Locations of Atmospheric Photoelectron Energy Peaks Within the Mars Environment

By identifying peaks in the photoelectron spectrum produced by photoionization of CO₂ in the Martian atmosphere, we have conducted a pilot study to determine the locations of these photoelectrons in the space around Mars. The significant result of this study is that these photoelectrons populate a region around Mars bounded externally by the magnetic pileup boundary, and internally by the lowest altitude of our measurements (∼250 km) on the dayside and by a cylinder of approximately the planetary radius on the nightside. It is particularly noteworthy that the photoelectrons on the nightside are observed from the terminator plane tailward to a distance of ∼3 R _M, the Mars Express apoapsis. The presence of the atmospherically generated photoelectrons on the nightside of Mars may be explained by direct magnetic field line connection between the nightside observation locations and the Martian dayside ionosphere. Thus the characteristic photoelectron peaks may be used as tracers of magnetic field lines for the study of the magnetic field configuration and particle transport in the Martian environment.     

Energisation of O+ and O+ 2 Ions at Mars: An Analysis of a 3-D Quasi-Neutral Hybrid Model Simulation

We have studied the loss of O⁺ and O⁺ ₂ ions at Mars with a numerical model. In our quasi-neutral hybrid model ions (H⁺, He⁺⁺, O⁺, O⁺ ₂) are treated as particles while electrons form a massless charge-neutralising fluid. The employed model version does not include the Martian magnetic field resulting from the crustal magnetic anomalies. In this study we focus the Martian nightside where the ASPERA instrument on the Phobos-2 spacecraft and recently the ASPERA-3 instruments on the Mars Express spacecraft have measured the proprieties of escaping atomic and molecular ions, in particular O⁺ and O⁺ ₂ ions. We study the ion velocity distribution and how the escaping planetary ions are distributed in the tail. We also create similar types of energy-spectrograms from the simulation as were obtained from ASPERA-3 ion measurements. We found that the properties of the simulated escaping planetary ions have many qualitative and quantitative similarities with the observations made by ASPERA instruments. The general agreement with the observations suggest that acceleration of the planetary ions by the convective electric field associated with the flowing plasma is the key acceleration mechanism for the escaping ions observed at Mars.     

Investigation of the Influence of Magnetic Anomalies on Ion Distributions at Mars

Using data from the Mars Express Ion Mass Analyzer (IMA) we investigate the distribution of ion beams of planetary origin and search for an influence from Mars crustal magnetic anomalies. We have concentrated on ion beams observed inside the induced magnetosphere boundary (magnetic pile-up boundary). Some north-south asymmetry is seen in the data, but no longitudinal structure resembling that of the crustal anomalies. Comparing the occurrence rate of ion beams with magnetic field strength at 400 km altitude below the spacecraft (using statistical Mars Global Surveyor results) shows a decrease of the occurrence rate for modest (< 40 nT) magnetic fields. Higher magnetic field regions (above 40 nT at 400 km) are sampled so seldom that the statistics are poor but the data is consistent with some ion outflow events being closely associated with the stronger anomalies. This ion flow does not significantly affect the overall distribution of ion beams around Mars.     

Mars Global Surveyor Measurements of the Martian Solar Wind Interaction

The solar wind at Mars interacts with the extended atmosphere and small-scale crustal magnetic fields. This interaction shares elements with a variety of solar system bodies, and has direct bearing on studies of the long-term evolution of the Martian atmosphere, the structure of the upper atmosphere, and fundamental plasma processes. The magnetometer (MAG) and electron reflectometer (ER) on Mars Global Surveyor (MGS) continue to make many contributions toward understanding the plasma environment, thanks in large part to a spacecraft orbit that had low periapsis, had good coverage of the interaction region, and has been long-lived in its mapping orbit. The crustal magnetic fields discovered using MGS data perturb plasma boundaries on timescales associated with Mars' rotation and enable a complex magnetic field topology near the planet. Every portion of the plasma environment has been sampled by MGS, confirming previous measurements and making new discoveries in each region. The entire system is highly variable, and responds to changes in solar EUV flux, upstream pressure, IMF direction, and the orientation of Mars with respect to the Sun and solar wind flow. New insights from MGS should come from future analysis of new and existing data, as well as multi-spacecraft observations.     

火星无人机实验台发展综述及构想

火星地表崎岖、环境复杂,火星无人机由于其具有高机动性和灵活性,为火星探测提供了一种新的工作模式,是未来深空探测的重要范式。本文对比了火星与地球相关地表环境参数的差异,分析了火星无人机需要克服的困难和主要用途,阐明了火星无人机实验台的重要性;详细介绍了国内外研究机构研发火星无人机实验台的技术特点与功能优劣,总结了实验台需要具备的模拟火星环境和测量相关参数。在此基础上,提出了构建火星无人机实验台设想,给出了总体设计思想和思路,并对火星无人机气动力学实验平台的应用前景进行了展望。     

Global Response of Martian Plasma Environment to an Interplanetary Structure: From Ena and Plasma Observations at Mars

As a part of the global plasma environment study of Mars and its response to the solar wind, we have analyzed a peculiar case of the subsolar energetic neutral atom (ENA) jet observed on June 7, 2004 by the Neutral Particle Detector (NPD) on board the Mars Express satellite. The “subsolar ENA jet” is generated by the interaction between the solar wind and the Martian exosphere, and is one of the most intense sources of ENA flux observed in the vicinity of Mars. On June 7, 2004 (orbit 485 of Mars Express), the NPD observed a very intense subsolar ENA jet, which then abruptly decreased within ∼10 sec followed by quasi-periodic (∼1 min) flux variations. Simultaneously, the plasma sensors detected a solar wind structure, which was most likely an interplanetary shock surface. The abrupt decrease of the ENA flux and the quasi-periodic flux variations can be understood in the framework of the global response of the Martian plasma obstacle to the interplanetary shock. The generation region of the subsolar ENA jet was pushed towards the planet by the interplanetary shock; and therefore, Mars Express went out of the ENA jet region. Associated global vibrations of the Martian plasma obstacle may have been the cause of the quasi-periodic flux variations of the ENA flux at the spacecraft location.     

Energetic Hydrogen and Oxygen Atoms Observed on the Nightside of Mars

We present measurements of energetic hydrogen and oxygen atoms (ENAs) on the nightside of Mars detected by the neutral particle detector (NPD) of ASPERA-3 on Mars Express. We focus on the observations for which the field-of-view of NPD was directed at the nightside of Mars or at the region around the limb, thus monitoring the flow of ENAs towards the nightside of the planet. We derive energy spectra and total fluxes, and have compiled maps of hydrogen ENA outflow. The hydrogen ENA intensities reach 10⁵ cm⁻² sr⁻¹ s⁻¹, but no oxygen ENA signals above the detection threshold of 10⁴ cm⁻² sr⁻¹ s⁻¹ are observed. These intensities are considerably lower than most theoretical predictions. We explain the discrepancy as due to an overestimation of the charge-exchange processes in the models for which too high an exospheric density was assumed. Recent UV limb emission measurements (Galli et al., this issue) point to a hydrogen exobase density of 10¹⁰ m⁻³ and a very hot hydrogen component, whereas the models were based on a hydrogen exobase density of 10¹² m⁻³ and a temperature of 200 K predicted by Krasnopolsky and Gladstone (1996). Finally, we estimate the global atmospheric loss rate of hydrogen and oxygen due to the production of ENAs.     

The Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) for the Mars Express Mission

The general scientific objective of the ASPERA-3 experiment is to study the solar wind – atmosphere interaction and to characterize the plasma and neutral gas environment with within the space near Mars through the use of energetic neutral atom (ENA) imaging and measuring local ion and electron plasma. The ASPERA-3 instrument comprises four sensors: two ENA sensors, one electron spectrometer, and one ion spectrometer. The Neutral Particle Imager (NPI) provides measurements of the integral ENA flux (0.1–60 keV) with no mass and energy resolution, but high angular resolution. The measurement principle is based on registering products (secondary ions, sputtered neutrals, reflected neutrals) of the ENA interaction with a graphite-coated surface. The Neutral Particle Detector (NPD) provides measurements of the ENA flux, resolving velocity (the hydrogen energy range is 0.1–10 keV) and mass (H and O) with a coarse angular resolution. The measurement principle is based on the surface reflection technique. The Electron Spectrometer (ELS) is a standard top-hat electrostatic analyzer in a very compact design which covers the energy range 0.01–20 keV. These three sensors are located on a scanning platform which provides scanning through 180^∘ of rotation. The instrument also contains an ion mass analyzer (IMA). Mechanically IMA is a separate unit connected by a cable to the ASPERA-3 main unit. IMA provides ion measurements in the energy range 0.01–36 keV/charge for the main ion components H⁺, He⁺⁺, He⁺, O⁺, and the group of molecular ions 20–80 amu/q. ASPERA-3 also includes its own DC/DC converters and digital processing unit (DPU).     

地火转移轨道误差分析与第1次中途修正计算

针对地火转移过程中出现的各种误差,基于地火转移轨道的误差传递矩阵分析误差发散的性质,在此基础上讨论如何选取轨道中途修正的时机,并基于该矩阵对地火转移轨道第一次中途轨道修正的速度增量进行估算。与微分修正方法的严格计算结果的比较表明,基于该方法定性研究地火转移轨道第1次中途修正速度增量变化和选取合适的轨道机动时机是可行的。使用蒙特卡洛数值模拟对上述方法和微分修正方法进行计算和比较,结果表明,第1次中途修正速度增量大小差异不超过1.2m/s,相对误差不超过6%。在轨道控制精度大约为1m/s的情况下使用该方法代替微分修正方法进行计算,可以节省大量的计算时间。     

总能量守恒格式的构造及检验

由于大气海洋方程大都带有拟线性形式的对（平）流项，本文依据一个有关格式构造的定是，提出一个构造总能量守恒格式的新方法，不仅使以往构造的许多平方守恒格式成其为特例，而且为大气海洋数值模拟提供了灵活地选择计算格式的机会。文中给出的算例表明所构造格式的守恒性很好。     

拓扑优化设计中刚度与密度关系的一种力学模型

为了探讨变密度法中伪密度的变化对材料刚度的影响,并建立两者之间的力学关系,本文采用有限元法研究这一问题。提出利用"实心"与"空心"两种八节点体单元来构建"微元体"模型,通过各种比例的"实心"和"空心"体单元的均匀组合,来模拟伪密度数值的变化过程。理论分析与推导表明:确定"微元体"的刚度时,本模型不仅与加载和约束形式无关,而且与"微元体"的形状亦无关。通过数值试验,可以给出这种模型的刚度与伪密度的离散数值关系;最后,利用幂指函数获得其解析关系。计算结果发现一个十分有趣的现象:刚度与伪密度不遵循人为给出的幂函数关系。     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.     

大气扰动建模及在民机工程应用中的研究

大气扰动是影响飞机飞行安全的重要因素。对民用飞机研制试验所需的及相关适航文件中规定的大气扰动进行了建模分析,包括环球风、风切变、大气紊流等。介绍了大气扰动模型在实时仿真系统中的实现及仿真,该研究是民用飞机飞行品质评估、FHA试验及大气扰动相关的适航验证试验的重要支撑。     

Arcadia建模方法与SysML建模方法比较研究

基于模型的系统工程与传统系统工程相比,有着形象化、具体化、沟通效率高等多种优势。基于系统建模(System Modeling Language,简称SysML)语言进行建模用途广泛,但是通过实践,针对系统架构和系统运行场景分析,基于Sys ML的建模方法特点并不突出。而Arcadia的基于模型系统工程建模有着简单、清晰等特点,对于系统架构和系统定义均有着Sys ML所不具备的特点。通过系统设计的目标与特点,对基于Sys ML的建模方法和Arcadia方法进行比较研究和实践,总结两种方法在基于模型的系统工程领域中的优劣。     

反向喷流与主流干扰数值模拟

反向喷流是改变钝体迎风面压力和温度分布的有效手段之一，所以了解反向喷流场对再入体防热及减阻设计具有重要意义，本文用有差分法求解轴称Ｎ－Ｓ方程模拟了球柱体部反向喷流与超声速自由来流的干扰流场。研究了喷流出口压力对流场的影响，物面压力分布及喷流Ｍａｃｈ盘、弓形激波的脱体距离与实验值进行了比较，取得了一致的结果，喷流附近分离区的再附位置及再附产生的激波位置也与实验相符，但高压比下再附激波略强于实验。     

滞止式温度传感器动态理论建模研究

根据滞止式温度传感器的换热原理建立了动态理论传热模型,采用数值计算方法对模型方程进行了求解,并对计算结果进行了分析.     

转子-电磁轴承系统动静件碰摩动力特性研究

对转子—磁轴承系统动静件间发生碰摩时的非线性动力学行为进行了研究,在考虑质量偏心的情况下建立了系统的数学模型,求解了系统的周期解,并结合分岔图、庞加莱映射和频谱分析研究了系统的动态特性,研究表明系统发生碰摩后,随着转速及偏心率的增加,转子运动中具有连续的周期分岔现象,并走向失稳,其频谱图中组合频率在奇数倍频附近发生了从右到左的频移现象。这些研究结果可用于控制碰摩后电磁轴承的稳定性,避免大事故的发生。其振动频率特征可判别磁轴承系统是否发生了碰摩故障。