Late Stages of Stellar Evolution

A large fraction of ISO observing time was used to study the late stages of stellar evolution. Many molecular and solid state features, including crystalline silicates and the rotational lines of water vapour, were detected for the first time in the spectra of (post-)Asymptotic Giant Branch (AGB) stars. Their analysis has greatly improved our knowledge of stellar atmospheres and circumstellar environments. A surprising number of objects, particularly young planetary nebulae with Wolf-Rayet (WR) central stars, were found to exhibit emission features in their ISO spectra that are characteristic of both oxygen-rich and carbon-rich dust species, while far-IR observations of the PDR around NGC 7027 led to the first detections of the rotational line spectra of CH and CH⁺. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.     

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.     

基于CPLD的高速可重构PCM帧同步器的实现

给出一种基于 CPL D的高速可重构帧同步器的设计思路和实现方法 ,探讨如何提高系统速度及其可靠性。既采用数字化相关检测技术和可容错的校验保护技术 ,又采用系统内在线可编程 ISP(In- System Programm ing)技术和提高系统速度的流水线技术 ,综合高速 PCI总线接口设计 ,完成了在线可重新配置的高速帧同步器的实现     

论航天遥感器研制过程中的防静电

文章从应用新技术、新器件可能对航天遥感器产品带来的静电损伤的现象入手 ,介绍了静电放电原理、带来的危害及生成的因素。分析了航天遥感器在研制过程中出现的静电放电现象和产生的原因 ,提出了研制过程中应采取的防静电措施     

“长征三号”一,二级火箭的防潮,防水

叙述了“长征三号”火箭，首次在雨季发射时，采用的防潮防水技术的实施方案及使用后的效果。它给运载火箭的电气系统正常工作创造了良好的环境条件，保证了火箭安全、可靠、及时发射。     

基于神经网络的电机智能保护器研究

介绍了一种电机智能保护装置系统，分析了对电动机进行各类保护的原理，并且针对过载保护．提出一种基于人工神经网络的电动机长期过载运行温升预测的算法，将这种算法应用于实际的保护中．有效地弥补了不能用数学模型精确描述电机运行中发热和散热过程的缺陷。实验证明，在样本足够多的情况下，这种方法是切实可行的。     

不均布行星齿轮传动装置设计的几个问题

推导了不均布行星传动的装配条件；提出了不均布所带来的各行星轮合力及工作过程中的动不平衡离心力的计算公式；推荐了使其合力为零或减至最小的方法；得出了行星轮不均布的行星传动装置的使用条件和设计时应注意的几个问题。     

现代飞机交流电源过电压保护问题探讨

本文在分析现代飞机电源系统所使用的几种过电压保护装置工作原理的基础上,着重对其反延时特性和动作电压进行计算,并就决定和影响过电压保护性能指标的电路参数的调整进行了计算和论述。     

载人飞船返回舱的烧蚀防热

载人飞船返回舱的烧蚀热防护技术研究和试验表明，碳化烧蚀材料是再入飞行器最有效的热防护层。对典型的碳化烧蚀体的热性能的预测分析模型和计算方法作了阐述。数值计算结果分别与电弧风洞试验和阿波罗的飞行验证试验作了比较，结果符合得很好。     

太阳质量损失对行星轨道的影响

本文利用Ｇｙｌｄｅｎ－Ｍｅｓｈｃｈｅｒｓｋｉｉ方程和Ｅｄｄｉｎｇｔｏｎ－Ｊｅａｎｓ定律，讨论太阳质量损失对行星轨道的影响，结果表明由于太阳质量损失会产生轨道半长径α的一阶周期项和二阶混合项；近日点角距ω的一阶周期项、二阶长期项和混合项，行星轨道半长径的长期变化会影响太阳系的稳定性。