Gravitational tractor for towing asteroids

We present a design concept for a spacecraft that can controllably alter the trajectory of an Earth-threatening asteroid by using gravity as a towline. The spacecraft hovers near the asteroid, with its thrusters angled outwards so that the exhaust does not impinge on the surface. This proposed deflection method is insensitive to the structure, surface properties and rotation state of the asteroid.     

The recent breakup of an asteroid in the main-belt region

The present population of asteroids in the main belt is largely the result of many past collisions. Ideally, the asteroid fragments resulting from each impact event could help us understand the large-scale collisions that shaped the planets during early epochs. Most known asteroid fragment families, however, are very old and have therefore undergone significant collisional and dynamical evolution since their formation. This evolution has masked the properties of the original collisions. Here we report the discovery of a family of asteroids that formed in a disruption event only 5.8 +/- 0.2 million years ago, and which has subsequently undergone little dynamical and collisional evolution. We identified 39 fragments, two of which are large and comparable in size (diameters of approximately 19 and approximately 14 km), with the remainder exhibiting a continuum of sizes in the range 2-7 km. The low measured ejection velocities suggest that gravitational re-accumulation after a collision may be a common feature of asteroid evolution. Moreover, these data can be used to check numerical models of larger-scale collisions.     

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。     

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.     

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.     

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.     

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.     

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).     

Retrograde spins of near-Earth asteroids from the Yarkovsky effect

Dynamical resonances in the asteroid belt are the gateway for the production of near-Earth asteroids (NEAs). To generate the observed number of NEAs, however, requires the injection of many asteroids into those resonant regions. Collisional processes have long been claimed as a possible source, but difficulties with that idea have led to the suggestion that orbital drift arising from the Yarkovsky effect dominates the injection process. (The Yarkovsky effect is a force arising from differential heating-the 'afternoon' side of an asteroid is warmer than the 'morning' side.) The two models predict different rotational properties of NEAs: the usual collisional theories are consistent with a nearly isotropic distribution of rotation vectors, whereas the 'Yarkovsky model' predicts an excess of retrograde rotations. Here we report that the spin vectors of NEAs show a strong and statistically significant excess of retrograde rotations, quantitatively consistent with the theoretical expectations of the Yarkovsky model.     

A reduced estimate of the number of kilometre-sized near-Earth asteroids

Near-Earth asteroids are small (diameters < 10 km), rocky bodies with orbits that approach that of the Earth (they come within 1.3 AU of the Sun). Most have a chance of approximately 0.5% of colliding with the Earth in the next million years. The total number of such bodies with diameters > 1 km has been estimated to be in the range 1,000-2,000, which translates to an approximately 1% chance of a catastrophic collision with the Earth in the next millennium. These numbers are, however, poorly constrained because of the limitations of previous searches using photographic plates. (One kilometre is below the size of a body whose impact on the Earth would produce global effects.) Here we report an analysis of our survey for near-Earth asteroids that uses improved detection technologies. We find that the total number of asteroids with diameters > 1 km is about half the earlier estimates. At the current rate of discovery of near-Earth asteroids, 90% will probably have been detected within the next 20 years.     

小行星35633和135356的历表研制及密近交会前后的轨道演化

在已知(349)Dembowska高精度质量的情况下,通过考虑密近交会改进了小行星35633和135356的历表.本文由蒙特卡罗方法给出了改进历表的不确定度,并利用姚安高精度望远镜的观测数据验证了历表改进的可靠性.与未考虑密近交会因素的JPL历表比较的结果表明,两种轨道之间瞬时根数的差值在密近交会时刻附近快速变化,这体现了(349)Dembowska在交会中对天体轨道演化的影响.尽管这种影响在一定时间内并不会产生显著的观测效应,但在历表研制中不予以考虑会显著降低外推历表位置的精度.     

Chaotic capture of Jupiter's Trojan asteroids in the early Solar System

Jupiter's Trojans are asteroids that follow essentially the same orbit as Jupiter, but lead or trail the planet by an angular distance of approximately 60 degrees (co-orbital motion). They are hypothesized to be planetesimals that formed near Jupiter and were captured onto their current orbits while Jupiter was growing, possibly with the help of gas drag and/or collisions. This idea, however, cannot explain some basic properties of the Trojan population, in particular its broad orbital inclination distribution, which ranges up to approximately 40 degrees (ref. 8). Here we show that the Trojans could have formed in more distant regions and been subsequently captured into co-orbital motion with Jupiter during the time when the giant planets migrated by removing neighbouring planetesimals. The capture was possible during a short period of time, just after Jupiter and Saturn crossed their mutual 1:2 resonance, when the dynamics of the Trojan region were completely chaotic. Our simulations of this process satisfactorily reproduce the orbital distribution of the Trojans and their total mass.     

Interplanetary dust from the explosive dispersal of hydrated asteroids by impacts

The Earth accretes about 30,000 tons of dust particles per year, with sizes in the range of 20-400 microm (refs 1, 2). Those particles collected at the Earth's surface--termed micrometeorites--are similar in chemistry and mineralogy to hydrated, porous meteorites, but such meteorites comprise only 2.8% of recovered falls. This large difference in relative abundances has been attributed to 'filtering' by the Earth's atmosphere, that is, the porous meteorites are considered to be so friable that they do not survive the impact with the atmosphere. Here we report shock-recovery experiments on two porous meteorites, one of which is hydrated and the other is anhydrous. The application of shock to the hydrated meteorite reduces it to minute particles and explosive expansion results upon release of the pressure, through a much broader range of pressures than for the anhydrous meteorite. Our results indicate that hydrated asteroids will produce dust particles during collisions at a much higher rate than anhydrous asteroids, which explains the different relative abundances of the hydrated material in micrometeorites and meteorites: the abundances are established before contact with the Earth's atmosphere.     

基于模糊关系的互补松弛定理

为完善和推广模糊线性规划对偶理论,在基于模糊关系的模糊线性规划(FLP)对偶理论的研究的基础上,分析对偶模糊线性(DFLP)最优解的概念,对经典LP对偶问题中的重要结果进行了推广.提出并推导证明了对偶模糊线性规划(DFLP)问题的对称性定理和互补松弛性定理.并举例说明该理论具有一定的应用价值,为存在于现实中的诸多模糊优化问题提供了理论基础.     

语言艺术与体育教学关系的探讨

在体育教学中，教师若能讲究语言的科学性和艺术性，就能使学生产生良好的心理定势和情感变化，也能激发学生的学习兴趣，教育学家告知：只有让学生处于积极的兴奋状态，处于轻松愉快的状态，他们才会积极地开动脑筋，认真思考，有效地掌握知识，因此，语言艺术在体育教学中的作用是显而见的，讨论了体育教师语言艺术的作用，基本要求及如何修练等，旨在为广大体育教师提供借鉴。     

A taxa-area relationship for bacteria

A positive power-law relationship between the number of species in an area and the size of that area has been observed repeatedly in plant and animal communities. This species-area relationship, thought to be one of the few laws in ecology, is fundamental to our understanding of the distribution of global biodiversity. However, such a relationship has not been reported for bacteria, and little is known regarding the spatial distribution of bacteria, relative to what is known of plants and animals. Here we describe a taxa-area relationship for bacteria over a scale of centimetres to hundreds of metres in salt marsh sediments. We found that bacterial communities located close together were more similar in composition than communities located farther apart, and we used the decay of community similarity with distance to show that bacteria can exhibit a taxa-area relationship. This relationship was driven primarily by environmental heterogeneity rather than geographic distance or plant composition.     

知识转化与企业创新绩效关系的实证研究

知识转化是知识管理的核心，是企业进行创新的动力源泉。构建了基于SECI模型的四个维度与企业创新绩效关系的理论模型，通过154家企业的调查样本，运用SEM 对模型及假设进行验证，揭示了知识转化对提升企业创新绩效的作用机理及微观路径。