一种半解析方法火星再入探测器一体化设计模型

提出了一种火星再入探测器的半解析法一体化模型,为未来火星探测器的初步设计提供包括弹道、气动参数、防热系统在内的设计依据。在任务初步设计阶段,由于涉及多个学科,火星大气与地球大气模型差异很大,需要考虑的因素很多,因此需要一个半解析的,能够实时进行弹道、气动参数和防热层温度分布计算的设计工具。该工具应该包括气动外形、弹道、防热为一体的设计模型,且能满足计算负担要求。基于此,提出了一种普遍适应的火星探测器外形定义方程,并对其中的一种特殊情况进行了解析公式的推导。在合理假设的前提下,给出了计算防热层内部温度分布的半解析计算公式,并以MER\|B (Mars Exploration Rover)探测器为例进行了弹道和气动受热仿真。计算结果表明,该一体化计算模型的仿真计算落点与实际落点很接近,达到了火星探测器初步设计阶段一体化的计算要求。
     

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。     

Particle acceleration and gamma rays in solar flares: Recent observations and new modeling

Experiments on SMM, GAMMA, Yohkoh, GRANAT, Compton GRO, INTEGRAL, RHESSI and CORONAS-F satellites over the past three decades have provided copious data for fundamental research relating to particle acceleration, transport and energetics of flares and to the ambient abundance of the solar corona, chromosphere and photosphere. We summarize main results of solar gamma-astronomy (including some results of several joint Russian–Chinese projects) and try to appraise critically a real contribution of those results into modern understanding of solar flares, particle acceleration at the Sun and some properties of the solar atmosphere. Recent findings based on the RHESSI, INTEGRAL and CORONAS-F measurements (source locations, spectrum peculiarities, ³He abundance etc.) are especially discussed. Some unusual features of extreme solar events (e.g., 28 October 2003 and 20 January 2005) have been found in gamma-ray production and generation of relativistic particles (solar cosmic rays, or SCR). A number of different plausible assumptions are considered concerning the details of underlying physical processes during large flares: (1) existence of a steeper distribution of surrounding medium density as compared to a standard astrophysical model (HSRA) for the solar atmosphere; (2) enhanced content of the ³He isotope; (3) formation of magnetic trap with specific properties; (4) prevailing non-uniform (e.g., fan-like) velocity (angular) distributions of secondary neutrons, etc. It is emphasized that real progress in this field may be achieved only by combination of gamma-ray data in different energy ranges with multi-wave and energetic particle observations during the same event. We especially note several promising lines for the further studies: (1) resonant acceleration of the ³He ions in the corona; (2) timing of the flare evolution by gamma-ray fluxes in energy range above 90 MeV; (3) separation of gamma-ray fluxes from different sources at/near the Sun (e.g., different acceleration sources/episodes during the same flare, contribution of energetic particles accelerated by the CME-driven shocks etc.); (4) asymmetric magnetic geometry and new magnetic topology models of the near-limb flares; (5) modeling of self-consistent time scenario of the event.     

基于单星定位的火星着陆器初定位方法研究

针对火星探测中着陆器的初定位问题,提出了一种利用单个轨道环绕器为着陆器进行无线电定位的计算方法。首先根据投影法求解着陆器的位置初值,再使用最小二乘法,利用一段时间内的轨道器的位置及其与着陆器的距离数据,求解着陆器的经纬度。通过与卫星工具包(Satellite Tool Kit,STK)软件的计算结果比较,表明此方法是有效的。     

火星车绝对定位方法选择

针对火星巡视探测任务,提出3种火星车绝对定位方法:无线电测控定位、图像匹配定位、位置圆定位。无线电测控方法首先确定环绕器的轨道,然后利用环绕器和火星车的器间通信定位确定火星车的绝对位置;图像匹配方法利用着陆过程中的降落图像与带地理信息的着陆区地形图进行匹配,实现火星车的位置确定;位置圆方法通过敏感器在多个时刻测量阳光矢量方向和重力矢量方向,结合星历信息求解火星车的位置。对3种方法进行分析比较,根据定位精度、使用约束等因素,给出在轨使用建议:位置圆定位为基本方法,无线电测控定位作为校验手段,图像匹配定位作为修正手段,以满足火星车快速、高精度的定位需求。     

火星探测发展历程与未来展望

火星作为距地球最近的类地行星之一,火星探测是继月球探测之后深空探测的最大热点。在简要总结人类火星探测历程与未来发展趋势的基础上,对未来的火星探测规划任务及其面临的主要关键技术进行了重点论述,并给出了相应启示和发展展望;结合我国深空探测能力,并对中国后续开展火星探测活动提出了相关的建议。     

Patterns of carbon monoxide in the middle atmosphere and effects of solar variability

We determine the spatial-time patterns of zonally averaged carbon monoxide (CO) in the middle atmosphere by applying Principle Component Analysis to the CO data obtained from the Microwave Limb Sounder (MLS) measurements on the Aura satellite in 2004–2012. The first two principal components characterize more than 90% of the CO variability. Both principal components are localized in the low thermosphere near the mesopause. The first principal component is asymmetric relative to the poles. It has opposite signs in the Northern and Southern Hemisphere at mid to high latitudes and strongly oscillates with an annual periodicity. The second principal component has the same sign in both hemispheres and oscillates mainly with a semi-annual frequency. Both principal components are modulated by the 11-year solar cycle and display short-term variations. To test possible correlations of these variations with the short term solar ultraviolet (UV) variability we use the simultaneous measurements of the UV solar radiance from the Solar-Stellar Irradiance Comparison Experiment (SOLSTICE) on the Solar Radiation and Climate Experiment (SORCE) satellite to investigate the correlation between CO in the middle atmosphere and solar UV in 2004–2012. Using a wavelet coherence technique a weak, intermittent 27-day signal is detected in high-frequency parts of the CO principal components.     

一种火星大气密度三维解析模型

根据火星大气数据库,建立了以高度和经纬度为输入的火星三维解析大气密度模型;在竖直方向上,采用分层指数模型;在水平方向上,将指数模型中的参考密度和参考高度视为经纬度的多项式函数,并通过最小二乘曲面拟合得到了多项式系数。相比传统的指数模型,三维指数模型不仅反映了火星大气密度随高度的变化规律,而且能够体现出大气密度在水平方向上的变化。与大气数据库相比,三维密度模型具有解析形式,计算速度快,仿真过程中只需存储简单的多项式系数即可实现密度的实时计算和调用,适用于地面实时仿真。     

火星尘埃对太阳电池阵的影响与电帘除尘研究

火星表面大量尘埃在太阳电池阵表面的累积将会导致其输出功率下降,甚至使太阳电池阵功能失效。近年来,电帘除尘方法被认为是在火星着陆任务中进行尘埃防护最有效的手段之一。本文开展了火星尘埃累积对三结砷化镓太阳电池性能影响的实验研究,得到了火星尘埃累积量与太阳电池电压、电流和相对输出功率数值模型;通过除尘技术分析,确定电帘除尘装置构型;依据制备得到的除尘电帘,对不同火星尘埃累积下电帘的除尘效率进行了研究,为火星着陆太阳电池阵遥测数据分析和开发自适应除尘太阳电池阵提供有力的技术支持。     

An innovative high accuracy autonomous navigation method for the Mars rovers

Autonomous navigation is an important function for a Mars rover to fulfill missions successfully. It is a critical technique to overcome the limitations of ground tracking and control traditionally used. This paper proposes an innovative method based on SINS (Strapdown Inertial Navigation System) with the aid of star sensors to accurately determine the rover?s position and attitude. This method consists of two parts: the initial alignment and navigation. The alignment consists of a coarse position and attitude initial alignment approach and fine initial alignment approach. The coarse one is used to determine approximate position and attitude for the rover. This is followed by fine alignment to tune the approximate solution to accurate one. Upon the completion of initial alignment, the system can be used to provide real-time navigation solutions for the rover. An autonomous navigation algorithm is proposed to estimate and compensate the accumulated errors of SINS in real time. High accuracy attitude information from star sensor is used to correct errors in SINS. Simulation results demonstrate that the proposed methods can achieve a high precision autonomous navigation for Mars rovers.