Ion Energization and Escape on Mars and Venus

Mars and Venus do not have a global magnetic field and as a result solar wind interacts directly with their ionospheres and upper atmospheres. Neutral atoms ionized by solar UV, charge exchange and electron impact, are extracted and scavenged by solar wind providing a significant loss of planetary volatiles. There are different channels and routes through which the ionized planetary matter escapes from the planets. Processes of ion energization driven by direct solar wind forcing and their escape are intimately related. Forces responsible for ion energization in different channels are different and, correspondingly, the effectiveness of escape is also different. Classification of the energization processes and escape channels on Mars and Venus and also their variability with solar wind parameters is the main topic of our review. We will distinguish between classical pickup and ??mass-loaded?? pickup processes, energization in boundary layer and plasma sheet, polar winds on unmagnetized planets with magnetized ionospheres and enhanced escape flows from localized auroral regions in the regions filled by strong crustal magnetic fields.     

Menus for Feeding Black Holes

Black holes are the ultimate prisons of the Universe, regions of spacetime where the enormous gravity prohibits matter or even light to escape to infinity. Yet, matter falling toward the black holes may shine spectacularly, generating the strongest source of radiation. These sources provide us with astrophysical laboratories of extreme physical conditions that cannot be realized on Earth. This chapter offers a review of the basic menus for feeding matter onto black holes and discusses their observational implications.     

Analysis of Warning Times For Collision Avoidance Systems

The time required to execute a successful escape maneuver must be deduced from considerations of the following times: time required to gain adequate altitude separation, delay time due to pilot reaction, aircraft servo-system delay, delay due to missed data, delay due to data arrival time, alarm delay due to ? errors, time to stop turning, and time to level off. Since each of these times is a random variable, the required escape time must be determined in a probabilistic sense. By assigning appropriate probability density functions to each of the times involved, formulas are derived for the escape times required by the CAS hazard logic. The results of a simulation of 10 000 aircraft encounters verify the suitability of the formulas.     

弹射救生数值仿真及不利姿态下救生性能分析

 国内弹射座椅救生性能预测分析主要依赖地面弹射试验。由于国内相关试验设备的缺乏,不利姿态下弹射座椅的救生性能很难通过试验获得,因此国内不利姿态下弹射座椅救生性能的分析研究比较薄弱。采用数值仿真的方法对弹射座椅的救生性能进行预测和分析,针对弹射座椅弹射过程的4个阶段分别建立了数学模型,其中自由飞阶段采用四元数法代替欧拉速率方程,以解决传统的六自由度方程出现的奇异性问题。采用四阶龙格-库塔法对数学模型进行求解,计算结果与地面弹射试验结果吻合较好。在此基础上,对某新型弹射座椅的弹射姿态轨迹进行计算,分析研究了弹射座椅在不利姿态下的救生性能,得到不利姿态下弹射座椅救生性能不佳的主要原因是座椅高速稳定性差以及飞机向下的牵连速度和飞机滚转角的影响,并根据分析结果提出了改善弹射座椅不利姿态下救生性能的基本方法。     

民用客机缝翼气动噪声数值模拟研究

空中应急离机系统是飞行试验过程中保证试飞机组人员安全的重要措施。对国外一些试飞飞机的空中应急离机系统进行介绍,并对空中应急离机系统的总体设计原则、组成、功能、设计理念及多种子系统设计方案进行研究及分析。     

基于自编码网络的导弹攻击区实时计算方法

针对传统中远距空空导弹三线攻击区无法为飞行员提供丰富的战术决策信息,火控系统计算攻击区实时性差、精度低的问题,提出以攻击机为中心,考虑目标逃逸机动的新型导弹杀伤包线概念。分析经典战例中目标机规避导弹的常见机动方式,将攻击区抽象为导弹的七种杀伤包线,给出准确的计算方法并进行离线仿真。确定8种影响杀伤包线的运动参数,构建样本库。引入深度学习方法,建立降噪自编码网络（AE）模型,采用无监督学习提取样本初级特征,获取表征样本库非线性规律的高维特征量;建立深度网络模型,采用监督学习提取高维特征量中的高级特征并进行拟合。实验表明深度网络的拟合值与六自由度仿真结果以及导弹真实数据相比,误差可控制在15 m之内;网络在线解算只需0.04 s,能够满足实时性需求;新型杀伤包线为飞行员及时掌握敌我态势提供了有效的辅助信息,为机动决策提供理论依据。     

Exospheric models of the topside ionosphere

The historical evolution of the study of escape of light gases from planetary atmospheres is delineated, and the application of kinetic theory to the ionsphere is discussed. Ionospheric plasma becomes collisionless above the ion-exobase which is located near 1000 km altitude in the trough and polar regions, and which coincides with the plasmapause at lower latitudes. When the boundary conditions at conjugate points of a closed magnetic field line are different, interhemispheric particle fluxes exist from the high temperature point to the low temperature point, and from the point of larger concentrations to the point of smaller concentrations; therefore the charge separation electric field in the exosphere is no longer given by the Pannekoek-Rosseland field. For non-uniform number densities and temperatures at the exobase, the observed r ^–4 variation of the equatorial density distribution is recovered in the calculated density distributions. Taking account of plasmasheet particle precipitation does not change very much the electric field and ionospheric ion distributions, at least for reasonable densities and temperatures of the plasmasheet electrons and protons. For field aligned current densities along auroral field lines smaller than 10^–5 Am^–2, the potential difference between the ion-exobase and plasmasheet is about –3V. In the case of open magnetic field lines the flow speed of hydrogen and helium ions in the exosphere becomes rapidly supersonic as a consequence of the upward directed charge separation electric field, whereas the oxygen ions have a negligible small bulk velocity. Adding a photoelectron efflux decreases the thermal electron escape but does not change significantly the number density distributions.     

风对弹射座椅救生性能的影响

 针对某型弹射座椅建立了考虑风速的弹射过程动力学模型。选取不同风速风向和不同弹射速度作为计算状态,对弹射救生过程进行数值仿真,根据仿真结果分析风对弹射座椅救生性能的影响。通过在低速和中速两个弹射速度下,前向风、侧向风和大气垂直运动对弹射座椅救生性能影响的分析可知:较大的逆风不但会降低伞衣充满的轨迹高度,而且会产生人伞系统的振荡和摇摆,对安全救生存在一定的影响;大气的垂直运动对弹射救生系统的救生性能影响最大,它直接影响到救生系统的纵向运动轨迹。研究结果表明:前向风、侧向风和大气垂直运动均会对弹射座椅的救生性能产生不利影响,在真实的弹射过程中必须考虑风速对弹射救生性能的影响。     

遗传算法在飞行冲突解脱中的应用分析

国内外的专家和学者研究过多种方法用于飞行冲突解脱及解脱成本最小化问题,本文主要简介了基于遗传算法对2架飞机的飞行冲突的解脱模型,并在实际应用中对原来的优化过程进行了修改和完善,以某大型客机巡航参数为例,计算了优化后的飞行成本,结果表明:重新改进后的优化轨迹能够进一步降低飞行成本。     

Ion Acceleration and Outflow from Mars and Venus: An Overview

Solar wind forcing of Mars and Venus results in outflow and escape of ionospheric ions. Observations show that the replenishment of ionospheric ions starts in the dayside at low altitudes (??300?C800 km), ions moving at a low velocity (5?C10 km/s) in the direction of the external/ magnetosheath flow. At high altitudes, in the inner magnetosheath and in the central tail, ions may be accelerated up to keV energies. However, the dominating energization and outflow process, applicable for the inner magnetosphere of Mars and Venus, leads to outflow at energies ??5?C20 eV. The aim of this overview is to analyze ion acceleration processes associated with the outflow and escape of ionospheric ions from Mars and Venus. Qualitatively, ion acceleration may be divided in two categories:

1. Modest ion acceleration, leading to bulk outflow and/or return flow (circulation).
2. Acceleration to well over escape velocity, up into the keV range.

In the first category we find a processes denoted ??planetary wind??, the result of e.g. ambipolar diffusion, wave enhanced planetary wind, and mass-loaded ion pickup. In the second category we find ion pickup, current sheet acceleration, wave acceleration, and parallel electric fields, the latter above Martian crustal magnetic field regions. Both categories involve mass loading. Highly mass-loaded ion energization may lead to a low-velocity bulk flow??A consequence of energy and momentum conservation. It is therefore not self-evident what group, or what processes are connected with the low-energy outflow of ionospheric ions from Mars. Experimental and theoretical findings on ionospheric ion acceleration and outflow from Mars and Venus are discussed in this report.     

基于弹道逃逸和小推力捕获的地月转移轨道设计

针对地月空间货运任务和环月轨道空间设施建设任务,提出一种弹道逃逸和小推力捕获相结合的新型地月轨道转移模式,并建立了一整套该类型轨道设计方法。首先,在三体模型假设下分别建立地心弹道逃逸轨道和月心小推力捕获轨道的二维极坐标动力学模型。对于弹道逃逸轨道,将地心旋转系对准角和地月转移加速速度增量作为控制变量,提出初值估计解析公式,并应用序列二次规划算法进行快速求解。对于小推力捕获轨道,以月心距为参考量设置与弹道逃逸轨道的拼接点约束,提出能量匹配方法预估飞行时间,采用最优螺旋轨道的初始伴随状态解析式预估近月点伴随变量初值。基于混合法和轨道逆推思想,采用人工免疫算法进行小推力捕获轨道求解。仿真结果表明,基于弹道逃逸和小推力捕获的地月轨道转移方式大幅降低了近月制动燃料消耗,能快速穿越地球辐射带,且飞行时间适中;同时,提出的轨道设计方法能快速搜索到基于弹道逃逸和小推力捕获的地月转移轨道,验证了该方法的有效性。     

Coronal Hole Boundaries and their Interactions with Adjacent Regions

Coronal hole boundaries are the interfaces between regions where the coronal magnetic field contains a significant component which is open into the heliosphere and regions where the field is primarily closed. It is pointed out that there are constraints on the magnetic field which opens into the heliosphere that must be satisfied in the corona: it must come into pressure equilibrium in the high corona, and the component of the field which connects to the polar regions of the Sun must differentially rotate. A model is presented in which satisfying these constraints determines which field lines are open and which are closed, and thus where the polar coronal hole boundaries occur. Some of the consequences of this model are discussed. This revised version was published online in June 2006 with corrections to the Cover Date.     

Microphysics of Magnetic Reconnection

Magnetic reconnection is a universal phenomenon where energy is efficiently converted from the magnetic field to charged particles as a result of global magnetic topology changes during which earlier separated plasma regions become magnetically connected. While the reconnection affects large volumes in space most of the topology changes and of the energization occur within small localized regions. Regions of special importance are the X-region and the separatrix region. The understanding of the microphysics of these regions is crucial for the overall understanding of the reconnection. The Earth magnetosphere is the best environment where the details of these regions can be studied in situ. We summarize their main properties and discuss recent spacecraft observations.     

Photon escape probabilities; Concepts and clarifications

The concept of the escape probability of photons created within an optically thick (scattering and/or absorbing) medium is well established as a useful tool for qualitative and quantitative analysis of photon transfer. However there exist some ambiguities of notation and definition which can present problems in applications of the concept. This review relates a number of different treatments or analyses involving photon escape probabilities, introducing a common notation in order to clarify the topic.     

Working Group 3 Report: Coronal Hole Boundaries and Interactions with Adjacent Regions

Summarized below are the discussions of working group 3 on "Coronal hole boundaries and interactions with adjacent regions" which took place at the 7th SOHO workshop in Northeast Harbor, Maine, USA, 28 September to 1 October 1998. A number of recent observational and theoretical results were presented during the discussions to shed light on different aspects of coronal hole boundaries. The working group also included presentations on streamers and coronal holes to emphasis the difference between the plasma properties in these regions, and to serve as guidelines for the definition of the boundaries. Observations, particularly white light observations, show that multiple streamers are present close to the solar limb at all times. At some distance from the sun, typically below 2 R, these streamers merge into a relatively narrow sheet as seen, for example, in LASCO and UVCS images. The presence of multiple current sheets in interplanetary space was also briefly addressed. Coronal hole boundaries were defined as the abrupt transition from the bright appearing plasma sheet to the dark coronal hole regions. Observations in the inner corona seem to indicate a transition of typically 10 to 20 degrees, whereas observations in interplanetary space, carried out from Ulysses, show on one hand an even faster transition of less than 2 degrees which is in agreement with earlier Helios results. On the other hand, these observations also show that the transition happens on different scales, some of which are significantly larger. The slow solar wind is connected to the streamer belt/plasma sheet, even though the discussions were still not conclusive on the point where exactly the slow solar wind originates. Considered the high variability of plasma characteristics in slow wind streams, it seems most likely that several types of coronal regions produce slow solar wind, such as streamer stalks, streamer legs and open field regions between active regions, and maybe even regions just inside of the coronal holes. Observational and theoretical studies presented during the discussions show evidence that each of these regions may indeed contribute to the solar slow wind. This revised version was published online in June 2006 with corrections to the Cover Date.     

阻拦索断裂对螺旋桨舰载机着舰安全影响数值分析

喷气动力舰载机着舰拦阻滑跑，如阻拦索断裂，其逃逸复飞的概率极小。螺旋桨动力舰载机零升阻力大，推重比小，其安全复飞的能力值得研究。本文基于建立的螺旋桨舰载机逃逸复飞仿真模型（含阻拦索工作模型、发动机动力响应模型、升降舵操纵模型与气动力的动力影响修正模型），数值模拟了E-2C舰载预警机着舰阻拦索断裂情况下，其逃逸复飞的过程。仿真计算显示对象飞机在不同气动力、离舰速度与舵面操纵逻辑状态下，其纵向动力学方程中敏感参数与航迹下沉量的动态变化，结合视频数据分析其复飞成功的原因。研究表明：动力对螺旋桨舰载机俯仰力矩与升力特性的影响是其逃逸复飞成功的关键。动力影响使对象飞机的俯仰力矩曲线上移0.15，8°迎角下纵向静稳定性减小85%，升力线斜率增大29.7%、最大升力系数增大39%。这显著改善了螺旋桨飞机逃逸复飞状态下俯仰操纵的敏捷性，升降舵操纵效率与失速特性。动力影响使螺旋桨舰载机可在较小的加速度、离舰速度与有限的留空时间情况下，迅速改变其航迹角，减小航迹下沉量，保证逃逸复飞安全。     

空天飞行器整体式救生座舱的稳定减速与分离特性数值模拟

整体式密闭救生座舱方案将座椅与驾驶舱进行整体设计，弹射后具有独立的气动型面，在包含亚声速、跨声速、超声速甚至高超声速等非常宽广的速度范围可以更好地保护飞行员免受高速气流的吹袭，是空天飞行器救生系统设计的重要途径之一。针对整体式救生座舱，首先开展基本静态气动性能数值模拟评估；之后采用一种刚性减速伞增稳方案（整体式座舱+减速伞）对其稳定性和减速效率进行改进；最后采用动态重叠网格方法，对整体式座舱+减速伞构型的近机弹射轨迹特性开展动态数值模拟计算，从而获得该构型在抛投过程中的稳定性和安全性。研究结果表明，单独整体式救生座舱难以具备静稳定性；减速伞方案可大幅改善座舱的稳定性能，使座舱在Ma=0.3~4.0范围内均具有静、动态稳定性，并呈现亚声速时随马赫数升高而增强、超声速时随马赫数升高而减弱的变化规律，且高马赫数（Ma=4.0）工况可通过降低飞行高度以增加动压的方式进一步提升座舱的动稳定性；在宽速域范围内，整体式座舱+减速伞构型经过弹射力和火箭推力的辅助作用，能够实现与机体的安全分离，并且分离后其俯仰振荡姿态均具有收敛特性。     

Planetary Magnetic Fields and Solar Forcing: Implications for Atmospheric Evolution

The solar wind and the solar XUV/EUV radiation constitute a permanent forcing of the upper atmosphere of the planets in our solar system, thereby affecting the habitability and chances for life to emerge on a planet. The forcing is essentially inversely proportional to the square of the distance to the Sun and, therefore, is most important for the innermost planets in our solar system—the Earth-like planets. The effect of these two forcing terms is to ionize, heat, chemically modify, and slowly erode the upper atmosphere throughout the lifetime of a planet. The closer to the Sun, the more efficient are these process. Atmospheric erosion is due to thermal and non-thermal escape. Gravity constitutes the major protection mechanism for thermal escape, while the non-thermal escape caused by the ionizing X-rays and EUV radiation and the solar wind require other means of protection. Ionospheric plasma energization and ion pickup represent two categories of non-thermal escape processes that may bring matter up to high velocities, well beyond escape velocity. These energization processes have now been studied by a number of plasma instruments orbiting Earth, Mars, and Venus for decades. Plasma measurement results therefore constitute the most useful empirical data basis for the subject under discussion. This does not imply that ionospheric plasma energization and ion pickup are the main processes for the atmospheric escape, but they remain processes that can be most easily tested against empirical data. Shielding the upper atmosphere of a planet against solar XUV, EUV, and solar wind forcing requires strong gravity and a strong intrinsic dipole magnetic field. For instance, the strong dipole magnetic field of the Earth provides a “magnetic umbrella”, fending of the solar wind at a distance of 10 Earth radii. Conversely, the lack of a strong intrinsic magnetic field at Mars and Venus means that the solar wind has more direct access to their topside atmosphere, the reason that Mars and Venus, planets lacking strong intrinsic magnetic fields, have so much less water than the Earth? Climatologic and atmospheric loss process over evolutionary timescales of planetary atmospheres can only be understood if one considers the fact that the radiation and plasma environment of the Sun has changed substantially with time. Standard stellar evolutionary models indicate that the Sun after its arrival at the Zero-Age Main Sequence (ZAMS) 4.5 Gyr ago had a total luminosity of ≈70% of the present Sun. This should have led to a much cooler Earth in the past, while geological and fossil evidence indicate otherwise. In addition, observations by various satellites and studies of solar proxies (Sun-like stars with different age) indicate that the young Sun was rotating more than 10 times its present rate and had correspondingly strong dynamo-driven high-energy emissions which resulted in strong X-ray and extreme ultraviolet (XUV) emissions, up to several 100 times stronger than the present Sun. Further, evidence of a much denser early solar wind and the mass loss rate of the young Sun can be determined from collision of ionized stellar winds of the solar proxies, with the partially ionized gas in the interstellar medium. Empirical correlations of stellar mass loss rates with X-ray surface flux values allows one to estimate the solar wind mass flux at earlier times, when the solar wind may have been more than 1000 times more massive. The main conclusions drawn on basis of the Sun-in-time-, and a time-dependent model of plasma energization/escape is that:

1. Solar forcing is effective in removing volatiles, primarily water, from planets,
2. planets orbiting close to the early Sun were subject to a heavy loss of water, the effect being most profound for Venus and Mars, and
3. a persistent planetary magnetic field, like the Earth’s dipole field, provides a shield against solar wind scavenging.

     

弹射座椅的发展趋势

本文回顾了弹射座椅的发展历程。重点讨论了改善弹射座椅低空救生和大速度救生的方案,指出了今后将采用的新技术,包括微处理机、各种传感器和可调节的动力装置,以满足座椅自适应控制的要求。最后分析了提到议事日程上的高过载座舱的三种拟议方案。     

定常幅值小推力登月飞行器轨道研究

 进行了基于平面三体模型的登月飞行器轨道控制方法的研究;研究了从近地低轨道到近月低轨道的飞行轨道;给出了在地球逃逸段、惯性漂移段和月球捕获段的运动轨迹和关键点的参数。提出使用“远地点可达”概念完成了地球逃逸段发动机推力终点的选择和使用飞行器相对月心能量完成了在月球捕获段止推发动机工作初始点的选择。