Observation of aphelion cloud belt over Martian tropics,its evolution,and associated dust distribution from MCS data

The present study uses five Martian years of observations from Mars Climate Sounder onboard Mars Reconnaissance Orbiter for investigating the Aphelion Cloud Belt (ACB) over the tropics. Analysis of zonal mean water ice column opacity suggests that the spatial extension of the ACB is mainly confined over the tropics and mid-latitudes (-20 – 40°N) during L_S ~ 45 – 135° (L_S = 0° signifies northern spring equinox). The ACB is seen primarily in the nighttime only due to the truncation of the daytime profile observations at significantly higher altitudes (at ~30 km). Zonal mean ice extinction profiles show ACB’s altitudinal range within ~10 – 40 km, and the existence of a thin cloud band in the absence of a thick ACB during aphelion season. Three phases of the ACB could be identified as the formation phase during L_S = 45 – 75° (phase 1), the peak phase during L_S = 76 – 105° (phase 2), and the decaying phase during L_S = 106 – 135° (phase 3). Observation of the cloud latitude belt shows a northward movement starting from phase 2, prominent over regions nearby Lunae Planum and Xanthe Terra. During this phase, the top level of thick clouds within the ACB decreases to ~20 km in the southern hemisphere, while it increases a little over the northern hemisphere (NH). The decreasing tendency continues in phase 3 over the entire region ?10 – 10°N, and the thick cloud base moves higher over the NH, though the vertical depth of it becomes narrower than phase 2. Temperature profiles do not show any noticeable influence on the northward evolution of the ACB. However, the study at a regional level indicates a possible association of upper tropospheric dustiness with the ACB’s evolution. The mechanism is evident in the correlation analysis mostly at an altitude range of ~18 – 35 km. The migrating semidiurnal tide (SMD) as a proxy of dust or water ice forcing, and the calculated upper tropospheric dust radiative heating, shows an apparent northward movement of their peak amplitude within the three phases of the ACB. This match between the spatiotemporal variations of the SMD and the water ice was not observed previously. However, the correlating behavior seems to be prominent in the areas nearby Lunae Planum and Xanthe Terra and the upper-tropospheric region of the atmosphere.     

Solar atmosphere wave dynamics generated by solar global oscillating eigenmodes

The solar atmosphere exhibits a diverse range of wave phenomena, where one of the earliest discovered was the five-minute global acoustic oscillation, also referred to as the p-mode. The analysis of wave propagation in the solar atmosphere may be used as a diagnostic tool to estimate accurately the physical characteristics of the Sun’s atmospheric layers.In this paper, we investigate the dynamics and upward propagation of waves which are generated by the solar global eigenmodes. We report on a series of hydrodynamic simulations of a realistically stratified model of the solar atmosphere representing its lower region from the photosphere to low corona. With the objective of modelling atmospheric perturbations, propagating from the photosphere into the chromosphere, transition region and low corona, generated by the photospheric global oscillations the simulations use photospheric drivers mimicking the solar p-modes. The drivers are spatially structured harmonics across the computational box parallel to the solar surface. The drivers perturb the atmosphere at 0.5?Mm above the bottom boundary of the model and are placed coincident with the location of the temperature minimum. A combination of the VALIIIC and McWhirter solar atmospheres are used as the background equilibrium model.We report how synthetic photospheric oscillations may manifest in a magnetic field free model of the quiet Sun. To carry out the simulations, we employed the magnetohydrodynamics code, SMAUG (Sheffield MHD Accelerated Using GPUs).Our results show that the amount of energy propagating into the solar atmosphere is consistent with a model of solar global oscillations described by Taroyan and Erdélyi (2008) using the Klein-Gordon equation. The computed results indicate a power law which is compared to observations reported by Ireland et al. (2015) using data from the Solar Dynamics Observatory/Atmospheric Imaging Assembly.     

火星大气O3光谱探测技术

O3是火星大气中最重要、最活跃的分子之一,它不仅能够控制到达火星地面的紫外光通量,而且能够追踪大气中水蒸气光化解产生的HOX基,同时也是建立火星大气光化学模型的基础。文章主要描述通过天基遥感和地基遥感两种方法探测得到火星大气O3含量,包括空间和时间的分布、垂直剖面及其变化;具体分析了两种方法的探测机理,详细描述了国际相应光谱仪的整机结构和探测的重要成果,为中国进行深空探测提供了参考。     

基于能量守恒的再入轻诱饵鉴别方法

针对稀薄大气中的诱饵干扰,提出了一种基于能量守恒定律的再入轻诱饵鉴别方法.该方法利用目标单位质量机械能的损耗表征质阻比的相对大小,实现对轻诱饵的鉴别,避开了质阻比估计的收敛过程.首先根据不同目标的能量方程,推导出目标单位质量机械能损耗的解析表达式,确定了鉴别量;然后理论推导了鉴别量的方差估计式并设计了鉴别门限;最后通过仿真验证了鉴别方法的有效性.     

发射星都应做热真空试验

介绍了国内外卫星热真空试验的发展概况、卫星热真空试验的重要性及其与常压热循环试验的关系,指出每一颗发射星都应做热真空试验。     

航空发动机燃油系统及其附件爆炸大气试验技术研究

燃油系统及其附件爆炸大气试验在航空发动机研制过程中极其重要。简述了航空发动机燃油系统及其附件爆炸大气试验技术的特点及国内外发展现状,分析了其试验技术发展需求。详细给出了航空发动机燃油系统及其附件爆炸大气试验的分类、试验要求、试验条件、试验方法和试验判据,并开展了某型航空发动机燃油系统液压机械装置爆炸大气试验验证。结果表明:该试验方案可行、数据可靠、结果有效,为航空发动机燃油系统及其附件爆炸大气试验的研究验证工作提供了依据。     

计算风工程中 k-ε模型的边界条件研究

从 k-ε湍流模型控制方程入手,对两类满足平衡大气边界层理论要求的入口边界条件进行了详细分析,比较了二者的理论差异。然后以我国公路桥梁抗风规范中建议的 A 类风场为来流条件,定义了相应的 k-ε模型常数与壁面条件,使用两类边界条件进行数值模拟。计算结果表明：两类边界条件结合相应的模型常数与壁面条件,均能在数值模拟中构建基本满足规范要求的平衡大气边界层,但各有其适用范围。在此基础上,对模型常数 C 1和湍动能耗散率与数值模拟结果之间的关系进行了研究,采用修改模型常数与边界条件的方法,改善了数值模拟结果。     

北京国际金融大厦风荷载风洞实验研究

具有独特外形、荣获１９９４～１９９５ 年度首都十佳建筑设计方案第一名的北京国际金融大厦风荷载风洞实验研究结果表明,由于该建筑独特的门廊型南北错落结构,其表面风荷载随风向角变化很大,这对今后同一类型的建筑设计从风荷载角度来考虑具有指导意义。笔者还结合北京地区特定的气象条件,参考国外文献,提出了较为合理和可靠的玻璃幕墙风荷载设计值     

地球大气边缘高超声速飞行再入点调整方法

分析环境波动对地球大气边缘高超声速飞行的影响,论证了利用微弱气动力实现再入点调整的可能性。提出神经网络I-PIDA姿态控制策略,控制力矩由脉宽调制驱动的反作用推力器实现,利用模糊预测制导的方法实现再入点的精确调整。仿真算例说明该方法可以实现姿态跟踪和再入点的位置调整,并具有较强的鲁棒性。     

微束等离子焊接

简要介绍了微束等离子焊接的工艺设备。通过对乌克兰巴顿焊接研究所几个实例的介绍，较全面地阐述了微束等离子焊接工艺方案、焊接设备的各项技术要求和特性。与氩弧焊、激光焊进行了比较，认为微束等离子焊接具有电弧收缩、能量集中、适用于薄壁件焊接的特点，在我国具有广阔的应用前景。