new member of the recently recognized class of main-belt comets. If confirmed, this new object would expand the range in heliocentric distance over which main-belt comets are found. Here we report observations of P/2010?A2 by the Rosetta spacecraft. We conclude that the trail arose from a single event, rather than a period of cometary activity, in agreement with independent results. The trail is made up of relatively large particles of millimetre to centimetre size that remain close to the parent asteroid. The shape of the trail can be explained by an initial impact ejecting large clumps of debris that disintegrated and dispersed almost immediately. We determine that this was an asteroid collision that occurred around 10 February 2009.     

The landing of the NEAR-Shoemaker spacecraft on asteroid 433 Eros

The NEAR-Shoemaker spacecraft was designed to provide a comprehensive characterization of the S-type asteroid 433 Eros (refs 1,2,3), an irregularly shaped body with approximate dimensions of 34 x 13 x 13 km. Following the completion of its year-long investigation, the mission was terminated with a controlled descent to its surface, in order to provide extremely high resolution images. Here we report the results of the descent on 12 February 2001, during which 70 images were obtained. The landing area is marked by a paucity of small craters and an abundance of 'ejecta blocks'. The properties and distribution of ejecta blocks are discussed in a companion paper. The last sequence of images reveals a transition from the blocky surface to a smooth area, which we interpret as a 'pond'. Properties of the 'ponds' are discussed in a second companion paper. The closest image, from an altitude of 129 m, shows the interior of a 100-m-diameter crater at 1-cm resolution.     

2018年深空探测热点回眸

 深空探测指人类航天器离开近地轨道、进入太阳系空间和宇宙空间，对地球以外天体（月球及以远天体）或空间环境开展的科学探测。2018年，国际深空探测叠彩纷呈：中国“嫦娥四号”成功实现国际首次月球背面软着陆并将开展巡视勘察；美国“洞察号”探测器登陆火星；向太阳系空间进发，朝向日心方向，欧洲空间局和日本合作研制的BeipiColombo探测器正飞向水星、美国“帕克号”探测器开启“史诗级”旅行去“触摸太阳”，远离日心方向，“新视野号”成功飞掠柯伊伯带的小行星“天涯海角”、“旅行者2号”突破日球层顶；美国“奥西里斯-REx”和日本“隼鸟2号”顺利抵达各自目标小行星执行采样任务。2018年，月球表面存在水冰、火星发现有机分子、太阳系边际再抵近等发现或突破对于探寻生命起源、太阳系起源和演化，拓展人类知识体系具有重要意义。     

Rotational breakup as the origin of small binary asteroids

Asteroids with satellites are observed throughout the Solar System, from subkilometre near-Earth asteroid pairs to systems of large and distant bodies in the Kuiper belt. The smallest and closest systems are found among the near-Earth and small inner main-belt asteroids, which typically have rapidly rotating primaries and close secondaries on circular orbits. About 15 per cent of near-Earth and main-belt asteroids with diameters under 10 km have satellites. The mechanism that forms such similar binaries in these two dynamically different populations was hitherto unclear. Here we show that these binaries are created by the slow spinup of a 'rubble pile' asteroid by means of the thermal YORP (Yarkovsky-O'Keefe-Radzievskii-Paddack) effect. We find that mass shed from the equator of a critically spinning body accretes into a satellite if the material is collisionally dissipative and the primary maintains a low equatorial elongation. The satellite forms mostly from material originating near the primary's surface and enters into a close, low-eccentricity orbit. The properties of binaries produced by our model match those currently observed in the small near-Earth and main-belt asteroid populations, including 1999 KW(4) (refs 3, 4).     

Seismic resurfacing by a single impact on the asteroid 433 Eros

Impact cratering creates a wide range of topography on small satellites and asteroids. The population of visible craters evolves with impacts, and because there are no competing endogenic processes to modify the surface, determining the various ways younger craters add to or subtract from the population is a fundamental aspect of small-body geology. Asteroid 433 Eros, the most closely studied small body, has regions of substantially different crater densities that remain unexplained. Here we show that the formation of a relatively young crater (7.6 km in diameter) resulted in the removal of other craters as large as 0.5 km over nearly 40 percent of the asteroid. Burial by ejecta cannot explain the observed pattern of crater removal. The limitation of reduced crater density to a zone within a particular straight-line distance through the asteroid from the centre of the large crater suggests degradation of the topography by seismic energy released during the impact. Our observations indicate that the interior of Eros is sufficiently cohesive to transmit seismic energy over many kilometres, and the outer several tens of metres of the asteroid must be composed of relatively non-cohesive material.     

红外地平仪外热流计算

红外地平仪部分凸出于航天器外表面．除受到太阳辐射、地球反照和红外辐射外,还受到航天器外表面的反射辐射．文中在对包括红外地平仪外表面在内的封闭系统进行辐射分析的基础上,得到红外地平仪外热流的空间有效辐射角系数计算公式;采用蒙特卡洛法,计算了某航天器两个位于不同外表面的红外地平议外凸圆柱体所受的外热流,并讨论了反射辐射对红外地子仪所受外热流的影响     

航天器交汇对接电位控制研究与航天器电位监测

 低轨航天器间的电位差异是航天器交汇对接面临的一个重大安全问题,分析了低轨航天器在电离层等离子体中的充电机制,并给出了等效物理电路模型。在此基础上分析了国际太空站的主动电位控制原理和方法,并针对航天器交汇对接中的电位控制问题给出了2种新的解决方案。最后,提出了航天器交汇对接中的电位监测方案,即由朗缪尔探针和表面电位探测器组成航天器电位监测包。     

The binary Kuiper-belt object 1998 WW31

The recent discovery of a binary asteroid during a spacecraft fly-by generated keen interest, because the orbital parameters of binaries can provide measures of the masses, and mutual eclipses could allow us to determine individual sizes and bulk densities. Several binary near-Earth, main-belt and Trojan asteroids have subsequently been discovered. The Kuiper belt-the region of space extending from Neptune (at 30 astronomical units) to well over 100 AU and believed to be the source of new short-period comets-has become a fascinating new window onto the formation of our Solar System since the first member object, not counting Pluto, was discovered in 1992 (ref. 13). Here we report that the Kuiper-belt object 1998 WW31 is binary with a highly eccentric orbit (eccentricity e approximately 0.8) and a long period (about 570 days), very different from the Pluto/Charon system, which was hitherto the only previously known binary in the Kuiper belt. Assuming a density in the range of 1 to 2 g cm-3, the albedo of the binary components is between 0.05 and 0.08, close to the value of 0.04 generally assumed for Kuiper-belt objects.     

我国小行星探测目标分析与电推进轨道设计

近几年,世界各航天大国陆续实施了小行星探测计划.近地小行星也是我国下一步深空探测的重要目标,国内航天相关单位正在积极开展近地小行星探测的前期任务论证与规划工作.以此为背景,研究了电推进方式探测近地小行星的目标选择与轨道设计问题.首先分析了近地小行星探测的科学和技术目标,结合我国技术水平的发展现状,给出了6颗适合作为探测目标的近地小行星.搜索了2016年至2020年之间探测每颗可能目标的发射窗口.为了增加探测任务的科学回报,特别关注了多目标、多任务的近地小行星探测,推荐了一次探测多个有价值目标的可行多任务探测方案：Earth出发-Nereus飞越-Apophis飞越-1999JU3交会.基于脉冲估算结果设计电推进轨道,将中途多任务探测作为内点约束整体优化小推力转移轨道,采用间接法求解燃料最优控制问题得到了小推力的最优轨迹.最后给出了推荐方案的详细飞行程序.     

充液航天器姿态稳定分析的Casimir方法

充液航天器中的液体燃料晃动将可能导致航天器姿态不稳定性现象的发生．本文采用哈密顿动力学方法研究了半充液航天器姿态运动的稳定性问题．首先将晃动液体等效为弹簧质量块力学模型,建立了液体晃动与航天器姿态多体耦合动力学系统的哈密顿方程,并进一步推导了与耦合动力学系统相关的Casimir函数;借助于Casimir函数并采用李亚普诺夫稳定性理论推导出耦合系统的稳定性和非稳定性条件,最后给出了数值仿真结果及相关结论．     

Acceleration of the rotation of asteroid 1862 Apollo by radiation torques

The anisotropic reflection and thermal re-emission of sunlight from an asteroid's surface acts as a propulsion engine. The net propulsion force (Yarkovsky effect) changes the orbital dynamics of the body at a rate that depends on its physical properties; for irregularly shaped bodies, the propulsion causes a net torque (the Yarkovsky-O'Keefe-Radzievskii-Paddack or YORP effect) that can change the object's rotation period and the direction of its rotation axis. The Yarkovsky effect has been observed directly, and there is also indirect evidence of its role in the orbital evolution of asteroids over long time intervals. So far, however, only indirect evidence exists for the YORP effect through the clustering of the directions of rotation axes in asteroid families. Here we report a change in the rotation rate of the asteroid 1862 Apollo, which is best explained by the YORP mechanism. The change is fairly large and clearly visible in photometric lightcurves, amounting to one extra rotation cycle in just 40 years even though Apollo's size is well over one kilometre. This confirms the prediction that the YORP effect plays a significant part in the dynamical evolution of asteroids.     

基于新型双曲正切趋近律的固定/有限时间姿态控制

本文研究了基于一种新型双曲正切趋近律和非奇异固定时间终端滑模面的固定/有限时间姿态控制方法. 对没有外部干扰的航天器姿态控制问题，本文基于双曲正切函数提出了一种新型的固定时间趋近律，该趋近律只需调节控制参数就可保证滑模变量在固定时间内收敛于原点，接着结合非奇异终端滑模面设计了固定时间姿态控制器，保证航天器姿态在固定时间内收敛于原点. 对存在未知外部干扰的情况，设计了双层自适应有限时间滑模观测器估计外部扰动，基于观测器的输出设计了基于非奇异固定时间滑模面与新型双曲趋近律的控制器来对扰动进行补偿. 数值仿真验证了所提控制方法的有效性.      

High-resolution subsurface water-ice distributions on Mars

Theoretical models indicate that water ice is stable in the shallow subsurface (depths of <1-2 m) of Mars at high latitudes. These models have been mainly supported by the observed presence of large concentrations of hydrogen detected by the Gamma Ray Spectrometer suite of instruments on the Mars Odyssey spacecraft. The models and measurements are consistent with a water-ice table that steadily increases in depth with decreasing latitude. More detailed modelling has predicted that the depth at which water ice is stable can be highly variable, owing to local surface heterogeneities such as rocks and slopes, and the thermal inertia of the ground cover. Measurements have, however, been limited to the footprint (several hundred kilometres) of the Gamma Ray Spectrometer suite, preventing the observations from documenting more detailed water-ice distributions. Here I show that by observing the seasonal temperature response of the martian surface with the Thermal Emission Imaging System on the Mars Odyssey spacecraft, it is possible to observe such heterogeneities at subkilometre scale. These observations show significant regional and local water-ice depth variability, and, in some cases, support distributions in the subsurface predicted by atmospheric exchange and vapour diffusion models. The presence of water ice where it follows the depth of stability under current climatic conditions implies an active martian water cycle that responds to orbit-driven climate cycles. Several regions also have apparent deviations from the theoretical stability level, indicating that additional factors influence the ice-table depth. The high-resolution measurements show that the depth to the water-ice table is highly variable within the potential Phoenix spacecraft landing ellipses, and is likely to be variable at scales that may be sampled by the spacecraft.     

载人飞船遭遇M/OD失效风险评估及其防护设计

 采用自主开发的M/OD风险评估软件系统,对某载人飞船遭遇M/OD的失效风险进行评估分析,给出了不同舱壁厚度下载人飞船遭遇M/OD的失效风险分析结果及其表面失效数分布。载人飞船舱壁厚度为0.6cm时,遭遇M/OD碰撞的非失效概率为96.447%,而当舱壁厚度减小为0.3cm时,非失效概率仅为9.460%。由于空间碎片具有方向性,使得载人飞船遭遇空间碎片时,其两侧失效风险最大,微流星体的任意分布性使其失效数呈带状分布。本文还对载人飞船进行了防护结构设计,给出了不同防护下载人飞船失效风险分析结果。采用与0.6cm厚舱壁面密度相同的Whipple和SW防护结构进行防护时,载人飞船非失效概率分别为99.704%和99.924%。若采用波纹角为30°和60°的CSW防护结构,则其非失效概率可分别提高到99.939%和99.995%,显著降低了载人飞船失效风险。     

Origin of asteroid rotation rates in catastrophic impacts

The rotation rates of asteroids, which are deduced from periodic fluctuations in their brightnesses, are controlled by mutual collisions. The link between asteroid spin and collision history is usually made with reference to impact experiments on centimetre-scale targets, where material strength governs the impact response. Recent work, however, indicates that for objects of the size of most observed asteroids (> or = 1 km in diameter), gravity rather than intrinsic strength controls the dynamic response to collisions. Here we explore this idea by modelling the effect of impacts on large gravitating bodies. We find that the fraction of a projectile's angular momentum that is retained by a target asteroid is both lower and more variable than expected from laboratory experiments, with spin evolution being dominated by 'catastrophic' collisions that eject approximately 50 per cent of the target's mass. The remnant of an initially non-rotating silicate asteroid that suffers such a collision rotates at a rate of approximately 2.9 per day, which is close to the observed mean asteroid rotation rate of approximately 2.5 d-1. Moreover, our calculations suggest that the observed trend in the mean spin frequency for different classes of asteroids (2.2 d-1 for C-type asteroids, 2.5 d-1 for S-type, and 4.0 d-1 for M-type) is due to increasing mean density, rather than increasing material strength.     

小行星群和Kirkwood空隙分布特征的探讨

引进小行星径向波函数Ｒｎｌ（ｒ）及划分小行星族的参考轨道根数（ａ，ｅ和ｉ），证明了小行星轨道半长径分布的３／２、４／３和１／１通约处是小行星径向概率最大的位置，而概率的零点与小行星轨道半长径分布的Ｋｉｒｋｗｏｏ空隙相对应，零点平移的位置，其平均运动的通约数为４／１、７／２、３／１、５／２、７／３、２／１。     

低重环境航天器贮箱内三维液体晃动数值模拟

为了研究低重环境下航天器贮箱内液体晃动的特性,采用了任意Lagrange-Euler有限元方法描述贮箱内不可压粘性液体的运动。用Laplace-Young表面张力公式将表面张力效应引入自由液面边界条件,采用最小二乘数值逼近方法拟合自由液面平均曲率,给出了含表面张力的动力学边界条件的数值计算形式。数值模拟显示:低重环境下,由于表面张力效应,液面平衡位置会升高;该平衡液面与常重情况下的平衡液面有明显不同,可以在任何位置以不同的形状出现。