Crustal S-Wave Velocity from Apparent Incidence Angles: A Case Study in Preparation for InSight

Retrieval of crustal structure and thickness of Mars is among the main goals of InSight. Here we investigate which constraints on the crust at the landing site can be provided by apparent P-wave incidence angles derived from P-receiver functions. We consider receiver functions for six different Mars models, calculated from synthetic seismograms generated via Instaseis from the Green’s function databases of the Marsquake Service, in detail. To allow for a larger range of crustal thicknesses and structures, we additionally analyze data from five broad-band stations across Central Europe. We find that the likely usable epicentral distance range for P-wave receiver functions on Mars lies between \(35^{\circ}\) and the core shadow, and can be extended to more than \(150^{\circ}\) by also using the PP-phase. Comparison to models for the spatial distribution of Martian seismicity indicates that sufficient seismicity should occur within the P-wave distance range around InSight within the nominal mission duration to allow for the application of our method. Apparent P-wave incidence angles are derived from the amplitudes of vertical and radial receiver functions at the P-wave onset within a range of period bands, up to 120 s. The apparent incidence angles are directly related to apparent S-wave velocities, which are inverted for the subsurface S-wave velocity structure via a grid search. The veracity of the forward calculated receiver functions and apparent S-wave velocities is ensured by benchmarking various algorithms against the Instaseis synthetics. Results indicate that apparent S-wave velocity curves provide valuable constraints on crustal thickness and structure, even without any additional constraints, and considering the location uncertainty and limited data quantity of InSight. S-wave velocities in the upper half of the crust are constrained best, but if reliable measurements at long periods are available, the curves also provide constraints down to the uppermost mantle. Besides, it is demonstrated that the apparent velocity curves can differentiate between crustal velocity models that are indistinguishable by other methods.     

The Origin,Early Evolution and Predictability of Solar Eruptions

Coronal mass ejections (CMEs) were discovered in the early 1970s when space-borne coronagraphs revealed that eruptions of plasma are ejected from the Sun. Today, it is known that the Sun produces eruptive flares, filament eruptions, coronal mass ejections and failed eruptions; all thought to be due to a release of energy stored in the coronal magnetic field during its drastic reconfiguration. This review discusses the observations and physical mechanisms behind this eruptive activity, with a view to making an assessment of the current capability of forecasting these events for space weather risk and impact mitigation. Whilst a wealth of observations exist, and detailed models have been developed, there still exists a need to draw these approaches together. In particular more realistic models are encouraged in order to asses the full range of complexity of the solar atmosphere and the criteria for which an eruption is formed. From the observational side, a more detailed understanding of the role of photospheric flows and reconnection is needed in order to identify the evolutionary path that ultimately means a magnetic structure will erupt.     

Venus: The Atmosphere,Climate, Surface,Interior and Near-Space Environment of an Earth-Like Planet

This is a review of current knowledge about Earth’s nearest planetary neighbour and near twin, Venus. Such knowledge has recently been extended by the European Venus Express and the Japanese Akatsuki spacecraft in orbit around the planet; these missions and their achievements are concisely described in the first part of the review, along with a summary of previous Venus observations. The scientific discussions which follow are divided into three main sections: on the surface and interior; the atmosphere and climate; and the thermosphere, exosphere and magnetosphere. These reports are intended to provide an overview for the general reader, and also an introduction to the more detailed topical surveys in the following articles in this issue, where full references to original material may be found.     

Towards a Global Unified Model of Europa’s Tenuous Atmosphere

Despite the numerous modeling efforts of the past, our knowledge on the radiation-induced physical and chemical processes in Europa’s tenuous atmosphere and on the exchange of material between the moon’s surface and Jupiter’s magnetosphere remains limited. In lack of an adequate number of in situ observations, the existence of a wide variety of models based on different scenarios and considerations has resulted in a fragmentary understanding of the interactions of the magnetospheric ion population with both the moon’s icy surface and neutral gas envelope. Models show large discrepancy in the source and loss rates of the different constituents as well as in the determination of the spatial distribution of the atmosphere and its variation with time. The existence of several models based on very different approaches highlights the need of a detailed comparison among them with the final goal of developing a unified model of Europa’s tenuous atmosphere. The availability to the science community of such a model could be of particular interest in view of the planning of the future mission observations (e.g., ESA’s JUpiter ICy moons Explorer (JUICE) mission, and NASA’s Europa Clipper mission). We review the existing models of Europa’s tenuous atmosphere and discuss each of their derived characteristics of the neutral environment. We also discuss discrepancies among different models and the assumptions of the plasma environment in the vicinity of Europa. A summary of the existing observations of both the neutral and the plasma environments at Europa is also presented. The characteristics of a global unified model of the tenuous atmosphere are, then, discussed. Finally, we identify needed future experimental work in laboratories and propose some suitable observation strategies for upcoming missions.     

用于薄片试样弹塑性应力-应变分析的半解析方法

针对圆弧漏斗薄片试样和圆环薄片试样提出了半解析统一模型,并进行了有限元验证,该模型对漏斗薄片试样与圆环薄片试样单调力学行为均有优良的描述性。完成了漏斗薄片试样与圆环薄片试样的单轴拉伸试验及变幅对称循环试验,获得了载荷-位移曲线和循环稳定载荷幅-位移幅曲线。通过该模型并利用试验曲线预测材料单轴应力-应变关系和循环应力-应变关系,发现根据两种薄片试样预测的材料应力-应变关系及循环应力-应变关系与标准圆棒试样结果吻合良好。     

数据挖掘在运载火箭智能测试中的应用

针对运载火箭复杂系统的故障检测难以建立准确的数学模型的问题,研究了基于数据驱动的数据挖掘异常检测算法,对多种数据挖掘算法在运载火箭发动机异常检测的应用进行了研究和分析,提出了基于混合概率密度统计的多策略异常检测评价算法。该算法基于非监督学习的算法挖掘火箭发动机不同参数间的正常关联模型,火箭发动机早期的异常数据会引起正常关联模型的破坏,引入混合概率密度统计的多策略异常检测评价机制,可以有效屏蔽参数测量故障对系统故障检测的影响,从而更加准确给出系统异常程度。使用发动机历史试车数据作为样本进行特征模型的训练,使用一元、多元和混合概率密度模型对存在异常的发动机试车数据进行了实时异常检测的实验验证。实验结果表明,相比传统基于阈值和规则的异常检测算法,基于概率密度统计的多策略异常检测算法不仅可给出系统的正常和异常的状态,还可计算各参数和整个系统的异常值,为运载火箭进一步的故障诊断提供更加灵活的参考。     

瓦状塞式喷管的设计和试验分析

为了分析瓦状塞式喷管的气动特性,提出轴对称内喷管和塞锥的型面设计方法,设计了两单元的模型发动机,内喷管面积比为5.81,总面积比为24.36、29.43、33.88、37.58。采用高压空气为介质对模型发动机进行冷流试验,分析内喷管倾角和底部二次流变化、以及有无底部盖板对推力性能和底部压强的影响情况。介绍了试验发动机的结构与设计参数,给出了试验模型照片、测量参数曲线和性能数据处理。结果表明：瓦状塞式喷管模型的高度补偿效果较为明显,在整个工作高度有较高的推力系数效率,20°模型的最高效率为96%;底部压强曲线反映出了底部气动特性由开放状态到闭合的转变过程;内喷管倾角增大,底部压强增大即增加底部推力,但存在一个优化性能的最佳倾角;底部加入二次流可以增加底部压强,提高性能,但其影响范围在1%～2%,少量的二次流对增加性能的效果较好;底部盖板会影响底部的气动特性,底部压强是否受环境压强的影响取决于底部处于开放或闭合状态。     

LaSr3Fe3O10-δ混合导体结构及氧非化学计量的研究

采用柠檬酸盐法制备了纯的LaSr3Fe3O10-δ粉体。利用间接碘量法测定了LaSr3Fe3O10-δ系列样品中铁离子的平均价态和氧的非化学计量值。实验发现,随着温度的逐渐升高,LaSr3Fe3O10-δ逐渐失氧,三价铁浓度增加使得铁的平均价态降低。     

后处理温度对邻苯二甲腈基复合材料高温性能的影响

制备了MT300/邻苯二甲腈复合材料,分析了不同后处理温度对其在室温和400℃下力学性能的影响。结果表明,复合材料的后处理温度由315℃提高到330℃,会使其室温下的弯曲强度和模量明显提高;但继续提高后处理温度至375℃,室温下的弯曲强度则不断下降而弯曲模量未出现显著变化;在400℃的测试温度下,复合材料的弯曲强度、模量和压缩强度则均随后处理温度提升逐步提高。复合材料的室温压缩性能随后处理温度升高呈下降趋势,但在350℃处理后其室温压缩强度又出现明显上升。室温、400℃下层间剪切强度则均随后处理温度由315℃升高至375℃而呈先下降后上升趋势。