Thermo-electro-hydrodynamic instabilities in a dielectric liquid under microgravity

Linear stability analysis of a dielectric fluid confined in a cylindrical annulus of infinite length is performed under microgravity conditions. A radial temperature gradient and a high alternating electric field imposed over the gap induce an effective gravity that can lead to a thermal convection even in the absence of the terrestrial gravity. The linearized governing equations are discretized using a spectral collocation method on Chebyshev polynomials to compute marginal stability curves and the critical parameters of instability. The critical parameters are independent of the Prandtl number, but they depend on the curvature of the system. The critical modes are non-axisymmetric and are made of stationary helices.     

Monitoring physiological variables with membrane probes

Membrane probes are implantable devices, which can be used to sample from the interstitial fluid of the tissues in which they are implanted. Two types of membrane probes, one based on microdialysis and the other on ultrafiltration, were developed and tested in vitro for the following analytes: sodium, potassium, chloride, glucose and lactate. These membrane probes were then implanted subcutaneously in rats and used to monitor changes in interstitial analytes during the head-down tilt model of microgravity.     

星载GPS的毫米级编队卫星相对定位

在比较分析编队卫星相对定位与陆地相对定位技术的基础上,结合陆地相对定位技术和 卫星精密定轨技术提出了基于GPS进行编队卫星相对定位的方法及原理。文章采用2004年4月 1日到10日的GRACE卫星实测数据进行了相对定位计算,并采用KBR观测数据对本文相对定位 结果和JPL单独定轨结果进行了外部检核,检核结果表明：1. 与直接采用单独定轨结果相 比,该方法可以明显提高卫星的相对位置精度。2. 利用本文方法计算的两颗GRACE卫星相 对位置精度约为4.5 mm。
     

Giant polygons and mounds in the lowlands of Mars: signatures of an ancient ocean?

This paper presents the hypothesis that the well-known giant polygons and bright mounds of the martian lowlands may be related to a common process-a process of fluid expulsion that results from burial of fine-grained sediments beneath a body of water. Specifically, we hypothesize that giant polygons and mounds in Chryse and Acidalia Planitiae are analogous to kilometer-scale polygons and mud volcanoes in terrestrial, marine basins and that the co-occurrence of masses of these features in Chryse and Acidalia may be the signature of sedimentary processes in an ancient martian ocean. We base this hypothesis on recent data from both Earth and Mars. On Earth, 3-D seismic data illustrate kilometer-scale polygons that may be analogous to the giant polygons on Mars. The terrestrial polygons form in fine-grained sediments that have been deposited and buried in passive-margin, marine settings. These polygons are thought to result from compaction/dewatering, and they are commonly associated with fluid expulsion features, such as mud volcanoes. On Mars, in Chryse and Acidalia Planitiae, orbital data demonstrate that giant polygons and mounds have overlapping spatial distributions. There, each set of features occurs within a geological setting that is seemingly analogous to that of the terrestrial, kilometer-scale polygons (broad basin of deposition, predicted fine-grained sediments, and lack of significant horizontal stress). Regionally, the martian polygons and mounds both show a correlation to elevation, as if their formation were related to past water levels. Although these observations are based on older data with incomplete coverage, a similar correlation to elevation has been established in one local area studied in detail with newer higher-resolution data. Further mapping with the latest data sets should more clearly elucidate the relationship(s) of the polygons and mounds to elevation over the entire Chryse-Acidalia region and thereby provide more insight into this hypothesis.     

Right ventricular tissue Doppler assessment in space during circulating volume modification using the Braslet device

Introduction: This joint US–Russian work aims to establish a methodology for assessing cardiac function in microgravity in association with manipulation of central circulating volume. Russian Braslet-M (Braslet) occlusion cuffs were used to temporarily increase the volume of blood in the lower extremities, effectively reducing the volume in central circulation. The methodology was tested at the International Space Station (ISS) to assess the volume status of crewmembers by evaluating the responses to application and release of the cuffs, as well as to modified Valsalva and Mueller maneuvers. This case study examines the use of tissue Doppler (TD) of the right ventricular (RV) free wall. Results: Baseline TD of the RV free wall without Braslet showed early diastolic E′ (16 cm/s), late diastolic A′ (14 cm/s), and systolic S′ (12 cm/s) velocities comparable with those in normal subjects on Earth. Braslet application caused 50% decrease of E′ (8 cm/s), 45% increase of A′, and no change to S′. Approximately 8 beats after the Braslet release, TD showed E′ of 8 cm/s, A′ of 12 cm/s, and S′ of 13 cm/s. At this point after release, E′ did not recover to baseline values while l A′ and S′ did recover. The pre-systolic cross-sectional area of the internal jugular vein without Braslet was 1.07 cm², and 1.13 cm² 10 min after the Braslet was applied. The respective cross-sectional areas of the femoral vein were 0.50 and 0.54 cm². The RV myocardial performance Tei index was calculated by dividing the sum of the isovolumic contraction time and isovolumic relaxation time by the ejection time ((IVCT+IVRT)/ET); baseline and Braslet-on values for Tei index were 0.25 and 0.22, respectively. Braslet Tei indices are within normal ranges found in healthy terrestrial subjects and temporarily become greater than 0.4 during the dynamic Braslet release portion of the study. Conclusions: TD modality was successfully implemented in space flight for the first time. TD of RV revealed that the Braslet influenced cardiac preload and that fluid was sequestered in the lower extremity interstitial and vascular space after only 10 min of application. This report demonstrates that Braslet application has an effect on RV physiology in long-duration space flight based on TD, and that this effect is in part due to venous hemodynamics.     

由应力松弛试验数据确定松弛模量和蠕变柔量

用粘弹性有限元法计算药柱应力需要给出推进剂的松弛模量和蠕变柔量的Ｐｒｏｎｇ级精有达式，利用应力松弛模量的Ｐｒｏｎｇ级数模式，通过最小二乘法对由试验求得的应力松弛模量－时间曲线进行拟合，求出松弛模量的Ｐｒｏｎｇ级数中系数和指数，再利用蠕变柔量与松弛模量的关系式，求得蠕变柔量的Ｐｒｏｎｇ级数中的系数和指数，以此计算药柱的应力。     

Subgravity states: key to understanding the role of terrestrial gravity in human behaviour

The early orbital flights, although undertaken with considerable confidence, involved some uncertainty because of the impossibility of simulating under terrestrial conditions all of the conditions encountered in space. However, space-flight achievements by both the American astronauts and Soviet cosmonauts have firmly established that man, if appropriately selected, trained, and protected by suitable life-support systems, can perform efficiently for long periods of time in the hostile environment of space. We know that the side effects of vestibular origin pose important problems in space exploration, and the neurophysiological effects of any extensive, rapid adaptation processes in subgravity states have enabled a better understanding of man's compensatory capabilities. With the successful establishment of orbiting research laboratories, an unparalleled opportunity exists that will undoubtedly enable better understanding of the role played by gravity in normal terrestrial activity, not only as it affects our vestibular physiology, but also as it may or may not concern other systems and at different organizational levels in the body.     

基于直方图修改的卫星遥感图像无损隐藏传输

针对星上低速率数据的传输问题,提出了一种基于直方图修改技术的卫星遥感图像无损隐藏传输方法。该方法通过对星上高速率遥感图像相邻像素差的直方图进行修改,将低速率数据嵌入到原始高速率遥感载体图像中,并利用卫星高速数传系统进行下传。地面接收端可以从载体图像中正确提取低速率数据,并无损恢复原始高速率遥感图像数据。该方法在不增加卫星数传系统复杂度和信息传输速率的前提下,提高了卫星数传系统的利用率,增强了数据传输的隐蔽性。实验结果表明,本文算法在保证良好的不可见性的情况下,获得了较高的纯载荷嵌入容量。与其它无损嵌入方法相比,在峰值信噪比和纯载荷嵌入容量方面都有很大的优势。     

基于北斗Ka星间链路的地面用户导航方法

针对导航系统L频段信号易受到有意或无意的干扰和欺骗,而导致地面区域性导航服务性能下降甚至失效的问题,提出了一种利用北斗Ka星间链路信号为地面用户提供导航服务的方法。首先,对该方法的可行性进行了研究,并给出了星间链路时分体制下的用户测距模型;然后,提出了基于时钟模型和惯导信息的测距值历元归算方法,并推导了基于北斗星间链路测距值的地面用户实时定位算法;最后,通过数值仿真分析了不同因素对算法性能的影响。仿真结果表明,该方法定位精度可达2.0 m以内,能够在一定程度上弥补L频段导航信号区域性失效带来的缺失。     

Exchange of meteorites (and life?) between stellar systems

It is now generally accepted that meteorite-size fragments of rock can be ejected from planetary bodies. Numerical studies of the orbital evolution of such planetary ejecta are consistent with the observed cosmic ray exposure times and infall rates of these meteorites. All of these numerical studies agree that a substantial fraction (up to one-third) of the ejecta from any planet in our Solar System is eventually thrown out of the Solar System during encounters with the giant planets Jupiter and Saturn. In this paper I examine the probability that such interstellar meteorites might be captured into a distant solar system and fall onto a terrestrial planet in that system within a given interval of time. The overall conclusion is that it is very unlikely that even a single meteorite originating on a terrestrial planet in our solar system has fallen onto a terrestrial planet in another stellar system, over the entire period of our Solar System's existence. Although viable microorganisms may be readily exchanged between planets in our solar system through the interplanetary transfer of meteoritic material, it seems that the origin of life on Earth must be sought within the confines of the Solar System, not abroad in the galaxy.     

Attitudes of UK and Australian farmers towards monitoring activity with satellite technologies: Lessons to be learnt

Governments are increasingly using satellite technologies to check for compliance with legislation, e.g. to verify that farmers are complying with environmental legislation on vegetation clearance in Australian states. As the detail of what can be seen by satellite technologies continues to improve and they are likely to become ever more attractive to those monitoring compliance with numerous different laws, it is important to consider the attitudes of those groups currently being monitored this way. Two surveys, the first of their kind internationally, were undertaken in the UK and Australia to assess attitudes in regulated communities (here farmers) where satellite monitoring was already being used. The aim was to understand attitudes to this method of monitoring, including its perceived benefits and drawbacks. Many of the farmers surveyed were either positive, or ambivalent, about satellite monitoring taking place. Only about a quarter of Australian farmers and a third of UK farmers were against being monitored this way. Large numbers actually wanted satellite monitoring to be used as a method of checking compliance, although if something was detected by a satellite many wanted any subsequent investigation to be done on the ground by humans. There were high levels of support for the use of satellite technologies because these were seen to be fairer, and more equitable than conventional methods, but concerns over how satellite monitoring might affect privacy and the technology not being used properly, or producing inaccurate results were expressed. Communication between regulator and regulated should be encouraged wherever possible, because many of the concerns of farmers and other potential regulated groups might be reduced if more information was given to them.     

空间飞行器推进系统的故障检测

文中采用基于人工智能条件下的专家系统知识，应用门限算法进行故障特性提取和相应的故障推理机制研究，在由大量小发动机组成的空间飞行器推进系统实验中进行应用，通过已有的实验数据，离线回放表明此方法具有实时检测功能，可以解决工程实际问题。     

An extensive phase space for the potential martian biosphere

We present a comprehensive model of martian pressure-temperature (P-T) phase space and compare it with that of Earth. Martian P-T conditions compatible with liquid water extend to a depth of ～310?km. We use our phase space model of Mars and of terrestrial life to estimate the depths and extent of the water on Mars that is habitable for terrestrial life. We find an extensive overlap between inhabited terrestrial phase space and martian phase space. The lower martian surface temperatures and shallower martian geotherm suggest that, if there is a hot deep biosphere on Mars, it could extend 7 times deeper than the ～5?km depth of the hot deep terrestrial biosphere in the crust inhabited by hyperthermophilic chemolithotrophs. This corresponds to ～3.2% of the volume of present-day Mars being potentially habitable for terrestrial-like life.     

Abiotic nitrogen fixation on terrestrial planets: reduction of NO to ammonia by FeS

Understanding the abiotic fixation of nitrogen and how such fixation can be a supply of prebiotic nitrogen is critical for understanding both the planetary evolution of, and the potential origin of life on, terrestrial planets. As nitrogen is a biochemically essential element, sources of biochemically accessible nitrogen, especially reduced nitrogen, are critical to prebiotic chemistry and the origin of life. Loss of atmospheric nitrogen can result in loss of the ability to sustain liquid water on a planetary surface, which would impact planetary habitability and hydrological processes that shape the surface. It is known that NO can be photochemically converted through a chain of reactions to form nitrate and nitrite, which can be subsequently reduced to ammonia. Here, we show that NO can also be directly reduced, by FeS, to ammonia. In addition to removing nitrogen from the atmosphere, this reaction is particularly important as a source of reduced nitrogen on an early terrestrial planet. By converting NO directly to ammonia in a single step, ammonia is formed with a higher product yield (~50%) than would be possible through the formation of nitrate/nitrite and subsequent conversion to ammonia. In conjunction with the reduction of NO, there is also a catalytic disproportionation at the mineral surface that converts NO to NO? and N?O. The NO? is then converted to ammonia, while the N?O is released back in the gas phase, which provides an abiotic source of nitrous oxide.     

A micro-gravity simulation of the Marangoni convection

An experimental verification of Marangoni convection in the liquid inter-space between two-coaxial discs is carried out at reduced gravity effect using small Bond's number obtained by choice of small characteristical diameter. Silicon oil is used as working fluid. The upper or lower disc can be heated electrically. The flow is visualized by illuminating fine powder of Titandioxide in the fluid with a vertical “light cut” of about 0.1 mm thickness, which is produced by a laser with a cylindrical glass rod and a microscope objective. Photographs and moving pictures are taken from a TV monitor. From these the vortex configuration and the velocity distribution can be determined, which would be expected for the Marangoni convection in the zero-g condition, for example in the spacelab.     

State propagation in an uncertain asteroid gravity field

Various spacecraft have been and will be sent to asteroids to characterize them. Generally, an asteroid's gravity field is very irregular and not accurately known when compared to the gravity field of a major planet, Earth in particular. It has been well studied that the irregularity significantly affects the trajectory of an orbiting spacecraft, and causes it to impact or to escape from the asteroid. Complementary to that, this paper focuses on the influence of the limited knowledge of this gravity field on the evolution of the spacecraft's orbit. It develops a general method by which this influence can be quantified. This method comprises specific Monte Carlo simulations with a discrete set of low-altitude orbits, taking into account the uncertainties in the gravity-field parameters. For illustration purposes, it is applied to two different asteroids. Already after three revolutions, the gravity-field uncertainties propagate to significant position uncertainties; this specifically holds for prograde orbits, and around the smaller asteroid. Applying this robust and accurate method helps mission designers and planners to assess the risk posed by gravity uncertainties, and take appropriate measures such as choosing the most favorable orbital geometries and/or lowering the orbit more slowly.     

充液航天器变质量液体大幅晃动的SPH分析方法

本文基于非惯性系下的光滑粒子流体动力学(SPH)方法,在以虚粒子设置缓冲层的开口边界处理方法基础上,提出一种流出流量可控的出口边界处理方法,能够根据当前时刻航天器的姿态信息和充液比,计算该动力学时间步下变质量液体晃动对航天器产生的作用力和作用力矩,使得航天器系统动力学的闭环仿真成为可能.最后,通过与计算流体动力学(CF...     

High-resolution simulations of the final assembly of Earth-like planets. 2. Water delivery and planetary habitability

The water content and habitability of terrestrial planets are determined during their final assembly, from perhaps 100 1,000-km "planetary embryos " and a swarm of billions of 1-10-km "planetesimals. " During this process, we assume that water-rich material is accreted by terrestrial planets via impacts of water-rich bodies that originate in the outer asteroid region. We present analysis of water delivery and planetary habitability in five high-resolution simulations containing about 10 times more particles than in previous simulations. These simulations formed 15 terrestrial planets from 0.4 to 2.6 Earth masses, including five planets in the habitable zone. Every planet from each simulation accreted at least the Earth's current water budget; most accreted several times that amount (assuming no impact depletion). Each planet accreted at least five water-rich embryos and planetesimals from the past 2.5 astronomical units; most accreted 10-20 water-rich bodies. We present a new model for water delivery to terrestrial planets in dynamically calm systems, with low-eccentricity or low-mass giant planets-such systems may be very common in the Galaxy. We suggest that water is accreted in comparable amounts from a few planetary embryos in a " hit or miss " way and from millions of planetesimals in a statistically robust process. Variations in water content are likely to be caused by fluctuations in the number of water-rich embryos accreted, as well as from systematic effects, such as planetary mass and location, and giant planet properties.     

高度-速度剖面内再入轨迹快速规划

提出一种升力式再入航天器进入稠密大气后的轨迹规划方法。在预先设定攻角剖面的前提下,利用路径约束(驻点热流、动压和过载)在高度-速度(H-V)剖面内直接获得轨迹下边界;利用终端约束确定以轨迹下边界为基准的高度增量,进而通过下边界与高度增量的加和形成满足要求的再入轨迹。其中,增量的形式选取为分段二次型函数,其大小可通过割线法快速获得。倾斜角大小可根据纵向动力学方程反解得到,其方向依据航向误差角走廊确定。通过对典型工况的仿真,结果表明所提方法能够快速规划出再入轨迹,且适应性好。     

The biological terraforming of Mars: planetary ecosynthesis as ecological succession on a global scale

Mars is bitterly cold and dry, but robotic spacecraft have returned abundant data that indicate Mars once had a much warmer and wetter climate in the past. These data, the basis of the search for past or present life on Mars, suggest the possibility of returning Mars to its previous climate by global engineering techniques. Greenhouse gases, such as perfluorocarbons, appear to be the best method for warming Mars and increasing its atmospheric density so that liquid water becomes stable. The process of making Mars habitable for terrestrial organisms is called terraforming or planetary ecosynthesis. The process of introducing terrestrial ecosystems to Mars can be compared with a descent down a high mountain. Each drop in elevation results in a warmer, wetter climate and more diverse biological community. Beginning with a polar desert, the sequence of ecosystems passes through tundra, boreal forest, and temperate ecosystems where moisture determines the presence of desert, grassland, or forest. This model suggests a sequence for the introduction of ecosystems to Mars and the communities to search for potential colonizing species for Mars.