Emergence of a Habitable Planet

We address the first several hundred million years of Earth’s history. The Moon-forming impact left Earth enveloped in a hot silicate atmosphere that cooled and condensed over ∼1,000 yrs. As it cooled the Earth degassed its volatiles into the atmosphere. It took another ∼2 Myrs for the magma ocean to freeze at the surface. The cooling rate was determined by atmospheric thermal blanketing. Tidal heating by the new Moon was a major energy source to the magma ocean. After the mantle solidified geothermal heat became climatologically insignificant, which allowed the steam atmosphere to condense, and left behind a ∼100 bar, ∼500 K CO₂ atmosphere. Thereafter cooling was governed by how quickly CO₂ was removed from the atmosphere. If subduction were efficient this could have taken as little as 10 million years. In this case the faint young Sun suggests that a lifeless Earth should have been cold and its oceans white with ice. But if carbonate subduction were inefficient the CO₂ would have mostly stayed in the atmosphere, which would have kept the surface near ∼500 K for many tens of millions of years. Hydrous minerals are harder to subduct than carbonates and there is a good chance that the Hadean mantle was dry. Hadean heat flow was locally high enough to ensure that any ice cover would have been thin (<5 m) in places. Moreover hundreds or thousands of asteroid impacts would have been big enough to melt the ice triggering brief impact summers. We suggest that plate tectonics as it works now was inadequate to handle typical Hadean heat flows of 0.2–0.5 W/m². In its place we hypothesize a convecting mantle capped by a ∼100 km deep basaltic mush that was relatively permeable to heat flow. Recycling and distillation of hydrous basalts produced granitic rocks very early, which is consistent with preserved >4 Ga detrital zircons. If carbonates in oceanic crust subducted as quickly as they formed, Earth could have been habitable as early as 10–20 Myrs after the Moon-forming impact.     

Modelling of Ejecta as a Space Debris Source

When a micro-debris or a micrometeoroid impacts a spacecraft surface, a large number of secondary particles, called ejecta, are produced. These particles can contribute to a modification of the debris environment: either locally by the occurrence of secondary impacts on the components of complex and large space structures, or at great distance by the formation of a population of small orbital debris. This paper describes firstly, the ejecta overall production, and secondly, the lifetime and the orbital evolution of the particles. Finally the repartition of ejecta in LEO is computed. Some results describing the population as a function of size and altitude are presented.     

抗空间碎片碰撞穿透的航天器加强防护板设计

文章描述了以整体薄护罩和等效重量波纹薄护罩制作的双层板结构系统穿孔阻力的研究结果。指出如果以等效重量波纹缓冲器代替整体缓冲器可以显著地增加穿孔防护能力。针对在倾斜超高速碰撞事件中跳飞碎片的产生,波纹薄护罩的波纹参数可以用减少势的方法优化。     

利用遥测数据预报导弹落点的方法

给出利用遥测数据对导弹进行落点预报的方法。根据遥测数据传输多遍的特点，对解码后的ＰＣＭ 数据进行处理，得到误码率很小的数据。然后对头体分离时刻前导弹飞行的状况和遥测数据进行分析，从而对发动机后效误差进行修正，得到较精确的导弹运动参数，最后利用弹道方程预报导弹落点     

克服地球轨道空间碎片的航天器防护结构几何规划设计

文章描述了一个用于航天器防护结构综合优化的独特方法——几何规划优化技术,以减小暴露于流星体和空间碎片超高速碰撞环境下的航天器防护结构系统的重量。空间碎片和流星体环境由广义加权目标函数的公式来定义。通过Wilkinson,Burch和Nysmith超高速碰撞预示模型说明几何规划的性能。表明遵循几何规划形式的超高速碰撞模型,可以进行综合非线性设计优化。     

综合离心试验全模拟设计

本文提出了一个新的综合离心试验方法，该方法不仅可以对试验件进行过载考核，同时也可实现对其任意截面的弯矩考核，实现了与真实飞行状态更为接近的试验加载方式。该试验方法已经在一些地面试验中得到了较好的应用。     

关于房地产项目环境影响评价工作的思路和要点

近些年来,房地产开发建设项目已经成为我国经济发展的支柱行业。在房地产开发建设过程中(施工期)会对外部环境产生不利影响,房地产项目建成后(营运期),居住小区对内部环境、外部环境都可能产生影响,外部污染也可能影响小区环境。作者根据多年来的环评工作经历,就房地产开发项目的环评从法律依据及项目分类管理、选址分析、标准选取、评价要点等方面进行较全面的分析阐述。     

尖头细长体中小迎角流动结构的数值模拟和实验研究

利用可压缩层流Navier-Stokes方程模拟了尖头细长体中小迎角的流动结构。给出了4个迎角状态的物面流谱,分析了极限流线随迎角的发展过程;给出了25°迎角的横截面流谱,分析了它们的拓扑特征。展示了由主涡涡对、二次涡对和Tertiary涡对等三重涡组成的完整的涡系结构,强调了Tertiary涡在涡系演化中的意义,及其沿轴向发展过程中迹线的合并与分叉现象。计算与实验结果定性一致。     

基于分段常滑翔角的长航时纵向远程滑翔飞行方程近似解

提出用包含地球旋转效应的n个常滑翔角飞行段近似实际滑翔飞行轨迹的方法。基于该方法推导了长航时纵向远程滑翔飞行轨迹近似解，并给出了各段常滑翔角、滑翔时间的求解方法及整个滑翔轨迹近似计算步骤。文中算例结果表明，该近似求解方法计算得到的滑翔航程和滑翔时间与实际值相差很小，航程误差率约为0．7％，时间误差率约为0．6％，因此该方法在近似小初始滑翔角的长航时远程纵向滑翔飞行时是有效的、可行的，尤其针对航程在地球半圈以上的滑翔飞行轨迹。