当高度H≥11000公尺时,计算涡轮喷气发动机飞机的某些飞行特性的新方法

飞机水平飞行的最大和最小速度一般是根据与马赫数成函数关系的发动机推力系数曲线C_P和飞机阻力系数曲线C_X的交点来确定,(图一,a)。     

For aerospace programs,the crises continue

The Legislative Update column reports on President Bush's supplemental budget request for the war in Iraq, the formation of a defense caucus in the House of Representatives, stabilized funding for airport security, the Department of Homeland Security budget, NASA's budget request, funding for NASA's aeronautics program, and NASA's new authorization. NASA's FY04 budget request is $15.47 billion, less than 1% more than FY03. The aeronautics program budget request for FY04 is $959 million, a decrease of 8.5% from FY03. Congress is working to introduce a multiyear authorization for NASA during the 108th session.     

吉尔南再入测量站在美国战略武器试验中的作用

吉尔南再入测量站(KREMS)是一个雷达测量站,位于马绍尔群岛中夸贾林珊瑚礁的罗伊—纳慕岛。该站是夸贾林导弹靶场的一部份,为各种导弹试验和空间跟踪任务收集雷达测量数据。这些数据可供各有关部门用来鉴定弹道导弹再入系统、防御系统以及美国和外国的卫星系统。本文对吉尔南再入测量站、测量能力及其在弹道导弹试验和空间跟踪活动中的作用等方面做了介绍。     

自动液氮加注系统

大量的光谱学的实验和其它物理测量必须在持续一段时间的液氮温度中进行。从最简单的杜瓦瓶到精心制做的自动冷却剂流体     

我参加美国环境科学学会1981年技术年会

应美国环境科学学会(I、E、S)的邀请,北京强度环境研究所和北京环境工程试验中心的三位同志参加了I、E、S第27届年会。北京强度环境研究所的黄友仙同志在会上宣读了技术论文“模拟瞬态环境的一种方法—快速扫描法”,受到与会者的欢迎。三位同志还在美国西部进行了参观访问。他们感到美国对环境试验工作相当重视。     

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:     

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.