固体推进剂点火研究评论

为了确定固体推进剂点火的现有技术水平,本文对该领域的有关文献作了广泛评论,对各种点火理论、实验测量和点火准则作了详细评定研究。为易于进行比较,本文用易懂的表格形式概括了各项研究工作的情况,也讨论了各种重要参数对点火过程的影响。指出了主要技术难点,同时提出了进一步研究的建议。     

高压气动逻辑

引言“气动逻辑”能以多种形式和用普通原理来实现。“气动逻辑”是通过使用压缩空气而不是电作为动力,为工厂和设备提供类似继电器或固体电子逻辑的顺序闭锁和控制功能。“逻辑”要涉及到器件预先规定的操作和将闭锁线路表示为“逻辑图”的绘图习惯和符号。1.历史和发展逻辑线路曾用传统的运动充气组件(通常是与空气压缩设备相连的短管阀)组成,但这样的组件有很多的缺点,如:     

非线性壁板颤振分析

利用一种改进的计算流体力学与计算结构动力学(CFD/CSD)耦合方法研究了由气动和结构几何非线性引起的壁板颤振问题。在非定常气动力计算中,考虑了通量分裂格式、隐式时间推进方法和几何守恒律;二维和三维壁板的结构几何非线性建模则采用了有限元的协同旋转理论,并利用一种近似能量守恒算法求解结构的非线性响应。流场和结构求解器采用二阶松耦合方法联立求解,并将其应用于壁板在超声速、跨声速和亚声速的颤振计算中。当考虑结构几何非线性和气动非线性时,出现了典型的极限环振荡现象,并对颤振边界和极限环振荡幅度进行了对比分析。     

土星磁层顶的Kelvin-Helmholtz不稳定性和磁流体表面波

本文采用可压缩磁流体力学近似并选取Voyager-1的观测数据,讨论了土星磁层顶的Kelvin-Helmholtz不稳定性和磁流体表面波.计算表明,土星磁层随星体自转同磁鞘流之间的速度差,可以在地方时午前、中午和距中午不远的午后磁层顶激发不稳定性;午前和午后区有很强的非对称性.计算所得的波的特性与观测一致.      

M stars as targets for terrestrial exoplanet searches and biosignature detection

The changing view of planets orbiting low mass stars, M stars, as potentially hospitable worlds for life and its remote detection was motivated by several factors, including the demonstration of viable atmospheres and oceans on tidally locked planets, normal incidence of dust disks, including debris disks, detection of planets with masses in the 5-20 M() range, and predictions of unusually strong spectral biosignatures. We present a critical discussion of M star properties that are relevant for the long- and short-term thermal, dynamical, geological, and environmental stability of conventional liquid water habitable zone (HZ) M star planets, and the advantages and disadvantages of M stars as targets in searches for terrestrial HZ planets using various detection techniques. Biological viability seems supported by unmatched very long-term stability conferred by tidal locking, small HZ size, an apparent short-fall of gas giant planet perturbers, immunity to large astrosphere compressions, and several other factors, assuming incidence and evolutionary rate of life benefit from lack of variability. Tectonic regulation of climate and dynamo generation of a protective magnetic field, especially for a planet in synchronous rotation, are important unresolved questions that must await improved geodynamic models, though they both probably impose constraints on the planet mass. M star HZ terrestrial planets must survive a number of early trials in order to enjoy their many Gyr of stability. Their formation may be jeopardized by an insufficient initial disk supply of solids, resulting in the formation of objects too small and/or dry for habitability. The small empirical gas giant fraction for M stars reduces the risk of formation suppression or orbit disruption from either migrating or nonmigrating giant planets, but effects of perturbations from lower mass planets in these systems are uncertain. During the first approximately 1 Gyr, atmospheric retention is at peril because of intense and frequent stellar flares and sporadic energetic particle events, and impact erosion, both enhanced, the former dramatically, for M star HZ semimajor axes. Loss of atmosphere by interactions with energetic particles is likely unless the planetary magnetic moment is sufficiently large. For the smallest stellar masses a period of high planetary surface temperature, while the parent star approaches the main sequence, must be endured. The formation and retention of a thick atmosphere and a strong magnetic field as buffers for a sufficiently massive planet emerge as prerequisites for an M star planet to enter a long period of stability with its habitability intact. However, the star will then be subjected to short-term fluctuations with consequences including frequent unpredictable variation in atmospheric chemistry and surficial radiation field. After a review of evidence concerning disks and planets associated with M stars, we evaluate M stars as targets for future HZ planet search programs. Strong advantages of M stars for most approaches to HZ detection are offset by their faintness, leading to severe constraints due to accessible sample size, stellar crowding (transits), or angular size of the HZ (direct imaging). Gravitational lensing is unlikely to detect HZ M star planets because the HZ size decreases with mass faster than the Einstein ring size to which the method is sensitive. M star Earth-twin planets are predicted to exhibit surprisingly strong bands of nitrous oxide, methyl chloride, and methane, and work on signatures for other climate categories is summarized. The rest of the paper is devoted to an examination of evidence and implications of the unusual radiation and particle environments for atmospheric chemistry and surface radiation doses, and is summarized in the Synopsis. We conclude that attempts at remote sensing of biosignatures and nonbiological markers from M star planets are important, not as tests of any quantitative theories or rational arguments, but instead because they offer an inspection of the residues from a Gyr-long biochemistry experiment in the presence of extreme environmental fluctuations. A detection or repeated nondetections could provide a unique opportunity to partially answer a fundamental and recurrent question about the relation between stability and complexity, one that is not addressed by remote detection from a planet orbiting a solar-like star, and can only be studied on Earth using restricted microbial systems in serial evolution experiments or in artificial life simulations. This proposal requires a planet that has retained its atmosphere and a water supply. The discussion given here suggests that observations of M star exoplanets can decide this latter question with only slight modifications to plans already in place for direct imaging terrestrial exoplanet missions.     

涡破裂诱导的垂尾抖振数值模拟

 采用数值模拟方法研究了大后掠三角翼前缘涡破裂诱导的垂尾抖振问题,分析了大迎角条件下的垂尾抖振特性。采用Navier-Stokes方程求解非定常气动力、耦合结构动力学方程,建立了气动弹性方程,在时域内采用松耦合方式推进以得到垂尾结构响应。研究结果表明:涡破裂流的脉动频带覆盖了垂尾扭转模态的固有频率,诱发了垂尾抖振现象;与传统的颤振频域响应特性不同,垂尾抖振响应的各阶位移与加速度响应主频均位于各阶结构模态固有频率附近。此外,弯曲与扭转响应存在耦合效应,且耦合作用的频率与提取的垂尾表面气动载荷脉动频率一致。垂尾的位移响应由一阶弯曲模态主导,振幅不大;加速度响应主要由扭转模态产生,量级较大,使结构持续遭受严重的附加惯性载荷作用。     

未来空天一体化力量的发展方向探讨

分析了空天一体化力量在未来战争中的重要作用,以及国外空天一体化力量的发展概况和发展趋势.在此基础上,重点探讨了我国空天一体化力量未来发展的五个主要方向.最后,针对世界空天一体化力量的发展趋势,结合我国具体国情给出了几点建议.     

头部波系对气动舵颤振特性的影响研究

以分析头部波系对气动舵颤振的影响为目的,采用CFD/CSD耦合算法.在耦合中采用保形动网格策略保持弹身和舵面的几何外形.对单独舵面和舵身组合体计算发现:与单独舵面相比,舵身组合体颤振边界随马赫数升高下降更快;在Ma=7时,单独舵面尚未颤振而组合体中的舵面已颤振.其机理为头部波系对气动舵的影响:马赫数升高,头部圆锥激波内移,膨胀低压区缩小,舵面上激波和外流场的总影响区扩大,气动舵更易颤振.     

高超音速飞行器气动加热计算

对高超音速飞行器气动加热计算方法进行研究，采用基于热流量平衡方程的工程估算方法和二维薄层近似N－S方程数值模拟，计算高超音速飞行器对称面中心线上的温度分布。以天地往返运输系统的气动加热为例进行了计算，并对计算结果进行了分析和比较，计算结果表明：该工程估算方法和数值计算方法是可行的。     

风能引信电机的超声速实验技术研究

对于榴弹风能引信电机输出特性的研究,过去都是在闭口式风洞中进行实验,但经大量实验证明,闭口式风洞中各种因素的影响,不利于研究榴弹风能引信电机输出性能及抗高转速的问题。笔者应用气体动力学和实验空气动力学理论,设计一种适合榴弹风能引信电机超声速射流实验装置,利用该装置进行了现有各种型号风能引信电机的超声速实验研究。在此基础上,把超声速风能引信电机进气通道改为拉瓦尔喷管形式。采用实验方法选择出最佳喉道面积。最后,通过实弹打靶得到了验证,同时对风能电机的输出电压和频率进行了风洞试验和打靶遥测数据比较,两者吻合较好。研究表明,拉瓦尔喷管形式的引信电机应用速度范围宽,并便于控制电机的转速。该研究解决了多年来引信电机抗高转速的问题。