谈合并会计报表抵销分录的编制

本文详细介绍了为何要编制合并会计报表,哪些应纳入合并会计报表范围,在公司连续编制情况下, 对以前年度已做抵销的事项在今后编制合并会计报表时为何还要进行抵销进行了论述。     

机动再入飞行器的复合制导方案研究

对机动再入飞行器弧段的复合制导方案进行了研究，首先提出了通过高低空复合制导控制再入飞行器的终端速度和弹道倾角的思路；然后分别给出了高空最优制导律和大气厚再入最优制导律；最后对此复合制导方案进行了数字仿真。仿真结果表明此方案在理论上是可行的。     

空间大气成分探测傅立叶变换红外光谱仪

文章阐述了用于空间大气成分探测傅立叶变换红外光谱仪的国外发展状况,主要介绍了几种国外先进的高分辨率空间大气探测用傅立叶变换红外光谱仪的结构、应用范围和技术指标,比较了这几种设备的优缺点和技术特点。     

跨大气层和空间区域飞行器的液体推进剂管理

根据大气层飞行环境与机动飞行特点,以及空间飞行环境与液体推进剂特点,分析了跨大气层和空间区域飞行器的保证重力场和失重状态下均无夹气液体输送、控制液体推进剂质心位移、剩余推进剂空间排放和重复使用等液体推进剂管理技术要求。阐述了相应的关键技术,如包括无夹气输送、液体质心位移控制、失重状态下的流体动力、参数确定和结构设计等管理模式确定,以及包括模型参数确定、模型、状态模拟和验证等的管理模式试验。     

飞行器完全非定常气动力的一种工程计算方法

本文以谐振运动非定常气动力计算理论为基础,采用偶极子格网技术进行数值计算、有理式拟合、Fourier积分和Duhamel积分等步骤,给出了飞行器任意运动和受任意大气扰动时完全非定常气动力的一种工程计算方法。该方法数学处理方便,得到的气动力表达式简单。算例结果表明:该完全非定常气动力计算方法可行,精度令人满意,具有工程实际意义。     

振动尖塔对风洞模拟大气湍流边界层的作用

针对大气边界层风洞模拟中常常出现的湍流度随高度衰减太快的问题，本文尝试了一种新的被动模拟方法——振动尖塔法。该方法主要采用了具有弹性底座的尖塔型旋涡发生器。尖塔群受风洞自由来流驱动，发生随机振动，向下游流场注入了强烈的低频扰动，致使试验区的湍流度、积分尺度和风谱惯性子区的宽度都明显增加，改善了风洞的模拟性能。     

基于大气传输软件激光透过率对比研究

简要地归纳了目前比较通用的大气传输软件LOWTRAN7、MODTRAN和FASCODE的概况和异同,分析了大气透过率的计算和激光武器选用的波长,比较了激光传输衰减和能见度的关系,重点研究对比了用LOWTRAN7和FASCODE计算1．06μm和10．6μm激光的透过率,并得出了结论。     

Flight Flutter Modal Parameters Identification with Atmospheric Turbulence Excitation Based on Wavelet Transformation

针对基于大气紊流激励的飞机颤振试验数据具有信噪比低以及测量数据以加速度响应形式给出等特点,将小波变换与随机减量法相结合对飞机颤振模态参数进行识别,首先利用随机减量法获得结构在非零初始加速度条件下的自由衰减响应,然后对该自由衰减响应进行Morlet连续小波变换,为使变换简单,本文采用了Parseval定理和留数定理,利用Morlet的带通滤波特性,通过搜索小波变换系数在不同的尺度区域内的极大值,再根据小波变换系数的极大值、相角与固有振动频率及阻尼系数间的关系,即可识别出各模态参数。并对利用小波变换识别颤振模态参数时,实现模态解耦应满足的条件进行了分析研究。通过仿真和飞机颤振试验数据分析,验证了该识别方法不仅简单、有效和可行,而且具有较强的抗噪性。     

一种新的空间飞行器再入制导律研究

基于阻力与能量关系的优化剖面,以该再入剖面作为基准轨迹,给出了跟踪这一基准轨迹的空间飞行器再入制导律与控制律,将基准轨迹转化为相应的迎角剖面和滚转角剖面,设计了相应的结构配置。仿真结果表明,基于阻力与能量关系剖面设计的制导律满足了各项约束条件,并能成功地控制飞行器到达所要求的位置。     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.