航电设备的"未发现故障"

所谓NFF是指在机上或外场维修中因故障而更换的设备,送到维修车间后却没有发现故障,或发现不了故障.NFF的原因很复杂,有的是因为设备本身并没有故障,但在装机后出现或外场认为有故障,有的设备存在断续性故障但在车间却检测不出来,还有可能是车间的测试能力有限不能将故障检测出来.     

USB测控通信载波功率的一种分配策略

针对USB(统一S频段)通信中副载波信号的功率分配问题,提出了一种载波功率分配策略,实现了副载波功率的最优分配,达到了提高功率效率的目的。结合某卫星副载波的特点,以应答机对副载波的检测门限为依据,对测控上行各副载波功率进行分配。计算结果表明,该载波功率分配策略在残留载波和遥控指令副载波的调制损耗上要优于传统常用调制度分配方法。该功率分配策略能够为卫星通信提供更佳的功率分配,使上行各种副载波信号能够达到卫星接收解调的最佳门限。     

滑阀副零位内泄漏量分布模型与参数灵敏度分析

针对尺寸参数摄动作用下滑阀副零位泄漏量的不确定性，建立了考虑参数摄动的滑阀副零位泄漏量数学模型，获得了尺寸参数摄动下的滑阀副零位泄漏量分布规律。进一步地，建立了工艺参数与零位泄漏量分布特征参数之间映射关系的Kriging代理模型，并基于代理模型利用Sobol法开展了零位泄漏量分布特性对工艺参数的全局灵敏度分析，最终为减小内泄漏量并提高一致性提供了理论依据。研究结果表明，尺寸参数摄动下的零位泄漏量服从正态分布规律，工艺参数之间的交互作用对滑阀副零位泄漏量分布特性的影响可以忽略不计。同时，相比轴向尺寸工艺参数，滑阀副零位泄漏量分布特性对径向尺寸工艺参数和节流边圆角半径工艺参数的变化更为敏感。滑阀副径向间隙最小值对滑阀副零位泄漏量平均值影响最大，而阀芯的节流边圆角半径最大值对滑阀副零位泄漏量的一致性影响最大。滑阀副内泄漏量实验结果表明零位泄漏量呈现出一定的波动性，与理论模型总体预测趋势相一致。     

滑阀副零位内泄漏量分布模型与参数灵敏度分析

针对尺寸参数摄动作用下滑阀副零位泄漏量的不确定性，建立了考虑参数摄动的滑阀副零位泄漏量数学模型，获得了尺寸参数摄动下的滑阀副零位泄漏量分布规律。进一步地，建立了工艺参数与零位泄漏量分布特征参数之间映射关系的Kriging代理模型，并基于代理模型利用Sobol法开展了零位泄漏量分布特性对工艺参数的全局灵敏度分析，最终为减小内泄漏量并提高一致性提供了理论依据。研究结果表明，尺寸参数摄动下的零位泄漏量服从正态分布规律，工艺参数之间的交互作用对滑阀副零位泄漏量分布特性的影响可以忽略不计。同时，相比轴向尺寸工艺参数，滑阀副零位泄漏量分布特性对径向尺寸工艺参数和节流边圆角半径工艺参数的变化更为敏感。滑阀副径向间隙最小值对滑阀副零位泄漏量平均值影响最大，而阀芯的节流边圆角半径最大值对滑阀副零位泄漏量的一致性影响最大。滑阀副内泄漏量实验结果表明零位泄漏量呈现出一定的波动性，与理论模型总体预测趋势相一致。     

滑阀副零位内泄漏量分布模型与参数灵敏度分析

针对尺寸参数摄动作用下滑阀副零位泄漏量的不确定性，建立了考虑参数摄动的滑阀副零位泄漏量数学模型，获得了尺寸参数摄动下的滑阀副零位泄漏量分布规律。进一步地，建立了工艺参数与零位泄漏量分布特征参数之间映射关系的Kriging代理模型，并基于代理模型利用Sobol法开展了零位泄漏量分布特性对工艺参数的全局灵敏度分析，最终为减小内泄漏量并提高一致性提供了理论依据。研究结果表明，尺寸参数摄动下的零位泄漏量服从正态分布规律，工艺参数之间的交互作用对滑阀副零位泄漏量分布特性的影响可以忽略不计。同时，相比轴向尺寸工艺参数，滑阀副零位泄漏量分布特性对径向尺寸工艺参数和节流边圆角半径工艺参数的变化更为敏感。滑阀副径向间隙最小值对滑阀副零位泄漏量平均值影响最大，而阀芯的节流边圆角半径最大值对滑阀副零位泄漏量的一致性影响最大。滑阀副内泄漏量实验结果表明零位泄漏量呈现出一定的波动性，与理论模型总体预测趋势相一致。     

滑阀副零位内泄漏量分布模型与参数灵敏度分析

针对尺寸参数摄动作用下滑阀副零位泄漏量的不确定性，建立了考虑参数摄动的滑阀副零位泄漏量数学模型，获得了尺寸参数摄动下的滑阀副零位泄漏量分布规律。进一步地，建立了工艺参数与零位泄漏量分布特征参数之间映射关系的Kriging代理模型，并基于代理模型利用Sobol法开展了零位泄漏量分布特性对工艺参数的全局灵敏度分析，最终为减小内泄漏量并提高一致性提供了理论依据。研究结果表明，尺寸参数摄动下的零位泄漏量服从正态分布规律，工艺参数之间的交互作用对滑阀副零位泄漏量分布特性的影响可以忽略不计。同时，相比轴向尺寸工艺参数，滑阀副零位泄漏量分布特性对径向尺寸工艺参数和节流边圆角半径工艺参数的变化更为敏感。滑阀副径向间隙最小值对滑阀副零位泄漏量平均值影响最大，而阀芯的节流边圆角半径最大值对滑阀副零位泄漏量的一致性影响最大。滑阀副内泄漏量实验结果表明零位泄漏量呈现出一定的波动性，与理论模型总体预测趋势相一致。     

平显分划副像消除问题的研究

平显备用标线画面的副像问题是影响平显质量的重要缺陷之一．经过分析、计算和试验，在判准了产生副像的根源之后，采用分划板镀黑铬措施，消除了这种副像，研制出了合格产品．     

大九湖的美·是一种原生态的美

<正>美在她的安详宁静:在淡淡的云雾笼罩下,阳光穿越群山徐徐升起,走在软软的草地上,如入仙境。成群的牛羊沐浴着阳光,悠然自得的享用着丰美的水草,好一副静谥的田园风光画卷,这里没有滚滚的热浪,也没有城市的喧嚣,有的只是世外桃源般得壮美和天然去雕饰的天籁。     

慢车燃油分级对高温升燃烧室燃烧效率的影响

在双级旋流多点喷射直接混合(TAMDIM)高温升燃烧室单头部试验件上进行了燃烧效率试验,对比了两种不同主副级喉道间距尺寸下的慢车主、副分级供油方案及副油路单独供油方案的燃烧效率,分析了不同主、副级当量比(副油路供油比例分别为40%，56%，65%，100%)及喉道间距对燃烧效率的影响.试验表明:主副级采用分级供油策略时,喉道间距对燃烧效率有显著影响,喉道间距设计为19.3mm,副油路供油比例控制在40%~56%,可以获得比单独副油路供油更好的燃烧效率.在扇形试验件上进行了试验验证,进一步验证了慢车分级供油策略在TAMDIM高温升燃烧室上的可行性.      

1 种新型燃油分配方案设计

针对航空发动机分级燃烧燃油分配的高精度、变比例需求，提出了1 种基于主、副油路分路计量的新型燃油分配设计方 案，并对该方案进行了理论分析以及仿真和试验验证。结果表明：该方案的燃油分配精度高，燃油分配比例调节灵活，可以满足发动 机日益复杂的低污染设计和控制的需求；在主、副油路同时供油时，燃油分配最小比例与泵后压力负相关，与副油路喷嘴节流特性 正相关。     

航空发动机转子振动的“热模态”和减振设计

为适应航空发动机变转速变工况下转子动力学设计,提出了航空发动机转子"热模态"的概念.利用两种模型解释了"热模态"的含义,并建立了"热模态"下转子动力学设计的方法.利用支承弹性转子(弹支转子)的临界转速与支承刚性转子(刚支转子)的临界转速之比作为优化参数,对转子进行优化设计,既包含了刚度的作用,也计及了质量的影响.结果表明:若所有"热模态"均在刚支转子的第1阶模态之下,则转子临界转速应尽量小于刚支转子的第1阶临界转速.若第1阶"热模态"在刚支转子第1阶模态之下,而第2阶"热模态"在刚支转子第1阶模态之上,但在刚支转子第2阶模态之下,则转子第2阶临界转速应取刚支转子第2阶临界转速和刚支转子第1阶临界转速之方均根值.除此之外,转子剩余不平衡量的分布应与刚支转子的模态正交.      

Anomalous Cosmic Rays and Solar Modulation

We review aspects of anomalous cosmic rays (ACRs) that bear on the solar modulation of energetic particles in the heliosphere. We show that the latitudinal and radial gradients of these particles exhibit a 22-year periodicity in concert with the reversal of the Sun's magnetic field. The power-law index of the low energy portion of the energy spectrum of ACRs at the shock in 1996 appears to be -1.3, suggesting that the strength of the solar wind termination shock at the helioequatorial plane is relatively weak, with s 2.8. The rigidity dependence of the perpendicular interplanetary mean free path in the outer heliosphere for particles with rigidities between 0.2 and 0.7 GV varies approximately as R2, where R is particle rigidity. There is evidence that ACR oxygen is primarily multiply charged above 20 MeV/nuc and primarily singly-charged below 16 MeV/nuc. The location of the termination shock was at 65 AU in 1987 and 85 AU in 1994.     

The evolution of massive stars to explosion

We review the possible evolutionary paths from massive stars to explosive endpoints as various types of supernovae associated with Population I and hence with massive stars: Type II-P, Type II-L, Type Ib, Type Ic, and the hybrid events SN 1987K and SN 1993J. We identify SN 1954A as another hybrid event from the evidence for both H and He in its spectrum with velocities nearly the same as SN 1983J. Evidence for ejected⁵⁶Ni mass of 0.07 M suggests that SN II-P underwent standard iron core collapse, not collapse of an O–Ne–Mg core nor thermonuclear explosion of a C–O core. Most SN II-P presumably arise in single stars or wide binaries of 10–20 M. There may be indirect evidence for duplicity in some cases in the form of strong Ba II lines, such as characterized SN 1987A. SN II-L are recognizably distinct from typical SN II-P and must undergo a significantly different evolution. Despite indications that SN II-L have small envelopes that may be helium enriched, they are also distinct from events like SN 1993J that must have yet again a different evolution. The SN II-L that share a common Luminosity seem to have ejected a small nickel mass and hence may come from stars with O–Ne–Mg cores. The amount of nickel ejected by the exceptionally bright events, SN 1980K and SN 1979C, remains controversial. SN Ib require the complete loss of the H envelope, either to a binary companion or to a wind. The few identified have relatively large ejecta masses. It is not clear what evolutionary processes distinguish SN Ib's evolving in binary systems from hybrid events that retain some H in the envelope. SN Ic events are both H and He deficient. Binary models that can account for transfer of an extended helium envelope from low mass helium cores, 2 to 4 M, imply C–O core masses that are roughly consistent with that deduced from the ejecta mass plus a neutron star, 2 to 3 M. It is possible that the hybrid events are the result of Roche lobe overflow and that the pure events, SN Ib or SN Ic, result from common envelope evolution.     

Cooling of neutron stars and X-ray observations

Cooling of neutron stars is calculated using an exact stellar evolution code. The full general relativistic version of the stellar structure equations are solved, with the best physical input currently available. For neutron stars with a stiff equation of state, we find that the deviation from the isothermality in the interior is significant and that it takes at least a few thousand years to reach the isothermal state. By comparing the most recent theoretical and observational results, we conclude that for Cas A, SN1006, and probably Tycho, standard cooling is inconsistent with the results from the Einstein Observatory, if neutron stars are assumed to be present in these objects. On the other hand, the detection points for RCW103 and the Crab are consistent with these theoretical results.On leave from Department of Physics, Ibaraki University, Japan     

突变截面燃烧室声腔纵向振荡频率规律分析

将药柱贴壁浇注的固体火箭发动机燃烧室简化为中间管型药两端容腔的形式,建立了突变截面H型声腔的物理模型,求解了此种声腔纵向振频的理论解和有限元解,以对称声腔与非对称声腔为对象,分析了一些关键几何尺寸对纵向声振频率变化的影响规律.计算结果表明,声振频率受装药长度与燃烧室长度的比值、装药内外径比值以及药柱浇注位置的共同影响.从合理的装药装填率考虑,初始振荡频率小于圆柱型声腔的振频,并随燃面退移连续增大.      

Halo White Dwarfs and Baryonic Dark Matter

We describe the formation of hot intergalactic gas along with baryonic remnants in galaxy halos. In this scenario, the mass and metallicity of the hot intracluster and intragroup gas relates directly to the production of baryonic remnants during the collapse of galactic halos. We construct a schematic but self-consistent model in which early bursts of star formation lead to a large remnant population in the halo, and to the outflow of stellar ejecta into the halo and ultimately the Local Group. We consider local as well as high redshift constraints on this scenario. This study suggests that the microlensing objects in the Galactic halo may predominantly be 0.5M white dwarfs, assuming that the initial mass function for early star formation favored the formation of intermediate mass stars with m 1M. However, the bulk of the baryonic dark matter in this scenario is associated with the ejecta of the white dwarf progenitors, and resides in the hot intergalactic medium.     

Kites are Fun-Composing Technical Material Using New Methods

"I can't get that stupid kite in the air! I can't! I can't!" "Oh, come on now, Charlie Brown ... that's no way to talk. The whole trouble with you is that you don't believe in yourself! You don't believe in your own abilities. You've got to say to yourself, 'I believe that I can fly this kite.' Now, go ahead, say to yourself, ' I believe that I can fly this kite.'" "I believe that I can fly this kite." "All right, now say it out loud. Say it over and over." "I believe that I can fly this kite! I believe that I can fly this kite! I actually believe I can fly this kite!" "You do? I'll bet you ten-to-one you're wrong!"     

Jet Vectoring Control Using a Novel Synthetic Jet Actuator

A primary air jet vectoring control system with a novel synthetic jet actuator (SJA) is presented and simulated numerically. The results show that, in comparison with an existing traditional synthetic jet actuator, which is able to perform the duty of either “push” or “pull”, one novel synthetic jet actuator can fulfill both “push” and “pull” functions to vector the primary jet by shifting a slide block inside it. Therefore, because the new actuator possesses greater efficiency, it has potentiality to replace the existing one in various appli- cations, such as thrust vectoring and the reduction of thermal signature. Moreover, as the novel actuator can fulfill those functions that the existing one can not, it may well be expected to popularize it into more flow control systems.     

SN 1987A and SN 1993J: Testing stellar evolution theory?

Nearby supernovae like SN 1987A and SN 1993J provide valuable constraints on the late evolution of massive stars. For this purpose, we review evolutionary models for the progenitor of SN 1987A and confront them with five observational/theoretical tests we devised. We show that single-star models (with the possible exception of rapid-rotation models) fail at least two of these tests, while two binary models (accretion and merger models) are consistent with all available constraints. We conclude that it is most likely that the progenitor of SN 1987A had a binary companion, either at the time of the explosion or at least in the not-too-distant past, and that SN 1987A should therefore not be used to calibrate single stellar evolution theory. For SN 1993J, we infer from the presupernova photometry and the early light curve that its progenitor was a 15M star that lost almost all of its hydrogen-rich envelope prior to the supernova. This seems to require that the progenitor underwent stable case C mass transfer. We discuss future observational tests of binary models for both supernovae.     

Turbulent transition in solar surges

It has been suggested that a surge can be modelled as a jet travelling in a sheared magnetic field, and that the transition to turbulence of this MHD tearing jet can explain several key observed features. In this paper we present our preliminary results of the transition to turbulencevia secondary instabilities of the MHD tearing jet. Our results confirm that turbulent transition can decelerate the surge, with decay times which compare well with surge data. Furthermore, we find that the turbulent MHD tearing jet forms magnetic field-aligned velocity filaments similar to those often observed in the surge flow field.