载人火星探测进展及其EDL过程GNC关键技术

随着火星探测技术的不断发展和探测任务的不断推进，载人火星探测在未来将会成为火星探测的重要手段。首先，回顾了无人火星探测任务的发展历程，对比分析了部分无人火星探测器进入、下降与着陆（EDL）过程的参数。然后，结合无人火星探测、载人月球探测和载人航天再入过程，梳理了载人火星探测的特点及需求，系统地总结了前苏联/俄罗斯和美国的载人火星探测研究进展以及技术储备。接着，归纳了载人火星探测的体系构成、集结方式和主要的技术挑战。最后，概括了载人火星EDL过程面临的难题，重点阐述了EDL的导航、制导与控制（GNC）关键技术。     

Atmospheric Ion-induced Aerosol Nucleation

Ion-induced nucleation has been suggested to be a potentially important mechanism for atmospheric aerosol formation. Ions are formed in the background atmosphere by galactic cosmic rays. A possible connection between galactic cosmic rays and cloudiness has been However, the predictions of current atmospheric nucleation models are highly uncertain because the models are usually based on the liquid drop model that estimates cluster thermodynamics based on bulk properties (e.g., liquid drop density and surface tension). Sulfuric acid (H₂SO₄) and water are assumed to be the most important nucleating agents in the free troposphere. Measurements of the molecular thermodynamics for the growth and evaporation of cluster ions containing H₂SO₄ and H₂O were performed using a temperature-controlled laminar flow reactor coupled to a linear quadrupole mass spectrometer as well as a temperature-controlled ion trap mass spectrometer. The measurements were complemented by quantum chemical calculations of the cluster ion structures. The analysis yielded a complete set of H₂SO₄ and H₂O binding thermodynamics extending from molecular cluster ions to the bulk, based on experimental thermodynamics for the small clusters. The data were incorporated into a kinetic aerosol model to yield quantitative predictions of the rate of ion-induced nucleation for atmospheric conditions. The model predicts that the negative ion-H₂SO₄-H₂O nucleation mechanism is an efficient source of new particles in the middle and upper troposphere.     

Did life exist on Mars? Search for organic and inorganic signatures, one of the goals for “SAM” (sample analysis at Mars)

Observation of Mars shows signs of a past Earth-like climate, and, in that case, there is no objection to the possible development of life, in the underground or at the surface, as in the terrestrial primitive biosphere. Sample analysis at Mars (SAM) is an experiment which may be proposed for atmospheric, ground and underground in situ measurements. One of its goals is to bring direct or indirect information on the possibility for life to have developed on Mars, and to detect traces of past or present biological activity. With this aim, it focuses on the detection of organic molecules: volatile organics are extracted from the sample by simple heating, whereas refractory molecules are made analyzable (i.e. volatile), using derivatization technique or fragmentation by pyrolysis. Gaseous mixtures thus obtained are analyzed by gas chromatography associated to mass spectrometry. Beyond organics, carbonates and other salts are associated to the dense and moist atmosphere necessary to the development of life, and might have formed and accumulated in some places on Mars. They represent another target for SAM. Heating of the samples allows the analysis of structural gases of these minerals (CO₂ from carbonates, etc.), enabling to identify them. We also show, in this paper, that it may be possible to discriminate between abiotic minerals, and minerals (shells, etc.) created by living organisms.     

A space radiation shielding model of the Martian radiation environment experiment (MARIE)

The 2001 Mars Odyssey spacecraft was launched towards Mars on April 7, 2001. Onboard the spacecraft is the Martian radiation environment experiment (MARIE), which is designed to measure the background radiation environment due to galactic cosmic rays (GCR) and solar protons in the 20–500 MeV/n energy range. We present an approach for developing a space radiation-shielding model of the spacecraft that includes the MARIE instrument in the current mapping phase orientation. A discussion is presented describing the development and methodology used to construct the shielding model. For a given GCR model environment, using the current MARIE shielding model and the high-energy particle transport codes, dose rate values are compared with MARIE measurements during the early mapping phase in Mars orbit. The results show good agreement between the model calculations and the MARIE measurements as presented for the March 2002 dataset.     

火星环绕器环火轨道的角动量管理方法

针对中国首次火星探测的任务需求和规划,结合环绕器质量特性和布局构型以及大椭圆轨道特性,分析了环绕器在环火飞行阶段所受的重力梯度力矩和光压力矩规律.空间干扰力矩累积导致飞轮转速上升,影响姿态机动能力,需要喷气卸载.为减少喷气卸载次数,在满足系统任务的基础上,设计了姿态偏置方案,利用光压力矩和重力梯度力矩相互抵消减少角动量...     

损耗大气中随机重力波场的传输方程

从包含分子粘性的非线性相互作用方程出发, 采用随机相位近似, 推导了损耗大气中重力波场的非线性传输方程。由于分子损耗的引入, 谱演变的速率发生了改变, 在某些情况下, 还会得到与无耗条件下的传输规律相反的结论。损耗大气中重力波场的传输方程是研究中高层大气重力波能量收支平衡的出发点。      

模型参数扰动下的火星大气进入鲁棒状态估计方法

针对火星大气进入段模型参数扰动及动力学系统的强非线性影响导航系统状态精确估计问题,提出了一种模型参数扰动下的鲁棒插值滤波（DDF）方法。该方法在传统插值滤波方法代价函数的基础上,通过把扰动参数对状态估计精度影响的度量矩阵乘积的迹增广到代价函数,推导了具有解析滤波增益形式的鲁棒插值滤波方法。同时,通过实时计算进入过程中导航系统的非线性,基于系统非线性度给出了鲁棒插值滤波方法阶次自适应选取准则。只在系统强非线性阶段采用高阶鲁棒插值滤波方法,既保证状态估计精度,同时满足导航系统实时性需求。仿真结果表明,提出的鲁棒插值滤波方法比传统的一阶插值滤波方法估计精度更高,能达到二阶鲁棒插值滤波方法的估计精度,比整个进入过程采用二阶鲁棒插值滤波方法具有更高的解算效率。     

火星探测降落伞模型高速风洞变迎角试验技术

为获得火星探测器物伞系统动力学仿真中需要使用的降落伞轴向力、法向力、俯仰力矩系数,开展了火星探测降落伞模型高速风洞变迎角试验技术研究,研制了火星探测降落伞模型高速风洞变迎角试验装置,进行了火星探测降落伞模型高速风洞变迎角试验,获得了火星探测降落伞模型在马赫数范围0.4～0.8、迎角范围0°～25°时的轴向力、法向力和俯仰力矩系数,并对支撑干扰及洞壁干扰影响进行了扣除修正。试验结果表明：火星探测降落伞模型的轴向力系数随迎角变化较小;常规透气伞的法向力系数随迎角增大而增大,在马赫数为0.4和0.6时,低透气伞的法向力系数在小迎角时随迎角增大而减小;在马赫数范围0.4～0.8时,常规透气伞静稳定,低透气伞的静稳定性较常规透气伞减小,在马赫数为0.4和0.6时,低透气伞在零迎角时静不稳定,出现了非零配平 迎角。     

火星进入器作强迫震荡运动壁面脉动压力数值模拟

为研究超声速阶段进入器作强迫震荡运动对壁面脉动压力环境的影响规律,本文耦合进入器刚体运动方程与流体力学方程,采用动网格技术,对火星进入器模型开展非定常数值模拟,获取壁面不同位置处的脉动压力信息。研究表明：在超声速阶段,进入器作强迫震荡运动诱导的脉动压力远大于进入器保持相对静止时仅由非定常流动诱导的脉动压力。来流马赫数为1.2时,进入器作强迫震荡运动对脱体激波影响较小,脱体激波强度较弱且形态变化较小,攻角的震荡导致同一测点距离脱体激波的位置发生周期性改变,舱体迎风面及配平翼迎风面的脉动压力环境主要受攻角变化的影响;来流马赫数为3时,进入器作强迫震荡运动对脱体激波的影响较大,脱体激波震荡剧烈,诱导舱体迎风面及配平翼迎风面产生极其恶劣的脉动压力环境,功率谱分析表明激波震荡诱导的脉动压力能量主要集中在30 Hz左右。     

基于有效透气量对火星降落伞气动力系数预测分析

针对火星探测任务中降落伞开伞环境为低密度大气的特点,本文由降落伞气动力系数与透气量关系,提出了通过降落伞有效透气量预测降落伞气动力系数的方法,该方法先由织物透气量试验获取伞衣透气量拟合曲线和透气量常数,再根据风洞试验得到两种有效透气量下的气动力系数,然后由有效透气量插值获取了盘缝带(DGB)伞火星大气条件下气动力系数,并且通过空投试验数据对该方法进行验证。计算结果表明,在火星条件下,降落伞气动力系数与风洞条件下变化趋势基本一致。Ma 0.4工况阻力系数的变化范围为0.583～0.622,Ma 0.8工况阻力系数的变化范围为0.438～0.494。